# last updated on Thu May 17 06:20:01 JST 2012, dbhost=host=athena, by rodos NAME RA DEC LII BII ROLL_ANGLE TIME STOP_TIME OBSID EXPOSURE TIME_AWARDED XIS0_EXPO XIS1_EXPO XIS2_EXPO XIS3_EXPO XIS0_NUM_MODES XIS1_NUM_MODES XIS2_NUM_MODES XIS3_NUM_MODES HXD_NUM_MODES HXD_EXPO_CO HXD_EXPO_FI HXD_EXPO_NO HXD_EXPO HXD_EXPO_WAM HXD_BURSTS PROCESSING_STATUS PROCESSING_DATE PUBLIC_DATE DISTRIBUTION_DATE PROCESSING_VERSION NUM_PROCESSED SOFTWARE_VERSION PRNB ABSTRACT SUBJECT_CATEGORY CATEGORY_CODE PRIORITY PI_LNAME PI_FNAME COPI_LNAME COPI_FNAME COUNTRY CYCLE OBS_TYPE TITLE AIMPOINT INJECTION E0102-72 16.139 -72.1205 301.50933431 -44.97149935 119.4064 53593.3086458333 53595.2485069444 100001010 2406.8 70000 2406.8 2406.8 2406.8 2406.8 1 1 1 1 0 0 0 0 0 0 0 PROCESSED 54324.1896990741 54247 54035.5925115741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000001 XIS door open with a SMC SNR E0102-72 CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG XIS door open NULL N E0102-72 15.9884 -72.0403 301.56673438 -45.05476105 119.5512 53595.2489236111 53595.4618518518 100001020 4159.8 10000 4159.8 4159.8 4159.8 4159.8 1 1 1 2 0 0 0 0 0 0 0 PROCESSED 54326.8727430556 54247 54035.6312731482 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000001 XIS door open with a SMC SNR E0102-72 CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG XIS door open NULL N N132D 81.2794 -69.6524 280.31514531 -32.77566051 53.3291 53595.4703125 53597.5313541667 100002010 7406.6 80000 7406.6 7406.6 7406.6 7406.6 2 2 2 2 0 0 0 0 0 0 0 PROCESSED 54330.31 54247 54038.5875925926 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD HV ON WITH N132D NULL N N132D 81.1356 -69.5861 280.24807804 -32.83670135 53.4639 53597.5317361111 53597.6932291667 100002020 0 7000 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 PROCESSED 54320.5084259259 54247 54230.4131828704 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD HV ON WITH N132D NULL N N132D 81.4173 -69.7177 280.38157857 -32.71705874 53.198 53597.6939814815 53597.8369328704 100002030 0 7000 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 PROCESSED 54320.4973032407 54247 54230.4133449074 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD HV ON WITH N132D NULL N N132D 81.0865 -69.7023 280.38777612 -32.83268249 53.5118 53597.8375 53597.9865625 100002040 0 7000 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 PROCESSED 54320.6242708333 54247 54230.4148726852 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD HV ON WITH N132D NULL N N132D 81.4727 -69.6025 280.24276086 -32.71811202 53.1485 53597.9869444444 53598.2398958333 100002050 0 7000 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 PROCESSED 54320.6674652778 54247 54230.4157291667 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD HV ON WITH N132D NULL N N132D 81.2751 -69.6506 280.31335191 -32.77744994 53.3312 53598.2402777778 53598.5140046296 100002060 5963.5 7000 5963.5 5963.5 5963.5 5963.5 1 1 1 1 0 0 0 0 0 0 0 PROCESSED 54327.1238888889 54247 54038.4700810185 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD HV ON WITH N132D NULL N DEM_L71/N23 76.4474 -67.958 278.75859594 -34.83581885 70.5849 53598.5206365741 53599.6042592593 100003010 5789.7 40000 5789.7 5789.7 5789.7 5789.7 2 2 2 2 0 0 0 0 0 93606.1 0 PROCESSED 54329.4726736111 54247 54035.7018171296 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000003 LMC SNRs L71/N23 CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG LMC SNRs NULL N MCG-6-30-15 203.9795 -34.2919 313.29805273 27.68293005 295.971 53599.6735300926 53601.1459027778 100004010 46698.7 40000 46700.9 50916.9 46698.7 46725.4 3 3 3 3 1 0 0 46484.6 46484.6 127099.9 0 PROCESSED 54330.2736458333 54247 54035.7991782407 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000004 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG MCG-60-30-15 NULL N Cen A 201.3695 -43.0177 309.51950829 19.41821819 303.9158 53601.1523032407 53602.4098148148 100005010 64675.9 40000 64694.2 64765.8 64675.9 64739.9 5 2 5 5 1 0 0 66258.2 66258.2 108611.9 0 PROCESSED 54327.7080208333 53705 53905.4597106482 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000005 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Cen A NULL N A 2052 229.2779 6.8766 9.31339919 49.96215441 281.2328 53602.4238078704 53602.743287037 100006010 13902.1 20000 13902.1 13902.1 13902.1 13902.1 1 1 1 1 1 0 0 13416.3 13416.3 27583.9 0 PROCESSED 54320.5582175926 53705 53905.4607523148 2.0.6.13 10 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000006 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Outer region of A 2052 NULL N A 2052 229.3237 7.1059 9.64711471 50.05514889 281.2373 53602.7440393518 53603.3406944445 100006020 25743.1 20000 25743.1 25743.1 25743.1 25743.1 1 1 1 1 1 0 0 21064.2 21064.2 51519.9 0 PROCESSED 54320.8272106482 53705 53905.4610300926 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000006 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Outer region of A 2052 NULL N A 2052 229.0933 7.1516 9.50335527 50.26933049 281.2093 53603.3412615741 53603.6114351852 100006030 12969 20000 12969 12969 12969 12969 1 1 1 1 1 0 0 13141.3 13141.3 23327.9 0 PROCESSED 54320.518287037 53705 53905.4613310185 2.0.6.13 8 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000006 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Outer region of A 2052 NULL N A 2052 229.0471 6.9211 9.16646689 50.17566284 281.2031 53603.6121875 53603.9938425926 100006040 16744.3 20000 16744.3 16744.3 16744.3 16744.3 1 1 1 1 1 0 0 12839.5 12839.5 32951.9 0 PROCESSED 54320.5766435185 53705 53905.4634143518 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000006 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Outer region of A 2052 NULL N A 2052 229.3311 7.2632 9.85579143 50.13807877 91.2371 53762.482650463 53762.9209953704 100006050 22366 20000 22366 22366 22366 22366 2 2 2 2 1 0 0 20388 20388 37865.9 0 PROCESSED 54405.5900578704 54247 54040.5318634259 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000006 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Outer region of A 2052 XIS N Crab Nebula 83.6274 22.0192 184.55062413 -5.78629385 86.8663 53604.1571412037 53604.2501273148 100007010 1722.9 5000 1722.9 1722.9 1722.9 1722.9 1 1 1 1 1 0 0 1808 1808 8034 0 PROCESSED 54320.5038425926 54247 54105.2758912037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000007 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Nebula NULL N Crab nebula 83.6201 22.1854 184.40591259 -5.70300776 86.8631 53604.2507175926 53604.3889351852 100007020 3053.1 5000 3057.1 3053.1 3053.1 3053.1 1 1 1 1 1 0 0 3134.3 3134.3 11940 1 PROCESSED 54320.7151273148 54247 54105.2987268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000007 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Nebula NULL N Crab nebula 83.6399 21.8519 184.69891686 -5.86604099 86.8683 53604.3898263889 53604.4890972222 100007030 2786.1 5000 2786.1 2786.1 2790.1 2786.1 1 1 1 1 1 0 0 2192.7 2192.7 8554.1 0 PROCESSED 54320.5508564815 54247 54105.2865393518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000007 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Nebula NULL N Crab nebula 83.4512 22.0082 184.47195778 -5.93010486 86.7989 53604.489849537 53604.5835416667 100007040 4268.2 5000 4268.2 4268.2 4268.2 4268.2 1 1 1 1 1 0 0 4139.2 4139.2 8056 0 PROCESSED 54326.8415277778 54247 54105.3073726852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000007 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Nebula NULL N Crab nebula 83.8083 22.0272 184.63396429 -5.64031243 86.9342 53604.5844791667 53604.6479861111 100007050 3262 5000 3262 3262 3262 3262 1 1 1 1 1 0 0 3179 3179 5448 0 PROCESSED 54320.5353819444 54247 54105.3334143518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000007 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Nebula NULL N NGC 4945 196.3712 -49.4666 305.27663793 13.34118784 313.9062 53604.7788310185 53605.1010763889 100008010 14338 15000 14338 14338 14338 14338 2 2 2 2 1 0 0 13806.7 13806.7 27841.9 1 PROCESSED 54320.7326157407 54247 54035.5212152778 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000008 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG NGC 4945 NULL N NGC 4945 196.3733 -49.4666 305.27803835 13.34111135 313.9078 53605.101087963 53605.1034490741 100008020 177.6 10000 181.5 181.5 179.6 177.6 1 1 1 1 1 0 0 200.1 200.1 202 0 PROCESSED 54320.5963888889 54247 54034.6891435185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000008 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG NGC 4945 NULL N NGC 4945 196.3681 -49.4152 305.27752827 13.39262005 96.1296 53750.3365625 53752.9655092593 100008030 95066.3 10000 95081.7 95129.7 95066.3 95106.3 2 2 2 2 1 0 0 84981.3 84981.3 227115.7 2 PROCESSED 54331.2095949074 54247 54040.3587615741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000008 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG NGC 4945 HXD N PSR1509-58 228.4798 -59.0943 320.34145971 -1.12587132 287.6342 53605.36 53606.8597569444 100009010 65161.8 60000 65161.8 65322.7 65242.7 65242.7 3 3 3 3 1 0 0 49735.7 49735.7 129529.8 4 PROCESSED 54330.3722222222 53705 53905.4622337963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000009 HXD spectrum and timing check CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG PSR1509-58 NULL N Crab Nebula 83.6267 22.0751 184.50282132 -5.75691305 86.8655 53607.0070833333 53607.1389814815 100010010 2937.9 5000 2937.9 2937.9 2937.9 2937.9 2 2 2 2 1 0 0 3438.7 3438.7 11381.9 0 PROCESSED 54323.3773148148 54247 54118.9886689815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.6336 21.9568 184.60669551 -5.81484075 86.8687 53607.1394560185 53607.2779282407 100010020 3653.3 5000 3653.3 3653.3 3653.3 3653.3 1 1 1 1 1 0 0 3806.7 3806.7 11934 0 PROCESSED 54320.7270717593 54247 54118.9337615741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.6105 22.3483 184.26290563 -5.62323625 86.8596 53607.2790509259 53607.5139583333 100010030 8112.9 5000 8112.9 8112.9 8112.9 8112.9 2 2 2 2 1 0 0 7835.9 7835.9 20264 1 PROCESSED 54320.9165625 54247 54118.9698958333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.6511 21.6763 184.85366771 -5.95118505 86.8795 53607.5153125 53607.7153472222 100010040 9580.6 5000 9580.6 9580.6 9580.6 9580.6 1 1 1 1 1 0 0 8178.3 8178.3 17248 0 PROCESSED 54326.880474537 54247 54118.943125 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.2708 21.9976 184.39063256 -6.07689385 86.7331 53607.7165162037 53607.9167361111 100010050 9346.9 5000 9346.9 9346.9 9346.9 9346.9 1 1 1 1 1 0 0 6653 6653 17287.9 0 PROCESSED 54326.8750347222 54247 54122.4223611111 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.5677 22.0135 184.52566905 -5.83608695 86.8444 53607.9175810185 53608.0695023148 100010060 4877.9 5000 4877.9 4877.9 4877.9 4877.9 1 1 1 1 1 0 0 5021.7 5021.7 13076 0 PROCESSED 54320.7265277778 54247 54122.4195486111 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.6922 22.0221 184.58047361 -5.73399538 86.8671 53608.0699768518 53608.2084027778 100010070 4089.9 5000 4089.9 4089.9 4089.9 4089.9 1 1 1 1 1 0 0 4228.3 4228.3 11925.9 0 PROCESSED 54323.0051041667 54247 54119.0149074074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.6222 22.1365 184.44846107 -5.72755512 86.8666 53608.2089236111 53608.316087963 100010080 3382 5000 3382 3382 3382 3382 1 1 1 1 1 0 0 3700.3 3700.3 9253.9 0 PROCESSED 54320.4816435185 54247 54119.0056134259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.5807 22.8483 183.82410841 -5.37832099 86.8677 53608.3175810185 53608.5139583333 100010090 6716 5000 6716 6716 6716 6716 1 1 1 1 1 0 0 6376.8 6376.8 16950.1 0 PROCESSED 54323.044537037 54247 54119.0235648148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.9887 22.0345 184.71743044 -5.49499441 86.8666 53608.5155902778 53608.7153472222 100010100 9694 5000 9694 9694 9694 9694 1 1 1 1 1 0 0 7581.2 7581.2 17247.9 0 PROCESSED 54326.8826967593 54247 54122.4242939815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.5122 24.0135 182.80375415 -4.80497322 86.8675 53608.7179976852 53608.930625 100010110 9480.5 5000 9480.5 9480.5 9480.5 9480.5 1 1 1 1 1 0 0 7363 7363 18336 0 PROCESSED 54320.855462963 54247 54118.98625 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.6374 21.9009 184.65605757 -5.84178049 86.8664 53608.9333217593 53609.069525463 100010120 4745.6 5000 4745.6 4745.6 4745.6 4745.6 2 2 2 2 1 0 0 5178.7 5178.7 11757.9 1 PROCESSED 54320.5947337963 54247 54118.9946180556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.5044 22.0116 184.49566519 -5.88665136 86.8658 53609.0701388889 53609.2014583333 100010130 4222 5000 4222 4222 4222 4222 1 1 1 1 1 0 0 4372.4 4372.4 11335.9 0 PROCESSED 54320.7159722222 54247 54119.0454282407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Crab nebula 83.7552 22.0249 184.60948321 -5.68314749 86.8656 53609.2022106482 53609.3125810185 100010140 3419 5000 3419 3419 3419 3419 1 1 1 1 1 0 0 3755.4 3755.4 9531.9 0 PROCESSED 54320.478275463 54247 54118.9983796296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000010 Crab nebula multi pointings CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab Offset 1 NULL N Galactic bulge 236.4313 -31.7013 340.99994533 17.99808229 283.5446 53609.4365856482 53611.060625 100011010 61133 70000 61133 61133 61133 61133 1 1 1 1 1 0 0 47983.4 47983.4 140282 2 PROCESSED 54324.9505439815 54247 54034.8288310185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000011 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Galactic bulge NULL N Eta Carinae 161.281 -59.6845 287.6040589 -0.62575348 343.8621 53611.0750347222 53612.0627546296 100012010 49782 40000 49790 49782 49782 49798 2 2 2 2 1 0 0 55960.7 55960.7 85252.9 0 PROCESSED 54329.4015162037 53705 53905.4648842593 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000012 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Eta Carinae NULL N N103B 77.2315 -68.7507 279.61119012 -34.36730962 73.8586 53612.0740162037 53613.0626273148 100013010 33064.6 40000 33064.6 33064.6 33064.6 33064.6 2 2 2 2 1 0 0 37281.4 37281.4 85405.9 1 PROCESSED 54327.767349537 54247 54034.8733449074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000013 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG N103B NULL N E0102-72 15.9813 -72.0378 301.56958331 -45.05740554 140.1798 53613.0710648148 53613.7640509259 100014010 24333.9 20000 24333.9 24333.9 24333.9 24333.9 2 2 2 2 1 0 0 24514.4 24514.4 59863.9 2 PROCESSED 54324.7676157407 53705 53905.4615740741 2.0.6.13 12 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000014 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG XIS monitor with E0102-72 NULL N Crab Nebula 83.6372 22.097 184.48946706 -5.73697 84.9994 53613.8323032407 53613.975787037 100015010 5658.7 5000 5658.7 5658.7 5658.7 5658.7 1 1 1 1 1 0 0 5790.7 5790.7 12387.9 0 PROCESSED 54320.6574884259 54247 54109.1053240741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000015 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD boresight check with Crab NULL N Crab Nebula 83.6296 22.1792 184.41590928 -5.69889955 84.9998 53613.9762152778 53614.1077314815 100015020 4950 5000 4950 4950 4950 4950 1 1 1 1 1 0 0 5117.8 5117.8 11359.9 0 PROCESSED 54320.5069791667 54247 54109.1090972222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000015 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD boresight check with Crab NULL N Crab Nebula 83.6449 22.0152 184.56274906 -5.77473152 84.9987 53614.1083449074 53614.1771759259 100015030 2100 5000 2100 2100 2100 2100 1 1 1 1 1 0 0 2307.4 2307.4 5943.9 0 PROCESSED 54322.7014467593 54247 54109.3966782407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000015 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD boresight check with Crab NULL N Crab Nebula 83.6442 22.0129 184.56435264 -5.77651077 84.9978 53614.830775463 53614.9098263889 100015040 2978.6 5000 2978.6 2978.6 2978.6 2978.6 1 1 1 1 1 0 0 3049.3 3049.3 6807.9 0 PROCESSED 54320.6198611111 54247 54109.1815625 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000015 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD boresight check with Crab NULL N Crab Nebula 83.5484 22.0881 184.45272098 -5.81121698 85.0004 53614.9103009259 53615.0418518518 100015050 5344.7 5000 5344.7 5344.7 5344.7 5344.7 1 1 1 1 1 0 0 5485.9 5485.9 11356 0 PROCESSED 54320.5288773148 54247 54109.1357986111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000015 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD boresight check with Crab NULL N Crab Nebula 83.727 22.1071 184.52563634 -5.6612791 84.9996 53615.0424652778 53615.2432175926 100015060 6525.6 5000 6525.6 6525.6 6525.6 6525.6 1 1 1 1 1 0 0 6759.9 6759.9 17340 0 PROCESSED 54320.5654398148 54247 54109.1715393518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000015 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD boresight check with Crab NULL N Cas A 350.8254 58.8156 111.72292809 -2.12474901 12.9937 53614.2486458333 53614.7640509259 100016010 27965 20000 27973 27973 27973 27965 2 2 2 2 1 0 0 24130 24130 44495.9 2 PROCESSED 54328.7484837963 53705 53905.4659606482 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000016 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Cas A NULL N Vega 279.2264 38.7699 67.43212753 19.23869014 301.7896 53615.367349537 53615.603587963 100017010 11398.5 10000 11406.5 11406.5 11406.5 11398.5 2 2 2 2 1 0 0 11575.1 11575.1 20403.9 0 PROCESSED 54323.0424305556 54247 53906.0764814815 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000017 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG XIS OBF check with Vega NULL N NEP 272.7884 65.9814 95.75202722 28.67554678 290.9299 53615.6136921296 53617.625162037 100018010 106201.5 100000 106201.5 106217.5 106249.5 106225.5 2 2 2 2 1 0 0 106125 106125 173571.8 3 PROCESSED 54389.5942013889 53705 53905.4636921296 2.1.6.14 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000018 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD background at North Ecliptic Pole NULL N SN1006 NE BG 226.7036 -41.3998 328.51405135 14.65073262 293.6503 53617.7018865741 53622.1668287037 100019010 44750.3 50000 44754.3 44754.3 44754.3 44750.3 2 2 2 2 1 0 0 37388.3 37388.3 385601.8 5 PROCESSED 54389.6071412037 54247 54035.4224768518 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000019 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG SN1006 observation with XIS and HXD NULL N SN1006 NE-Rim 225.9645 -41.7797 327.82254414 14.6038019 294.6606 53622.1683217593 53623.5835532407 100019020 42844.2 50000 42844.2 42852.6 42852.2 42848.2 2 2 2 2 1 0 0 37615.6 37615.6 122196 7 PROCESSED 54389.651412037 54247 54034.9646875 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000019 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG SN1006 observation with XIS and HXD NULL N SN1006 SW-Rim 225.5051 -42.0698 327.36692545 14.52303039 297.2712 53623.5862962963 53624.993287037 100019030 28524.5 50000 28532.5 28524.5 28540.9 28540.5 2 2 2 2 1 0 0 27008.2 27008.2 121551.9 5 PROCESSED 54389.6513888889 54247 54034.9697453704 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000019 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG SN1006 observation with XIS and HXD NULL N SN1006 SW BG 224.655 -42.4005 326.632731 14.54333558 310.4886 53624.9999189815 53626.0071643518 100019040 32333.4 50000 32333.4 32349.4 32341.4 32341.4 2 2 2 2 1 0 0 24673.6 24673.6 87015.9 5 PROCESSED 54389.7908912037 54247 54035.4482638889 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000019 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG SN1006 observation with XIS and HXD NULL N SN 1006 SW-Rim 225.4961 -42.0706 327.36052248 14.52564865 117.2713 53761.0914930556 53761.7155555556 100019050 28418.6 50000 28418.6 28418.6 28418.6 28418.6 2 2 2 2 1 0 0 24744.4 24744.4 53910 0 PROCESSED 54405.5687847222 54247 54040.4586689815 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000019 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG SN1006 observation with XIS and HXD XIS N SN1006 SW BG 224.6468 -42.4025 326.62625739 14.54451897 100.3489 53761.7199652778 53762.4752777778 100019060 27981.3 50000 27981.3 27989.3 27997.3 27997.3 2 2 2 2 1 0 0 29550.4 29550.4 65249.9 2 PROCESSED 54324.0084143518 54247 54040.5663541667 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000019 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG SN1006 observation with XIS and HXD XIS N Fornax Cluster 54.6395 -35.4918 236.7850293 -53.61976834 103.5002 53626.0756018518 53627.5002662037 100020010 76078.2 100000 76078.2 76078.2 76078.2 76078.2 2 2 2 2 1 0 0 71112.8 71112.8 123063.9 3 PROCESSED 54328.8938310185 54247 54035.4442013889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000020 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Fornax Cluster NULL N A0535+026 84.7243 26.3189 181.44092218 -2.64422146 83.608 53627.5694907407 53628.0418865741 100021010 21761 20000 21761 21761 21761 21761 2 2 2 2 1 0 0 21257.2 21257.2 40783.9 1 PROCESSED 54323.1530671296 54247 54035.0644444444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000021 We propose to observe the X-ray binary pulsar A0535+26. The main objectives is measuring changes in the cyclotron resonance energy in an outburst decay.It is known from another X-ray pulsar 4U0115+63 that the cyclotron resonance energy increased from 11 keV to 16 keV, as the luminosity decreased across a threshold luminosity of 4x10^37 erg/s. The flare of A0535+26 is a chance to know whether this behavior is the RULE among binary pulsars or an EXCEPTION. A0535+26 is fading down and will reach 30mCrab (5-100keV) on September 17, which is 5x10^36 erg/s. It is better to be observed as soon as possible, before it fades out. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG TOO Observation of A0535+026 NULL N Crab Nebula 83.6622 21.1838 185.27784655 -6.20565133 88.1125 53628.0468055556 53628.2988194444 100022010 12881 10000 12881 12881 12881 12881 1 1 1 1 1 0 0 12241 12241 21767.9 0 PROCESSED 54326.8429513889 54247 54109.2599768518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000022 Crab at 50arcmin off from the XIS aimpoint to study stray light. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab at 50 arcmin off NULL N Crab Nebula 82.7325 21.9883 184.12771921 -6.50224239 88.0978 53628.3006828704 53628.5835416667 100022020 10919.8 10000 10919.8 10919.8 10919.8 10919.8 1 1 1 1 1 0 0 6340.1 6340.1 24400 2 PROCESSED 54320.8114351852 54247 54109.1486342593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000022 Crab at 50arcmin off from the XIS aimpoint to study stray light. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab at 50 arcmin off NULL N Crab Nebula 84.5289 22.0469 184.974122 -5.06424795 87.5879 53629.0921759259 53629.368275463 100022030 12824.4 10000 12840.4 12832.4 12824.4 12848.4 2 2 2 2 1 0 0 10351.8 10351.8 23824 1 PROCESSED 54326.8580208333 54247 54109.1621527778 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000022 Crab at 50arcmin off from the XIS aimpoint to study stray light. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab at 50 arcmin off NULL N Crab Nebula 83.6282 22.0761 184.5027205 -5.75520363 87.79 53628.5852199074 53628.8265393518 100023010 11997.8 10000 11997.8 11997.8 11997.8 11997.8 1 1 1 1 1 0 0 10513.2 10513.2 20823.9 0 PROCESSED 54322.5218865741 54247 54109.2268287037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000023 Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab at nominal positions NULL N Crab Nebula 83.6309 22.0151 184.55585082 -5.78574816 87.8466 53628.8269212963 53629.0904976852 100023020 12527.1 10000 12531.1 12527.1 12536.4 12535.1 2 2 2 2 1 0 0 13352.9 13352.9 22764 1 PROCESSED 54322.5040856482 54247 54109.193599537 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000023 Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Crab at nominal positions NULL N NGC 2110 88.0444 -7.458 212.92660512 -16.54877043 103.4188 53629.3796296296 53631.8308333333 100024010 101748.7 100000 101926.5 103760.1 101748.7 102148.3 2 2 2 2 1 0 0 86043.3 86043.3 211755.8 4 PROCESSED 54389.7523726852 54247 54035.4624189815 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000024 The Narrow Emission Line Galaxy NGC 2110 was the brightest AGN in the initial BAT survey release (BAT flux of 2.1E-10 erg/cm2/sec) visible to Suzaku during Sept./Oct., and is still currently bright in BAT. A 2003 RXTE observation yielded F_2-10 keV = 4E-11 erg/cm2/sec. The source is currently almost 3 times brighter than during the SAX observations. The main goals are to measure the high energy cutoff and to place a strong limit on the presence of reflection. The Compton reflection hump is weak in SAX data (suggesting that the Fe K line originates in Compton-thin material). Determining the strength of the reflection component is critical for constraining the geometry of the accreting material. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Narrow Emission Line Galaxy NGC 2110 NULL N BD +30 3639 293.6887 30.5051 64.77556877 5.01383279 277.8713 53634.3814930556 53635.2473842593 100025010 35214.6 40000 35230.6 35230.6 35214.6 35222.6 2 2 2 2 1 0 0 33372.8 33372.8 74803.9 1 PROCESSED 54324.5771527778 54247 54035.4664583333 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000025 The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Observation of planetary nebula BD +30 3639 NULL N BD +30 3639 293.6993 30.5065 64.78119899 5.00649051 237.7342 53676.9934837963 53677.8230324074 100025020 31138.4 40000 31138.4 31162.4 31146.4 31154.4 2 2 2 2 1 0 0 27125.8 27125.8 71638 1 PROCESSED 54324.7078703704 54247 54037.1080902778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000025 The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Observation of planetary nebula BD +30 3639 NULL N RXJ1713.7-3946 258.074 -39.935 347.05133682 -0.37925502 269.9977 53639.6563194444 53641.2960648148 100026010 68495.9 80000 68495.9 68565.3 68511.9 68525.3 2 2 2 2 1 0 0 56238.2 56238.2 141661.9 0 PROCESSED 54329.6084606482 54247 54037.0750694445 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000026 RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Observation of RXJ1713.7-3946 NULL N RXJ1713-3946-BKGD1 257.3853 -38.8228 347.63223985 0.70836337 270.0091 53638.7997685185 53639.6542708333 100026020 34928.4 40000 34928.4 34928.4 34928.4 34928.4 2 2 2 2 1 0 0 28371.3 28371.3 73819.9 0 PROCESSED 54322.9338425926 54247 54035.5347453704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000026 RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Observation of RXJ1713.7-3946 NULL N RXJ1713-3946-BKGD2 257.2742 -41.0338 345.80577047 -0.54060643 270.0033 53641.2980671296 53642.1843055556 100026030 37513.2 40000 37537.2 37529.2 37513.2 37513.2 2 2 2 2 1 0 0 31898.2 31898.2 76565.9 0 PROCESSED 54324.5779166667 54247 54035.6187268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000026 RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Observation of RXJ1713.7-3946 NULL N Sgr_A_East 266.5146 -28.9267 0.05802898 -0.07696746 264.7152 53636.3044560185 53637.462025463 100027010 44785 50000 44801 44852.3 44785 44828.3 2 2 2 2 1 0 0 37854.3 37854.3 100013.9 1 PROCESSED 54327.4356365741 54247 54035.502662037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Observation of Galactic Center Region NULL N Sgr_A_west 266.3057 -29.1697 359.75546849 -0.04768885 264.9601 53637.5953356482 53638.7273032407 100027020 42814.8 50000 42814.8 42814.8 42814.8 42814.8 2 2 2 2 1 0 0 36091 36091 97800 0 PROCESSED 54324.666724537 54247 54035.5135532407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Observation of Galactic Center Region NULL N 1A1742-294(GC_BGD_1) 266.5264 -29.516 359.56008755 -0.392308 264.8664 53637.463287037 53637.527962963 100027030 2066.3 5000 2066.3 2066.3 2066.3 2066.3 1 1 1 1 1 0 0 1887.7 1887.7 5584 0 PROCESSED 54320.6100578704 54247 54035.4639583333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Observation of Galactic Center Region NULL N KS1741-293(GC_BGD_2) 266.2069 -29.3515 359.55541243 -0.06909433 265.0174 53637.5288541667 53637.5946296296 100027040 1937 5000 1937 1937 1937 1937 1 1 1 1 1 0 0 1763.7 1763.7 5680 0 PROCESSED 54320.4688425926 54247 53907.393275463 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Observation of Galactic Center Region NULL N 1E1743.1-2843(GC_BGD_3) 266.592 -28.6516 0.32828705 0.00813221 264.88 53638.7286111111 53638.793275463 100027050 1984.6 5000 1984.6 1984.6 1984.6 1984.6 1 1 1 1 1 0 0 1793.4 1793.4 5567.9 0 PROCESSED 54318.5558912037 54247 53905.6343055556 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Observation of Galactic Center Region NULL N HESS J1616-508 244.1248 -50.8971 332.40352084 -0.15000913 282.8476 53632.5000231482 53633.8183333333 100028010 41352 50000 41352 41376 41352 41368 2 2 2 2 1 0 0 35373.1 35373.1 113889.9 0 PROCESSED 54328.1468634259 54247 54035.4361111111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000028 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG New HESS sources and the Galactic ridge Background NULL N HESS J1616-508_BGD1 243.666 -51.1742 332.00349288 -0.15039556 283.0062 53631.9497222222 53632.4990856482 100028020 19327.7 25000 19327.7 20630 19360 19632.3 1 1 1 1 1 0 0 16642.6 16642.6 47447.9 0 PROCESSED 54320.8714583333 54247 54035.1692476852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000028 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG New HESS sources and the Galactic ridge Background NULL N HESS J1616-508_BGD2 244.4656 -50.6883 332.70353325 -0.14997577 283.1793 53633.8196412037 53634.3120833333 100028030 21873.5 25000 21889.5 21889.5 21881.5 21873.5 1 1 1 1 1 0 0 18206.3 18206.3 42535.9 0 PROCESSED 54322.7236111111 54247 54035.4698842593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000028 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG New HESS sources and the Galactic ridge Background NULL N GRO J1655-40 253.5027 -39.8455 344.98315976 2.45489032 268.0237 53635.3140625 53636.2968055556 100029010 35222.8 40000 0 35233.6 35222.8 35230.8 0 1 2 2 1 0 0 28731.5 28731.5 84901.9 1 PROCESSED 54327.2611689815 54247 54035.4940625 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000029 We propose to observe GRO J1655-40, a transient galactic black hole candidate. With M=~7 Msolar and distinct radio lobes, GRO J1655-40 has been classified as a microquasar. It was highly variable during the first few years after its discovery while showing irregular flaring and a wide range of continuum states. Discrete Fe K absorption structure was observed with ASCA. In the summer of 1997 it entered an extended quiescence that lasted for ~8 years. In March 2005 it became active again and XMM & Chandra have observed it since. Only Suzaku can provide the broadband sensitivity required to map the Fe K structure and the continuum as they change. GRO J1655-40 is rapidly declining and must be observed soon before it reenters quiescence. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG GRO J1655-40 NULL N A 2218 249.0001 66.203 97.724401 38.11892096 242.3617 53644.3643402778 53645.3446643518 100030010 43362.9 50000 43362.9 44717.3 43425.3 43824.8 2 2 2 2 1 0 0 41491.8 41491.8 84678 1 PROCESSED 54324.0657986111 54247 54035.7677314815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000030 Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG A2218 and its offset observation NULL N A2218_offset 244.4769 65.4468 97.72059475 40.11912915 237.1965 53645.3474537037 53646.32375 100030020 44859.2 50000 44859.2 46190.7 44914.1 45374.7 2 2 2 2 1 0 0 42536.6 42536.6 84343.9 0 PROCESSED 54412.4325115741 54247 54036.969224537 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000030 Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG A2218 and its offset observation NULL N NGC3516 166.7299 72.5779 133.2179652 42.40001774 148.9366 53655.5813541667 53658.3801388889 100031010 134469.6 150000 134509.6 134595.6 134509.6 134469.6 2 2 2 2 1 0 0 122818 122818 241684.8 0 PROCESSED 54331.3324421296 54247 54036.4704976852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000031 NGC 3516 is one of the brightest Seyfert 1s seen in BAT currently visible to Suzaku. Recent BAT and RXTE observations show that this source is ~2-3 mCrb in the 2-10 keV band and ~4-5 mCrb in 15-100 keV. NGC 3516 is currently much brighter than when XMM observed it in 2000 (e.g., it has since returned to "typical" flux). This source's Fe K line and Compton reflection hump are both quite strong (e.g., as seen with SAX; R is ~1.8 in SAX data). CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG NGC 3516 NULL N ULXs in NGC 1313 49.5245 -66.5352 283.41323765 -44.63106544 172.6337 53658.556400463 53659.6252777778 100032010 32878 40000 32878 32878 32878 32878 1 1 1 1 1 0 0 30380 30380 92343.9 1 PROCESSED 54327.0733101852 54247 54036.1929398148 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000032 We propose Suzaku observation of a nearby (4.5 Mpc) galaxy NGC 1313 hosting two prototypical ULXs. These ASCA specta of many ULXs were described with a "high temperature diskbb" model, spectra obtained with XMM (and Chandra) prefer a "power-law plus low-temperature disk" modeling. The superior 5-10 keV sensitivity of Suzaku allows us to examine whether the spectra of luminous ULXs indeed exhibit a turn-over around 5 keV or extend up to 10 keV. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG ULXs in NGC 1313 NULL N M82-Wind 148.8893 69.7655 141.33880284 40.49464345 137.7608 53647.5072800926 53648.1418287037 100033010 32327.4 100000 32327.4 32327.4 32327.4 32327.4 2 2 2 2 1 0 0 30222.4 30222.4 54802.1 0 PROCESSED 54327.0792592593 54247 54037.0057175926 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000033 We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Largely Extended Emission (~12kpc) around M82 NULL N M82-Wind 148.894 69.7643 141.33883884 40.49666381 146.246 53662.0401273148 53662.9390393518 100033020 40358.6 100000 40358.6 40382.6 40358.6 40366.6 2 2 2 2 1 0 0 38353.3 38353.3 77658 0 PROCESSED 54324.7042708333 54247 54036.4196296296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000033 We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Largely Extended Emission (~12kpc) around M82 NULL N M82-Wind 148.8885 69.7652 141.33933547 40.4945935 137.7608 53670.4681134259 53671.1002199074 100033030 28363.8 100000 28379.8 28379.8 28371.8 28363.8 2 2 2 2 1 0 0 25812.1 25812.1 54604 1 PROCESSED 54320.7539930556 54247 54036.8639467593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000033 We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Largely Extended Emission (~12kpc) around M82 NULL N A 3376 90.5561 -39.9584 246.50686261 -25.98989573 107.6124 53649.6153703704 53653.4495833333 100034010 118779.2 150000 118779.2 121737.3 118849.8 119335.7 2 2 2 2 1 0 0 100540.1 100540.1 331253.7 3 PROCESSED 54331.7007060185 54247 54109.6396990741 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000034 Abell 3376 (z=0.046) is a merging cluster with a T=4 keV (*3) hosting a pair of strong radio halos (see figure). It is one of the few clusters from which BeppoSAX positively detected excess hard X-rays (Nevalainen et al. ApJ 608, 166, 2004). Because of the relatively low temperature, the HXD-PIN energy band is expected to be relatively free from thermal emission, making this object ideal to the search for non-thermal signals. We expect the non-thermal flux to be 4-5% of the PIN background at 20 keV, and a 150 ksec on-source exposure would be needed to securely detect this. To know the current background over the full COR range, an off-source exposure for one day or a ~40 ksec exposure onto a very soft source, would be required immediately before or after the on-source data acquisition. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Diffuse Hard X-rays from Clusters NULL N Her X-1 254.465 35.3306 58.13562438 37.51514805 249.5714 53648.6450462963 53649.4341898148 100035010 36123.5 40000 36923.5 36123.5 36923.5 36923.5 2 1 2 2 1 0 0 33322.9 33322.9 68178 0 PROCESSED 54412.4794560185 54247 54036.0084375 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000035 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG HXD Performance Verification using Her X-1 NULL N CYG X-1 299.5907 35.1892 71.32454904 3.06010347 276.9898 53648.2025347222 53648.6335532407 100036010 18213 20000 18213 18213 18213 18213 1 1 1 1 1 0 0 18145.7 18145.7 37229.9 0 PROCESSED 54412.5121412037 54247 54037.7278819444 2.1.6.15 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000036 We propose to probe the geometry of optically-thick accretion disks which should exist around a BH even in the hard state and to verify the HXD performance to thermal cut-off in hard X-rays expected from AGN. The 1st may be done by measuring the cool disk emission with the XIS-BI, resolving the fluorescent Fe-K line with the XIS-FI and detecting the reflection continuum with the HXD. Since these features are thought to come from the optically-thick disk a simultaneous measurement will for the 1st time allow for self-consistent constraining of the disk geometry in the hard state. Cyg X-1 is the best & most secure object for this stufy and is now in the low/hard state. A 20 ks Suzaku obs. is sufficient to get a fine spectrum up to 300 keV & to determine the cutoff with a high significance. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Cyg X-1 in the low state NULL N Sgr_A_west 266.3063 -29.1685 359.75676556 -0.04750971 264.9604 53642.1914467593 53643.187025463 100037010 43741.2 50000 43741.2 43749.2 43749.2 43749.2 2 2 2 2 1 0 0 39394.1 39394.1 86013.9 0 PROCESSED 54325.098900463 54247 54035.6663310185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N 1A1742-294(GCBGD1) 266.5239 -29.5135 359.5610912 -0.38914955 264.8673 53643.1880092593 53643.2536921296 100037020 3273 5000 3281 3273 3288.7 3281 1 1 1 1 1 0 0 3091.1 3091.1 5671.9 0 PROCESSED 54389.6632638889 54247 54035.5547453704 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N KS1741-293(GCBGD2) 266.2067 -29.3539 359.55327497 -0.0701996 265.0162 53643.254537037 53643.3203703704 100037030 2970 5000 2994 2986 2978 2970 2 2 2 2 1 0 0 2824.4 2824.4 5679.9 0 PROCESSED 54389.6703819444 54247 54035.7774189815 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N Sgr_A_East 266.5133 -28.9266 0.05752244 -0.07594372 264.7159 53643.3215393518 53644.2648611111 100037040 42917.6 50000 42957.6 42961.6 42917.6 42939.2 2 2 2 2 1 0 0 39453.3 39453.3 81494 1 PROCESSED 54389.7149305556 54247 54035.7619675926 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N 1E1743.1-2843 GCBGD3 266.5944 -28.6526 0.32852719 0.00581314 264.8798 53644.2657523148 53644.3162268518 100037050 2400 5000 2400 2400 2400 2400 2 2 2 2 1 0 0 2232.9 2232.9 4353.9 0 PROCESSED 54320.5997453704 54247 54056.1970833333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N Sgr_B2 266.8775 -28.4435 0.63628385 -0.09835114 265.3727 53653.5194560185 53655.2954050926 100037060 76596.6 100000 76628.6 76644.6 76596.6 76628.6 2 2 2 2 1 0 0 70819.2 70819.2 153431.9 0 PROCESSED 54329.7041666667 54247 54036.2262731482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N Sgr_B2_BGD 267.0943 -28.1356 0.99854005 -0.10262599 269.0208 53655.2988888889 53655.4620833333 100037070 9161.2 10000 9161.2 9164.3 9164.3 9163.2 2 2 2 2 1 0 0 9536.4 9536.4 14092 0 PROCESSED 54320.6769560185 54247 54036.0749884259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000037 NULL CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Suzaku Obseration of Galactic Center region 2 NULL N NORTH POLAR SPUR 260.5905 4.7489 26.83412197 21.95376599 264.1143 53646.4785763889 53647.4515277778 100038010 43068.9 50000 43148.9 44212.9 43068.9 43292.9 2 2 2 2 1 0 0 40771.5 40771.5 84001.9 0 PROCESSED 54412.4658680556 54247 54035.8928009259 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000038 We propose to observe the North Polar Spur for 100 ksec. The main objectives are below (1) Search for emission lines of N and C that originates from low kT emission (2) Precisely determine the abundance of the NPS The measurement of N and C lines will be the first for XIS. This is also the first for extended sources. The first trial to measure the emission from the C-band (below 0.3keV) by using BI. This will be a guide line how to use the C-band data. Since the C-band intensity is already known, this will be the first calibration of the BI at low energy. The scientific objectives are already given in the mail distributed in the swg. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG North Polar Spur NULL N GRS1915+105 288.8014 10.9368 45.35928754 -0.22611181 260.5762 53659.6951967593 53661.9724305556 100039010 84777.7 80000 85063.1 86430.5 85071.1 84777.7 3 3 3 3 1 0 0 68862.3 68862.3 196733.8 2 PROCESSED 54332.4893402778 54247 54043.8117476852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000039 This observation will be performed as a part of the big multiwavelength campain including Suzaku, VLA, Integral, RXTE, and Spitzer. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG Campaign of coordinated observation of GRS 1915+105 NULL N MKN 3 93.8839 71.0477 143.2836301 22.71631463 71.8326 53665.0848263889 53667.2682175926 100040010 95026.5 100000 95026.5 95077.2 95045.2 95034.5 2 2 2 2 1 0 0 91344.1 91344.1 188629.9 0 PROCESSED 54329.9908796296 54247 53906.4896759259 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000040 Mkn 3 is the second brightest Compton-thick Sy 2 currently visible with Suzaku. The broadband spectrum of Mkn 3, as probed by previous SAX and Chandra observations, is dominated by a reflection component (Compton hump strength R is near 1), but there is also evidence for a strongly absorbed hard X-ray power law that may be direct emission from the obscured nucleus, filtering through Compton-thick material (such as the molecular torus). CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG MKN 3 HXD N RXJ1856.5-3754 284.1498 -37.9103 358.59888263 -17.21635309 269.4259 53667.2829976852 53669.4793287037 100041010 76254.8 80000 0 76254.8 0 0 0 2 0 0 1 0 0 62621.7 62621.7 189720 3 PROCESSED 54330.4892476852 54247 54037.2294791667 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000041 We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG LOW ENERGY QE CALIBRATION OF XIS XIS N RXJ1856.5-3754 284.1433 -37.91 358.59722216 -17.21146697 84.0127 53817.9388078704 53819.4433217593 100041020 79169 80000 79177 79169 79177 79177 2 2 2 2 1 0 0 53209.9 53209.9 129975.9 1 PROCESSED 54327.6521064815 54247 54042.2967824074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000041 We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. CALIBRATION 1 A SWG NULL NULL NULL JAP 0 SWG LOW ENERGY QE CALIBRATION OF XIS XIS N CAS A 350.8729 58.8094 111.74406014 -2.13880346 214.7372 53768.5363657407 53768.833599537 100043010 0 10000 0 0 0 0 0 0 0 0 1 0 0 10326.8 10326.8 25673.9 1 PROCESSED 54405.6122569444 54247 54040.7488888889 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001097 We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 0 SWG XIS FLIGHT CAIBRATION PLAN XIS N CAS A 350.8761 58.8091 111.74552355 -2.13963884 214.5537 53783.6003472222 53783.9218055556 100043020 14155 10000 14155 14155 14155 14155 1 1 1 1 1 0 0 17371.3 17371.3 27768 0 PROCESSED 54322.8381018518 54247 54041.4627893518 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001097 We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 0 SWG XIS FLIGHT CAIBRATION PLAN XIS N E0102-72 15.9926 -72.0236 301.56327722 -45.07133229 226.8326 53720.0716203704 53723.4377199074 100044010 59731 20000 59735 125919.5 59731 59737 3 3 3 3 1 0 0 115330.2 115330.2 290803.7 1 PROCESSED 54331.8694907407 54247 54119.7612615741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001097 We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 0 SWG XIS FLIGHT CAIBRATION PLAN NULL N E0102-72 16.0206 -72.0231 301.55102123 -45.07123322 281.396 53752.9742708333 53755.3752199074 100044020 41260.5 20000 41268 41852.4 41260.5 41361 3 4 3 4 1 0 0 99793.5 99793.5 207429.8 3 PROCESSED 54331.0584375 54247 54040.6979513889 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001097 We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 0 SWG XIS FLIGHT CAIBRATION PLAN XIS N E0102-72 16.027 -72.0223 301.54815221 -45.07189388 294.0751 53768.8467592593 53769.4065393518 100044030 20827.7 20000 20835.7 20843.7 20843.7 20827.7 2 2 2 2 1 0 0 20268.8 20268.8 48360 1 PROCESSED 54405.6412268518 54247 53905.6764351852 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001097 We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 0 SWG XIS FLIGHT CAIBRATION PLAN XIS N ETA CARINAE 161.248 -59.6859 287.58997588 -0.63475906 156.124 53769.4163194444 53769.9481944444 100045010 21367.8 20000 21367.8 21367.8 21367.8 21367.8 2 2 2 2 1 0 0 18145.8 18145.8 45945.9 1 PROCESSED 54326.9105902778 54247 54040.9846643518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001097 We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 0 SWG XIS FLIGHT CAIBRATION PLAN XIS N LOCKMANHOLE 163.4063 57.6108 148.98193179 53.14624927 119.611 53688.2372337963 53689.8300694444 100046010 76980.6 100000 76980.6 77044.6 77012.6 77020.6 2 2 2 2 1 0 0 94510.7 94510.7 137607.9 3 PROCESSED 54329.2318634259 54247 54037.5889814815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001098 We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background. CALIBRATION 1 A KOKUBUN MOTOHIDE NULL NULL JAP 0 SWG BACKGROUND ESTABLISHMENT OF HXD XIS N GALACTIC CENTER 266.5135 -28.9269 0.05735731 -0.07624929 270.2495 53986.0995833333 53987.3793402778 100048010 63007.9 50000 63007.9 63007.9 63007.9 63007.9 2 2 2 2 1 0 0 60322.8 60322.8 110567.9 2 PROCESSED 54325.0017824074 54526 54056.4849189815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 SWG XIS FLIGHT CALIBRATION PLAN XIS N CYGNUS LOOP 314.0345 31.9311 75.67403832 -8.61676541 64.2261 53884.1556018518 53884.3793865741 100049010 8380.5 10000 8380.5 8380.5 8380.5 8380.5 1 1 1 1 1 0 0 6021.1 6021.1 19304 0 PROCESSED 54405.7350925926 54258 54059.411099537 2.1.6.15 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 SWG XIS FLIGHT CALIBRATION PLAN SPE N CYGNUS LOOP 314.0785 32.0438 75.78588033 -8.57358243 64.2263 53884.3796759259 53884.6086342593 100049020 7892.8 10000 7892.8 7892.8 7892.8 7892.8 2 2 2 2 1 0 0 7452 7452 19769.9 0 PROCESSED 54405.7474074074 54258 54088.8429513889 2.1.6.15 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 SWG XIS FLIGHT CALIBRATION PLAN SPE N CYGNUS LOOP 313.9494 32.0818 75.74490282 -8.46508453 64.2292 53884.6089236111 53884.8377777778 100049030 11697.1 10000 11705.1 11697.1 11705.1 11705.1 2 2 2 2 1 0 0 12268.8 12268.8 19772 0 PROCESSED 54405.7510763889 54258 54052.4915046296 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 SWG XIS FLIGHT CALIBRATION PLAN SPE N CYGNUS LOOP 313.9037 31.9696 75.63250703 -8.50670526 64.2245 53884.8380671296 53885.0891666667 100049040 11765.6 10000 11781.6 11781.6 11773.6 11765.6 1 1 1 1 1 0 0 9788 9788 21687.9 0 PROCESSED 54405.7566435185 54258 54052.5201157407 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 SWG XIS FLIGHT CALIBRATION PLAN SPE N HER X-1 254.4224 35.4083 58.22535664 37.56185232 67.8783 53823.7669907407 53824.640462963 101001010 33062.1 40000 33062.1 38804.5 33062.1 33070.1 4 3 4 4 1 0 0 26222.8 26222.8 75437.9 0 PROCESSED 54327.3297800926 53826 53906.9875925926 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015002 The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO. CALIBRATION 1 A KOKUBUN MOTOHIDE NULL NULL JAP 1 AO1 SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATION HXD N LOCKMAN HOLE 162.9366 57.2557 149.70344314 53.20093146 281.8721 53872.7389583333 53874.7939583333 101002010 80398.2 80000 80398.2 80406.2 80406.2 80406.2 3 3 3 3 1 0 0 88854 88854 177513.8 4 PROCESSED 54329.1568865741 53826 53927.7689814815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015003 We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD. CALIBRATION 1 A KOKUBUN MOTOHIDE NULL NULL JAP 1 AO1 SUZAKU OBSERVATION OF LOCKMANHOLE XIS N CRAB 83.6569 21.9577 184.61755594 -5.79610428 250.9424 53830.5463425926 53831.5925115741 101003010 37832.3 40000 37832.3 37853.3 37832.3 37832.3 1 1 1 1 1 0 0 30989 30989 90379.9 1 PROCESSED 54328.6719444444 53826 53907.1306944445 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015004 Crab cal at the XIS and HXD nominal positions. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB HXD N CRAB 83.6371 22.0108 184.56259415 -5.78319491 253.3318 53824.652650463 53825.1668865741 101004010 16363.2 20000 16363.2 16372.8 16365 16365 1 1 1 1 1 0 0 9761.6 9761.6 44426 0 PROCESSED 54324.0120023148 53826 53906.0621875 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015004 Crab cal at the XIS and HXD nominal positions. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB XIS N CRAB 83.6368 22.0131 184.56049184 -5.78219867 250.943 53829.1296643518 53829.5974305556 101004020 19138.9 20000 19138.9 19145.8 19138.9 19138.9 1 1 1 1 1 0 0 13283.1 13283.1 40411.9 1 PROCESSED 54323.9096412037 53826 53906.6409375 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015004 Crab cal at the XIS and HXD nominal positions. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB XIS N E0102.2-7219 16.0331 -72.0338 301.54662861 -45.06029066 8.2024 53841.404212963 53841.9793865741 101005010 21324 40000 21340 21324 21332 21340 1 1 1 1 1 0 0 16683.1 16683.1 49663.9 0 PROCESSED 54323.0970949074 53826 53905.6938425926 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 16.0278 -72.0394 301.54948943 -45.0548182 34.4136 53876.719525463 53877.1793287037 101005020 18161.9 20000 18161.9 18193.9 18161.9 18193.9 2 1 2 1 1 0 0 17763.3 17763.3 39719.9 0 PROCESSED 54323.0878703704 53826 53926.1422222222 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 16.0175 -72.0405 301.55408267 -45.05394165 60.6353 53912.8662731482 53913.4245833333 101005030 21675.8 20000 21715.8 21683.8 21715.8 21675.8 2 4 2 4 1 0 0 35062.6 35062.6 48203.9 0 PROCESSED 54326.9764467593 53826 53928.4586458333 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 15.9978 -72.0424 301.56284618 -45.05246644 92.9794 53933.2656597222 53933.9030439815 101005040 22063.4 20000 22063.4 22103.4 22063.4 22095.4 4 2 4 2 1 0 0 20982.3 20982.3 55047.9 1 PROCESSED 54327.0259606482 53826 53942.4630092593 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 15.9824 -72.0369 301.56901677 -45.05828014 133.8232 53972.2052662037 53973.3933333333 101005050 68363.2 20000 68987.2 68363.2 68987.2 68971.2 5 5 5 6 1 0 0 68002.4 68002.4 102633.9 1 PROCESSED 54329.2787962963 53826 54020.9929050926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 15.9812 -72.0315 301.5690149 -45.06369281 159.2453 53997.2263425926 53997.562662037 101005060 10790.7 40000 10806.7 10806.7 10790.7 10798.7 2 2 2 2 1 0 0 10322.3 10322.3 29050 0 PROCESSED 54323.1288425926 53826 54021.1325115741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 15.9801 -72.0277 301.56912514 -45.06750714 192.8855 54029.650625 54030.2265625 101005070 37130.5 40000 37170.5 37130.5 37170.5 37162.5 3 3 3 3 1 0 0 36471.6 36471.6 49760 0 PROCESSED 54323.2554513889 53826 54055.5631828704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0029 -72.0223 301.55865958 -45.07240987 252.2709 54082.7869907407 54083.1279976852 101005090 28226 20000 28226 28226 0 28226 1 1 0 1 1 0 0 23054.6 23054.6 29455.9 0 PROCESSED 54320.7912037037 53826 54094.5930324074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0137 -72.0201 301.5537348 -45.07437383 265.9905 54115.1395023148 54115.6655555556 101005100 22614 20000 22614 22614 0 22614 1 1 0 1 1 0 0 19149.6 19149.6 45424 1 PROCESSED 54323.0598148148 53826 54132.8509490741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 16.0273 -72.0256 301.54834682 -45.06859544 302.8131 54141.9262384259 54142.812662037 101005110 36093.8 20000 36101.8 36093.8 0 36101.8 1 1 0 1 1 0 0 52703.8 52703.8 76575.9 1 PROCESSED 54322.7344675926 53826 54153.2227430556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0373 -72.0314 301.54456169 -45.06259438 341.0006 54177.8828587963 54178.2994675926 101005120 18242 20000 18242 18250 0 18258 1 1 0 1 1 0 0 14755.1 14755.1 35983.9 0 PROCESSED 54320.5929513889 53826 54185.4459027778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N PKS2155-304 329.7138 -30.2259 17.72949775 -52.24318888 57.9013 53856.2600925926 53857.2501041667 101006010 38551.5 30000 38551.5 38551.5 38551.5 38551.5 2 2 2 2 1 0 0 23947.6 23947.6 85514.1 2 PROCESSED 54327.1750694444 53826 53913.2773842593 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N RXJ1856.5-3754 284.1489 -37.9077 358.6011477 -17.21474589 254.2953 54028.5128472222 54029.6405208333 101009010 40784.1 40000 40784.1 40784.1 40784.1 40784.1 2 2 2 2 1 0 0 35169.9 35169.9 97403.9 1 PROCESSED 54324.6576851852 53826 54055.4732523148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N CRAB 83.6301 22.0172 184.55366892 -5.78525038 85.7026 53983.2227430556 53983.8196643518 101010010 20717.5 20000 20877.5 20717.5 20893.5 20885.5 3 2 3 3 1 0 0 19607.1 19607.1 51569.9 1 PROCESSED 54323.921412037 53826 54024.6695833333 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015014 HXD cal. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 1 AO1 CRAB CAL FOR HXD ON 2006 AUTUMN XIS N THE CRAB OFFSETS 83.6209 22.1323 184.45137768 -5.73082135 85.7132 53983.8199537037 53983.8891087963 101011010 3348 2000 3348 3348 3348 3348 1 1 1 1 1 0 0 3676 3676 5967.9 0 PROCESSED 54320.5337268518 53826 54104.4418287037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6229 22.105 184.47554642 -5.74387633 85.7146 53983.889212963 53983.9516087963 101011020 3350 2000 3350 3350 3350 3350 1 1 1 1 1 0 0 3004 3004 5383.9 0 PROCESSED 54320.5378587963 53826 54104.4374189815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6254 22.076 184.50140903 -5.75744861 85.7164 53983.951712963 53984.0904976852 101011030 6703 2000 6703 6703 6703 6703 1 1 1 1 1 0 0 5445.8 5445.8 11983.9 0 PROCESSED 54320.5911226852 53826 54104.972650463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS HXD N THE CRAB OFFSETS 83.6274 22.0499 184.52456216 -5.76985767 85.719 53984.0906018518 53984.1529976852 101011040 3353 2000 3353 3353 3353 3353 1 1 1 1 1 0 0 2414 2414 5383.9 0 PROCESSED 54320.5453703704 53826 54104.4143518518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6323 21.9916 184.57650041 -5.79723168 85.7244 53984.1531944445 53984.2224421296 101011050 3355 2000 3355 3355 3355 3355 1 1 1 1 1 0 0 2187 2187 5975.9 0 PROCESSED 54320.5475347222 53826 54104.4478587963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6331 21.9589 184.60466298 -5.81410844 87.5062 53996.8758680556 53996.9515509259 101011060 3368 2000 3368 3368 3368 3368 1 1 1 1 1 0 0 2716 2716 6527.9 0 PROCESSED 54320.4950115741 53826 54104.4231481482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6338 21.931 184.62870178 -5.82849289 87.5103 53996.9516550926 53997.0140509259 101011070 2636 2000 2636 2636 2636 2636 1 1 1 1 1 0 0 2157 2157 5383.9 0 PROCESSED 54320.4840046296 53826 54104.4160069444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6343 21.9041 184.65179297 -5.84249768 87.5094 53997.0141550926 53997.0834953704 101011080 2251 2000 2251 2251 2251 2251 1 1 1 1 1 0 0 2275 2275 5983.9 1 PROCESSED 54320.6079861111 53826 54104.4469675926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.7555 22.0251 184.60946275 -5.68280554 87.8963 53997.0840625 53997.1529282407 101011090 1895 2000 1895 1895 1895 1895 2 2 2 2 1 0 0 2081.5 2081.5 5945.9 0 PROCESSED 54320.6105092593 53826 54104.4517708333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.7241 22.023 184.59560566 -5.70852703 87.5484 53997.1534490741 53997.2154513889 101011100 1545 2000 1545 1545 1545 1545 1 1 1 1 1 0 0 1806 1806 5356 0 PROCESSED 54320.4757060185 53826 54104.4337731482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6927 22.0229 184.58004352 -5.7331758 85.756 53984.5680092593 53984.6252199074 101011110 2635.4 2000 2635.4 2635.4 2635.4 2635.4 1 1 1 1 1 0 0 2457.3 2457.3 4942 0 PROCESSED 54320.6459375 53826 54104.4321527778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.6616 22.0194 184.56751127 -5.75940556 85.7473 53984.6253703704 53984.6876967593 101011120 2976.1 2000 2976.1 2976.1 2976.1 2976.1 2 2 2 2 1 0 0 2802 2802 5380 0 PROCESSED 54320.6675115741 53826 54104.4254513889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.5991 22.0137 184.54117278 -5.81139714 85.7249 53984.6879398148 53984.7572222222 101011130 3366.1 2000 3366.1 3366.1 3366.1 3366.1 1 1 1 1 1 0 0 3190 3190 5983.9 0 PROCESSED 54320.6656712963 53826 54104.4575 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.5675 22.0116 184.5271819 -5.8372614 85.7131 53984.7573263889 53984.8197222222 101011140 3369 2000 3369 3369 3369 3369 1 1 1 1 1 0 0 3632 3632 5383.9 0 PROCESSED 54320.6588425926 53826 54104.4270601852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.536 22.0119 184.51119717 -5.8617583 85.703 53984.8198263889 53984.8891666667 101011150 3370 2000 3370 3370 3370 3370 1 1 1 1 1 0 0 3347.2 3347.2 5983.9 0 PROCESSED 54320.5381712963 53826 54104.9730439815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N THE CRAB OFFSETS 83.5056 22.0085 184.49889553 -5.88737418 85.6939 53984.8892708333 53984.935 101011160 2765.1 2000 2765.1 2765.1 2765.1 2765.1 1 1 1 1 1 0 0 2152 2152 3943.9 0 PROCESSED 54320.6432986111 53826 54104.4508449074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 1 AO1 CRAB OFFSET POINTINGS SPE N PERSEUS CLUSTER 49.9436 41.5175 150.56798595 -13.25929387 66.0393 53976.788275463 53980.0793865741 101012010 150905.1 150000 150905.1 150921.1 150937.1 150921.1 6 6 6 6 1 0 0 142533.4 142533.4 284336 3 PROCESSED 54331.9796412037 53826 54024.8648726852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015016 We propose the observation of Perseus cluster for 150ks. To recover the energy resolution of the XIS, we will try the periodic charge injection method. However, the charge injection will change calibrations such as gain, QE and so on dramatically. To study the change of the clibrations, Perseus cluster is one of the best targets, because it is extended over the whole XIS FOV and the iron K line from the cluster is extremely strong. For the first 50ks, the observation will be done with the normal mode without the charge injection. For the second and third 50ks, we will do the charge injections with every 54 and 108 rows, repectively. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 PERSEUS OBSERVATION FOR CALIBRATIONS ON THE PERIODIC CHARGE INJECTION METHOD XIS Y PERSEUS CLUSTER 49.9542 41.5047 150.58204074 -13.26559499 258.6515 54136.6651388889 54137.6043287037 101012020 43871.4 40000 43895.4 43879.4 0 43871.4 2 2 0 2 1 0 0 41573.2 41573.2 81137.9 1 PROCESSED 54326.7386111111 53826 54151.6542361111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y CYGNUS LOOP 314.0118 31.9912 75.70842949 -8.56360013 217.4642 54090.3953935185 54090.6848842593 101013010 9102 10000 9102 9102 0 9102 2 2 0 2 1 0 0 9212.6 9212.6 25006 1 PROCESSED 54320.6062962963 53826 54108.4571990741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y CYGNUS LOOP 314.0133 31.992 75.70987313 -8.56406979 213.2117 54090.6869791667 54091.1175231482 101013020 21004 20000 21004 21004 0 21004 1 1 0 1 1 0 0 18871.9 18871.9 37168 1 PROCESSED 54320.8528819444 53826 54132.7085763889 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y CYGNUS LOOP 314.0129 31.9925 75.71004378 -8.56348961 212.8468 54091.1180439815 54091.6036342593 101013030 19729.5 20000 19729.5 19729.5 0 19729.5 2 2 0 2 1 0 0 20100.5 20100.5 41927.9 1 PROCESSED 54326.8660069444 53826 54132.7375694444 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y E0102.2-7219 16.0421 -72.0341 301.54273778 -45.05979748 2.5391 54200.4410648148 54200.8127199074 102001010 18115 20000 18115 18115 0 18115 1 1 0 1 1 0 0 24523 24523 32103.9 0 PROCESSED 54320.8671759259 54191 54210.6037268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0153 -72.0406 301.55505042 -45.05388895 60.6693 54264.42375 54265.1467476852 102002010 27871.7 20000 27871.7 27871.7 0 27871.7 2 2 0 2 1 0 0 28315.5 28315.5 62463.9 1 PROCESSED 54320.758912037 54191 54271.4505092593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 15.9919 -72.0394 301.56512259 -45.05558467 110.1956 54324.2230208333 54325.1565277778 102003010 39482 20000 39490 39482 0 39490 1 1 0 1 1 0 0 37350.5 37350.5 80647.9 1 PROCESSED 54404.4523611111 54191 54347.4795717593 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 15.9812 -72.0282 301.56869429 -45.06698503 193.1812 54398.5171875 54399.375162037 102004010 26175.7 20000 26175.7 26175.7 0 26175.7 2 2 0 2 1 0 0 25480.7 25480.7 74093.8 0 PROCESSED 54407.5148148148 54191 54407.5260416667 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0039 -72.0219 301.55818443 -45.07278758 249.4582 54435.8094907407 54436.4099421296 102005010 24766.7 20000 24766.7 24790.7 0 24790.7 1 1 0 1 1 0 0 23722.3 23722.3 51871.9 1 PROCESSED 54441.0045833333 54191 54441.0108449074 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0383 -72.0304 301.54402708 -45.06357038 338.1 54540.2385069444 54540.8648611111 102006010 28238.9 20000 28238.9 28238.9 0 28238.9 2 2 0 2 1 0 0 38612.6 38612.6 54114 0 PROCESSED 54550.2177314815 54191 54550.2250347222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP 313.9884 32.004 75.70560343 -8.54015129 44.0016 54263.5520833333 54263.8668402778 102007010 13345.5 10000 13353.5 13345.5 0 13353.5 2 2 0 2 1 0 0 12560.7 12560.7 27191.9 1 PROCESSED 54320.8209722222 54191 54269.4117013889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP 314.0072 31.9862 75.70201861 -8.56378367 248.0186 54437.219224537 54437.5627314815 102008010 13265.5 10000 13265.5 13265.5 0 13265.5 2 2 0 2 1 0 0 13271.6 13271.6 29676 0 PROCESSED 54445.1796412037 54191 54445.1862731482 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP 313.9882 32.0035 75.70510458 -8.54033943 43.7589 54263.8673148148 54264.412025463 102009010 22896.5 20000 22896.5 22900.5 0 22916.5 3 3 0 3 1 0 0 18570.8 18570.8 47060 0 PROCESSED 54326.9052893518 54191 54269.4275462963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS_LOOP_55FE 314.0065 31.9862 75.70163572 -8.56332634 247.7519 54437.5631597222 54438.1890740741 102010010 29585 20000 29585 29585 0 29585 3 3 0 3 1 0 0 27780.4 27780.4 54075.9 0 PROCESSED 54445.2233449074 54191 54451.4647916667 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y PERSEUS CLUSTER 49.9461 41.5179 150.56936377 -13.25792808 83.376 54327.5283449074 54328.477337963 102011010 42281.7 40000 42281.7 42281.7 0 42281.7 2 2 0 2 1 0 0 36206.3 36206.3 81983.9 1 PROCESSED 54404.4795486111 54191 54347.6070833333 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y PERSEUS_CLUSTER_Normal 49.9565 41.505 150.58334697 -13.26439478 255.1861 54503.0900694444 54504.4377199074 102012010 61742.6 40000 61742.6 61742.6 0 61742.6 4 4 0 4 1 0 0 62315.7 62315.7 116399.9 0 PROCESSED 54546.3906828704 54191 54515.8301736111 2.2.7.18 2 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y GALACTIC CENTER 266.5129 -28.9278 0.05631549 -0.07626904 265.2972 54346.7924768518 54348.2224537037 102013010 51396 50000 51396 51420 0 51404 2 2 0 2 1 0 0 44477.8 44477.8 123535.8 0 PROCESSED 54404.4841319444 54191 54356.3951388889 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y RXJ1856.5-3754 284.1483 -37.9083 358.60038232 -17.21452318 271.9345 54388.7289930556 54389.587025463 102014010 41318 40000 41318 41318 0 41318 2 2 0 2 1 0 0 40654.5 40654.5 74129.9 1 PROCESSED 54403.0509837963 54191 54403.060462963 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y RXJ1856.5-3754 284.1438 -37.9098 358.59756743 -17.21176167 89.7041 54547.2693402778 54548.4723842593 102015010 50652.3 40000 50652.3 50668.3 0 50652.3 2 2 0 2 1 0 0 38365.4 38365.4 103923.8 2 PROCESSED 54566.3017592593 54191 54566.3157523148 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS Y PSR 1509-58 AT NOM. 228.4878 -59.1337 320.32453924 -1.16169081 289.2119 54333.5632060185 54334.1044444444 102016010 41213.8 40000 41221.8 41221.8 0 41213.8 1 1 0 1 1 0 0 32908.4 32908.4 46759.9 1 PROCESSED 54404.4475347222 54191 54350.4146875 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025156 PSR 1509-58 CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 2 AO2 PSR 1509-58 XIS Y PSR 1509-58 AT FIXEA 228.4815 -59.094 320.34236207 -1.12606748 287.6329 54334.1057060185 54334.7690277778 102017010 43803.8 40000 43843.8 43827.8 0 43803.8 2 2 0 2 1 0 0 37119.9 37119.9 57303.9 3 PROCESSED 54404.4777777778 54191 54350.6658449074 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025156 PSR 1509-58 CALIBRATION 1 A MAEDA YOSHITOMO NULL NULL JAP 2 AO2 PSR 1509-58 XIS Y LOCKMANHOLE 162.9257 57.2581 149.70707974 53.19495056 319.512 54223.9667592593 54226.0835532407 102018010 96071.6 80000 96079.6 96079.6 0 96071.6 2 2 0 2 1 0 0 92778 92778 182824.8 3 PROCESSED 54329.3278356482 54191 54230.4555902778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025157 The purpose of this observation is to verify the energy response of HXD-PIN/GSO. CALIBRATION 1 A KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 CALIBRATION OBSERVATION OF HXD WITH CRAB XIS Y CRAB 83.6357 21.9546 184.60961134 -5.81437304 269.3898 54179.4457407407 54180.6008912037 102019010 47633.1 40000 47633.1 47633.1 0 47633.1 3 2 0 3 1 0 0 43407.5 43407.5 99773.9 1 PROCESSED 54319.6803356482 54191 54314.6631597222 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025158 The purpose of this observation is to verify the energy response of HXD-PIN/GSO. CALIBRATION 1 A KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 CALIBRATION OBSERVATION OF HXD WITH CRAB HXD Y PKS2155-304 329.716 -30.2268 17.72837689 -52.24517694 58.2058 54212.5208796296 54212.8488310185 102020010 12036.6 15000 12036.6 12036.6 0 12036.6 1 1 0 1 1 0 0 10572 10572 28327.9 1 PROCESSED 54320.6566319444 54191 54217.2257523148 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025160 This is a coordinated observation of PKS2155-304 with Chandra and XMM-Newton for spectral calibration. The observation also aims at evaluating the amount of contaminant on the XIS OBF. CALIBRATION 1 A ISHIDA MANABU NULL NULL JAP 2 AO2 PKS2155-304 COORDINATED WITH CHANDRA AND XMM-NEWTON XIS Y E0102.2-7219 15.976 -72.0294 301.57107704 -45.06589786 179.7828 54371.2595833333 54371.6390509259 102021010 25314.6 12000 25314.6 25314.6 0 25314.6 2 2 0 2 1 0 0 20225 20225 32781.9 0 PROCESSED 54402.263125 54191 54402.2749421296 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 025155 The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 2 AO2 XIS FLIGHT CALIBRATION PLAN XIS N E0102.2-7219 16.0349 -72.0243 301.54490568 -45.06972875 306.7237 54510.7065740741 54512.1322222222 102022010 48424.5 40000 48424.5 48437.3 0 48432.5 3 2 0 3 1 0 0 46842.1 46842.1 123151.8 0 PROCESSED 54553.194837963 54191 54553.2132523148 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025161 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. CALIBRATION 1 A SWG NULL NULL NULL JAP 2 AO2 SUZAKU ADDITIONAL CALIBRATION XIS Y PSR B0540-69 85.0333 -69.3191 279.70305196 -31.5216772 241.3303 54512.1372337963 54513.444537037 102023010 52168.9 40000 52168.9 52168.9 0 52168.9 2 2 0 2 1 0 0 46459 46459 112937.8 1 PROCESSED 54522.213599537 54191 54522.2283217593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025161 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. CALIBRATION 1 A SWG NULL NULL NULL JAP 2 AO2 SUZAKU ADDITIONAL CALIBRATION XIS Y HER X-1 254.4589 35.3557 58.16585628 37.52408174 104.6168 54517.6276736111 54518.4863888889 102024010 38931 40000 38939 38931 0 38939 2 2 0 2 1 0 0 34312.1 34312.1 74190 2 PROCESSED 54525.4793171296 54191 54525.4895138889 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025161 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. CALIBRATION 1 A SWG NULL NULL NULL JAP 2 AO2 SUZAKU ADDITIONAL CALIBRATION XIS Y E0102.2-7219 16.0298 -72.0236 301.54705976 -45.07053683 295.9817 54501.0571990741 54501.5245833333 102026010 0 15000 0 0 0 0 0 0 0 0 1 0 0 19059.4 19059.4 40380 0 PROCESSED 54515.4175115741 54191 54515.8508912037 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 025162 Recovery operation of XIS CPU HALT CALIBRATION 1 A SWG NULL NULL NULL JAP 2 AO2 XIS RECOVERY AND VERIFICATION XIS Y E0102.2-7219 16.0427 -72.0346 301.54252595 -45.05928576 1.5429 54564.6063888889 54565.2190277778 103001010 22361.5 20000 22377.5 22361.5 0 22377.5 2 2 0 2 1 0 0 22318.5 22318.5 52926 1 PROCESSED 54580.9326388889 54557 54580.9409722222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0204 -72.038 301.5525741 -45.05637352 46.6005 54622.1603356482 54622.8557175926 103001020 21313 20000 21329 21313 0 21329 2 2 0 2 1 0 0 19486.9 19486.9 60069.9 0 PROCESSED 54636.3151851852 54557 54636.3245833333 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 15.987 -72.0401 301.56732456 -45.05499026 122.9265 54690.9315740741 54691.5905555556 103001030 21301.8 20000 21309.8 21309.8 0 21301.8 2 2 0 2 1 0 0 17083.1 17083.1 56929.9 0 PROCESSED 54710.2652662037 54557 54710.2804166667 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 15.9798 -72.0267 301.56915878 -45.06851113 190.5435 54761.1055092593 54761.6265277778 103001040 25405.2 20000 25405.2 25405.2 0 25405.2 2 2 0 2 1 0 0 22263.6 22263.6 45005.9 1 PROCESSED 54778.0033101852 54557 54780.7231134259 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0024 -72.0211 301.55876018 -45.07361767 248.5277 54813.5648263889 54814.3092476852 103001050 29618 20000 29633.6 29634 0 29618 2 2 0 2 1 0 0 27676.9 27676.9 64293.9 0 PROCESSED 54839.9805439815 54557 54839.9906481482 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y E0102.2-7219 16.0385 -72.0294 301.54384101 -45.06456362 331.5978 54899.1304861111 54899.6454282407 103001060 23843.9 20000 23859.9 23843.9 0 23867.9 1 1 0 1 1 0 0 21711.2 21711.2 44463.9 0 PROCESSED 54962.3705902778 54557 54916.3664814815 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP 313.9898 32.0072 75.70886169 -8.53902556 62.1393 54628.6164814815 54629.4703125 103002010 33166.9 10000 33166.9 33166.9 0 33166.9 3 3 0 3 1 0 0 29636.1 29636.1 73763.9 0 PROCESSED 54642.2957523148 54557 54655.4782523148 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP 313.9023 31.8775 75.55993186 -8.5644348 221.2652 54811.2228587963 54811.8571064815 103002020 21920.2 10000 21920.2 21920.2 0 21920.2 2 2 0 2 1 0 0 19489.9 19489.9 54770 0 PROCESSED 54826.3421412037 54557 54826.3522569444 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP (WIN FE) 313.9898 32.0072 75.70886169 -8.53902556 62.1393 54628.6164814815 54629.4703125 103003010 33166.9 20000 33166.9 33166.9 0 33166.9 3 3 0 3 1 0 0 29636.1 29636.1 73763.9 0 PROCESSED 54642.3231597222 54557 54655.483287037 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y CYGNUS LOOP (WIN FE) 313.902 31.8775 75.55976783 -8.56423835 221.2647 54811.8571180556 54812.4321064815 103003020 26673.2 20000 26673.2 26673.2 0 26673.2 2 2 0 2 1 0 0 22795.9 22795.9 49663.9 1 PROCESSED 54826.1622685185 54557 54828.3679166667 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y PERSEUS 49.9468 41.518 150.56975635 -13.25755566 86.8161 54691.602974537 54692.6204166667 103004010 40568.5 40000 40584.5 40568.5 0 40584.5 2 2 0 2 1 0 0 31597.9 31597.9 87897.9 1 PROCESSED 54710.2585300926 54557 54710.2764467593 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y PERSEUS 49.9546 41.5055 150.58184418 -13.26476244 256.0759 54873.7298611111 54874.8141087963 103004020 50006.6 40000 50014.6 50014.6 0 50006.6 2 2 0 2 1 0 0 44840.4 44840.4 93669.9 0 PROCESSED 54962.4890625 54557 54893.3133680556 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y PERSEUS (1/4WIN) 49.9475 41.518 150.57020557 -13.25726666 86.8158 54692.6204282407 54693.1071643518 103005010 21478 20000 21478 21501 0 21486 3 3 0 3 1 0 0 16992.2 16992.2 42049.9 0 PROCESSED 54710.3053125 54557 54780.5282291667 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y PERSEUS (1/4WIN) 49.9551 41.5057 150.58205177 -13.2643891 255.655 54874.8146759259 54875.4398032407 103005020 28816.2 20000 28816.2 28840.2 0 28824.2 3 3 0 3 1 0 0 26779.3 26779.3 53986 0 PROCESSED 54962.2071875 54557 54893.0113888889 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y RXJ1856.5-3754 284.1503 -37.908 358.6012758 -17.21588394 280.5087 54759.7973148148 54761.0974421296 103006010 43040.2 40000 43048.2 43048.2 0 43040.2 2 2 0 2 1 0 0 37677.4 37677.4 112322 0 PROCESSED 54778.0592824074 54557 54780.5234837963 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 035001 Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 AO-3 XIS FLIGHT CALIBRATION PLAN XIS Y CRAB 83.6308 22.0168 184.5543577 -5.78491639 87.005 54705.3561458333 54706.218912037 103007010 39822 40000 39822 39822 0 39822 2 2 0 2 1 0 0 32782.3 32782.3 74527.8 1 PROCESSED 54720.3652662037 54557 54780.5351851852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 035002 We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 3 AO3 HXD CALIBRATIONS ON AO-3 XIS Y CRAB 83.6295 22.0815 184.49878495 -5.75129488 87.125 54710.3844560185 54711.412662037 103008010 45090 40000 45090 45090 0 45090 2 2 0 2 1 0 0 33916.7 33916.7 88827.8 0 PROCESSED 54777.4816666667 54557 54780.4386458333 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 035002 We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 3 AO3 HXD CALIBRATIONS ON AO-3 HXD Y LOCKMANHOLE 162.9369 57.2546 149.70462232 53.2017902 281.5296 54604.4635300926 54606.0529398148 103009010 83419.7 80000 83419.7 83419.7 0 83419.7 2 2 0 2 1 0 0 87485.2 87485.2 137300 3 PROCESSED 54616.4074768518 54557 54616.4206597222 2.2.7.18 2 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 035002 We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 3 AO3 HXD CALIBRATIONS ON AO-3 XIS Y PKS2155-304 329.7153 -30.2277 17.72680762 -52.24467434 58.2307 54598.5708912037 54599.1120138889 103011010 23119 20000 23119 23119 0 23119 2 2 0 2 1 0 0 17813.1 17813.1 46745.9 0 PROCESSED 54608.9835069444 54557 54608.9900115741 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 035003 XMM/Chandra/Suzaku cross calibration by an coordinated observation of PKS215-304. CALIBRATION 1 A ISHIDA MANABU NULL NULL JAP 3 AO3 COORDINATED OBSERVATION FOR CROSS-CALIBRATION WITH PKS2155-304 XIS Y CRAB 83.6356 21.9544 184.60973125 -5.81455843 269.3968 54923.0747337963 54924.0418287037 104001010 42105.2 40000 42808.5 42105.2 0 42808.5 2 2 0 2 1 0 0 33587.7 33587.7 83539.8 0 PROCESSED 54945.440162037 54922 54949.4458680556 2.3.12.25 3 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045003 N/A CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 4 AO4 CRAB CAL 2009 HXD Y CRAB 83.6363 22.0087 184.56397797 -5.78494551 270.0021 55250.0427199074 55251.1904976852 104001070 45830.9 40000 45830.9 45830.9 0 45830.9 3 2 0 2 1 0 0 16318 16318 99157.9 1 PROCESSED 55267.2501157407 54922 55267.2846643518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045003 N/A CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 4 AO4 CRAB CAL 2009 XIS Y LOCKMAN HOLE 162.9377 57.2549 149.70376614 53.20190951 281.53 54994.3039351852 54996.0634375 104002010 92848.4 80000 92848.4 92848.4 0 92848.4 2 2 0 2 1 0 0 79880 79880 152000 0 PROCESSED 55005.1218634259 54922 55005.1389814815 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045004 HXD / XIS NXB/ CXB cal CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 4 AO4 LOCKMAN HOLE 2009 XIS Y LOCKMAN HOLE 162.9419 57.2782 149.67240249 53.18794557 110.367 55161.4316319444 55161.7502199074 104002020 2359.1 12000 2383.1 2359.1 0 2375.1 5 2 0 3 1 0 0 10017.4 10017.4 27515.9 0 PROCESSED 55182.5883101852 54922 55182.6514467593 2.4.12.27 3 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045004 HXD / XIS NXB/ CXB cal CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 4 AO4 LOCKMAN HOLE 2009 XIS Y PKS2155-304 329.7145 -30.2263 17.72895666 -52.2438339 83.4423 54978.6583217593 54980.486400463 104004010 62440.1 60000 62440.1 62440.1 0 62440.1 2 2 0 2 1 0 0 53071.7 53071.7 157931.8 2 PROCESSED 54994.3203819444 54922 54994.3621296296 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045006 This is a cross calibration observation with PKD2155-304 among Suzaku, XMM-Newton and Chandra. CALIBRATION 1 A ISHIDA MANABU NULL NULL JAP 4 AO4 CROSS CALIBRATION OF SUZAKU/XMM/CHANDRA WITH PKS2155-304 XIS Y E0102-72 16.0343 -72.0367 301.54639234 -45.05737191 19.8885 54944.6369560185 54945.6225 104005010 45028.7 20000 45654.5 45028.7 0 45654.5 3 2 0 3 1 0 0 49726.9 49726.9 85135.8 1 PROCESSED 54966.3423958333 54922 54966.3543518518 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 16.0181 -72.0439 301.55415549 -45.05053701 69.1611 55008.1544097222 55008.571087963 104006010 22061.5 20000 22061.5 22061.5 0 22061.5 2 2 0 2 1 0 0 16326.3 16326.3 35991.9 1 PROCESSED 55022.2321180556 54922 55022.2400694445 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 15.9824 -72.0274 301.56809353 -45.06775773 194.7588 55130.7598148148 55131.4169444444 104007010 20375.6 20000 20383.6 20383.6 0 20375.6 2 2 0 2 1 0 0 18037.9 18037.9 56761.8 1 PROCESSED 55141.2386574074 54922 55141.2502777778 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 15.9813 -72.0285 301.56867985 -45.06668362 180.8386 55115.6048032407 55116.6237615741 104008010 31449.9 20000 31449.9 49641.1 0 49935.3 2 2 0 2 1 0 0 43716.7 43716.7 88013.9 1 PROCESSED 55134.2097106482 54922 55134.4398842593 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 16.0091 -72.0251 301.55623091 -45.06948422 251.7193 55190.9159837963 55191.5411921296 104009010 21985.2 20000 21993.2 21985.2 0 21993.2 2 2 0 2 1 0 0 21639.6 21639.6 54016 0 PROCESSED 55225.1324884259 54922 55225.1469328704 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 16.0186 -72.0293 301.55250278 -45.06509107 296.1745 55231.7435069444 55232.4343055556 104010010 20500.6 20000 20508.6 20500.6 0 20508.6 2 2 0 2 1 0 0 24497.1 24497.1 59675.9 2 PROCESSED 55249.7128587963 54922 55249.7236111111 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 1/4 WIN 15.9806 -72.0277 301.56890722 -45.06749655 189.3214 55124.8016203704 55125.3654282407 104011010 19091.3 20000 19091.3 20038.1 0 20038.1 3 3 0 3 1 0 0 16209 16209 48711.9 1 PROCESSED 55134.1666203704 54922 55134.1777777778 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 1/4 WIN 16.0261 -72.0284 301.54914583 -45.06582801 296.9556 55232.435150463 55233.0002777778 104012010 23553.7 20000 23553.7 23553.7 0 23560 2 2 0 2 1 0 0 25339.4 25339.4 48815.9 0 PROCESSED 55266.2249421296 54922 55266.2358449074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y E0102-72 PSUM 15.9904 -72.0242 301.56429483 -45.07078046 218.0047 55166.9023032407 55167.9336111111 104014010 62658.9 20000 63019.2 62658.9 0 63011.2 1 2 0 1 1 0 0 54915.1 54915.1 89091.8 1 PROCESSED 55181.2059259259 54922 55181.4406365741 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS N CYGNUS LOOP NE2 313.9438 31.9667 75.6521583 -8.53477618 43.0005 54998.5732407407 54998.7883449074 104015010 10889.7 10000 10889.7 10889.7 0 10889.7 2 2 0 2 1 0 0 9923 9923 18577.9 0 PROCESSED 55008.0992592593 54922 55008.1053356482 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y CYGNUS LOOP NE2 313.9634 31.9567 75.65508045 -8.55396375 223.0007 55175.7922106482 55176.0640509259 104016010 12573.5 10000 12573.5 12573.5 0 12573.5 1 1 0 1 1 0 0 10077.6 10077.6 23479.9 0 PROCESSED 55189.1092939815 54922 55189.115625 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y CYGNUS LOOP P8 313.9958 31.4752 75.29735897 -8.88195371 62.5173 54998.7930787037 54999.0668865741 104017010 9708.7 10000 9708.7 9708.7 0 9708.7 1 1 0 1 1 0 0 6711.9 6711.9 23652 1 PROCESSED 55108.9983101852 54922 55008.151087963 2.4.12.27 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y PERSEUS 49.9444 41.5171 150.56872595 -13.25929731 66.998 55069.1669907407 55070.1453009259 104018010 41279.8 40000 41279.8 41279.8 0 41295.8 4 3 0 3 1 0 0 37348.8 37348.8 84499.8 1 PROCESSED 55088.1088541667 54922 55088.1261458333 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y PERSEUS 49.9512 41.4934 150.58651783 -13.27626038 277.3248 55228.3356944444 55229.2502199074 104019010 38615.1 40000 38615.1 38615.1 0 38615.1 2 2 0 2 1 0 0 35781.4 35781.4 78997.9 0 PROCESSED 55249.7809259259 54922 55249.7985069444 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y PERSEUS 1/4 WIN 49.9444 41.516 150.56934906 -13.260215 66.9976 55070.1453125 55071.500162037 104020010 55044.9 20000 55067.7 55052.9 0 55044.9 3 3 0 3 1 0 0 51280.2 51280.2 117049.8 2 PROCESSED 55106.3415277778 54922 55109.4175115741 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y PERSEUS 1/4 WIN 49.9506 41.4949 150.58528271 -13.27525693 276.9447 55229.250787037 55229.7078587963 104021010 21641.5 20000 21649.1 21646.9 0 21641.5 3 3 0 3 1 0 0 21574.3 21574.3 39482 0 PROCESSED 55249.7033912037 54922 55249.7129513889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y RXJ1856.5 284.1483 -37.909 358.59969969 -17.21477781 277.829 55127.9550115741 55128.8363425926 104022010 43484.5 40000 43484.5 43492.5 0 43492.5 2 2 0 2 1 0 0 39424.6 39424.6 76101.8 0 PROCESSED 55141.2708912037 54922 55141.2812384259 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y RXJ1856.5 284.0709 -37.7784 358.70367738 -17.11026819 79.4744 55269.4572569444 55270.6856944444 104022020 40415.2 40000 40426.9 40415.2 0 40415.2 2 2 0 2 1 0 0 34577.2 34577.2 106107.9 0 PROCESSED 55285.0717939815 54922 55285.0858564815 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y RXJ1856.5 284.1421 -37.9072 358.59959193 -17.20956639 77.5864 55281.1527083333 55282.3710069444 104022030 42450.9 40000 42450.9 42450.9 0 42450.9 2 2 0 2 1 0 0 11139.6 11139.6 105252 2 PROCESSED 55301.2699537037 54922 55301.2941203704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 045007 We propose some observations for the calibtaions of XIS. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 4 AO4 XIS FLIGHT CALIBRATION IN AO4 XIS Y G21.5-0.9 278.3939 -10.5728 21.49883061 -0.89086145 264.65 55114.5957986111 55115.5953009259 104023010 40156.1 40000 40156.1 40156.1 0 40156.1 2 2 0 2 1 0 0 30452.1 30452.1 86354 0 PROCESSED 55131.2417361111 54922 55131.2519675926 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 045008 We propose G21.5-0.9 observation for the cross-calibtaions of XIS. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 4 AO4 CROSS CALIBRATION OF G21.5-0.9 XIS Y PKS2155-304 329.7122 -30.2251 17.73054892 -52.24172704 58.9372 55313.9868171296 55315.8536458333 105001010 63457.2 60000 63465.2 63471 0 63457.2 2 2 0 2 1 0 0 54701.5 54701.5 161277.8 2 PROCESSED 55327.3554976852 55287 55327.3816087963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055001 This observation of PKS2155-304 is coordinated with XMM-Newton and Chandra. CALIBRATION 1 A ISHIDA MANABU NULL NULL JAP 5 AO5 COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON XIS Y CRAB 83.6381 22.0079 184.56555504 -5.78396412 269.4791 55291.5258680556 55292.5001273148 105002010 481.5 40000 481.5 481.6 0 481.6 2 2 0 2 1 0 0 33897.4 33897.4 84133.8 1 PROCESSED 55350.3157291667 55287 55350.3368981482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055002 We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 5 AO5 AO-5 CRAB CALIBRATION XIS Y LOCKMAN_HOLE 162.9382 57.2507 149.70866001 53.20492954 279.8869 55358.311875 55360.0828935185 105003010 77997.6 80000 78013.6 77997.6 0 78258.3 2 2 0 1 1 0 0 73083.2 73083.2 152981.8 1 PROCESSED 55370.3136921296 55287 55370.3379861111 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055003 2010 Annual observation of Lockman hole, with XIS in the Psum mode. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 5 AO5 LOCKMAN HOLE XIS N E0102-72 16.0161 -72.0335 301.55400478 -45.06095473 357.7405 55291.0014699074 55291.5147453704 105004010 21592.8 20000 21592.8 21592.8 0 21592.8 1 1 0 1 1 0 0 17139 17139 44311.9 0 PROCESSED 55306.2070486111 55287 55306.2144328704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72 16.0035 -72.0383 301.55996349 -45.05643533 65.2308 55366.1296412037 55366.7869791667 105004020 19230.2 20000 19238.2 19238.2 0 19230.2 2 2 0 2 1 0 0 16589.5 16589.5 56783.9 2 PROCESSED 55413.2677199074 55287 55413.4019097222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72 16.00833 -72.03131 301.55717515 -45.06330557 -99 NULL NULL 105004030 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 55287 NULL NULL NULL NULL 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS N E0102-72 16.0129 -72.0282 301.55487873 -45.06631044 194.5389 55495.8125694444 55496.3217939815 105004040 20018.9 20000 20619.9 20018.9 0 20643.9 2 2 0 2 1 0 0 19219.3 19219.3 43988 0 PROCESSED 55505.2191666667 55287 55505.2302893518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72 16.0026 -72.0263 301.55918173 -45.06842583 227.0923 55539.0256481482 55539.487662037 105004050 20046.8 20000 20070.8 20070.8 0 20046.8 1 2 0 2 0 0 0 0 0 39913.9 0 PROCESSED 55551.4886921296 55287 55552.4359953704 2.5.16.29 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72 16.0173 -72.0347 301.55359992 -45.05973194 299.5457 55600.0152430556 55600.4516319444 105004060 17242.6 20000 17258.6 17242.6 0 17258.6 1 1 0 1 1 0 0 13743.2 13743.2 37695.9 0 PROCESSED 55614.7171643518 55287 55617.4086805556 2.5.16.29 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72_1_4_WIN 16.0018 -72.0347 301.56035188 -45.06006295 65.8655 55366.7877314815 55367.3098842593 105005010 20345.6 20000 20353.6 20345.6 0 20361.6 2 2 0 2 1 0 0 17482.3 17482.3 45080 2 PROCESSED 55400.2717476852 55287 55400.4271412037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72_1_4_WIN 16.0156 -72.0284 301.55372169 -45.06605315 226.5285 55539.4883680556 55540.2502546296 105005020 22538.8 20000 22546.8 22538.8 0 22554.8 3 3 0 3 1 0 0 5796.9 5796.9 65821.9 2 PROCESSED 55550.9296875 55287 55550.9436689815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y E0102-72_PSUM 15.883 -72.0319 301.61184542 -45.06533979 66.3881 55367.3105439815 55368.5202314815 105006010 356.5 40000 356.5 356.5 0 356.5 1 1 0 1 1 0 0 303 303 36191.9 0 PROCESSED 55400.3158564815 55287 55400.4299537037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS N E0102-72_PSUM 16.0136 -72.0296 301.55471109 -45.06489883 226.8844 55537.8034375 55539.0252199074 105006020 40871.5 40000 40936.3 40871.5 0 41120.5 4 3 0 1 1 0 0 157.4 157.4 105549.9 0 PROCESSED 55777.5091898148 55287 55778.433275463 2.7.16.30 4 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS N E0102-72_PSUM 16.0081 -72.0302 301.5571666 -45.06441782 138.5223 55437.769525463 55438.8884606482 105006030 37067.5 40000 37083.1 37067.5 0 37636.5 2 2 0 1 1 0 0 33043.8 33043.8 96641.9 1 PROCESSED 55449.0119328704 55287 55449.0261574074 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS N CYGNUS LOOP P8 313.9885 31.4813 75.29810685 -8.87326903 62.5188 55358.0139583333 55358.3015393518 105007010 12093.9 10000 12881.6 12093.9 0 12889.6 2 3 0 2 1 0 0 9985.5 9985.5 24839.9 0 PROCESSED 55370.6569675926 55287 55376.4220717593 2.5.16.28 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y CYGNUS LOOP P8 CI 6 314.021 31.4644 75.3027873 -8.90540252 222.2994 55552.9622569444 55553.0467824074 105007020 2740 10000 2755.6 2740 0 2755.6 1 1 0 1 1 0 0 2487.4 2487.4 7295.9 0 PROCESSED 55593.253125 55287 55593.2584722222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y CYGNUS LOOP P8 CI 2 314.0088 31.4691 75.29974588 -8.89438689 222.2165 55553.0469791667 55553.1446990741 105007030 4963.1 10000 4987 4979 0 4963.1 1 2 0 1 1 0 0 3566.5 3566.5 8431.9 0 PROCESSED 55593.2589930556 55287 55593.2653587963 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y RXJ1856.5-3754 284.1491 -37.9166 358.59252855 -17.21813017 271.239 55496.329537037 55497.4509722222 105008010 40091.7 40000 40091.7 40099.7 0 40107.7 2 2 0 2 1 0 0 32908.1 32908.1 96875.8 0 PROCESSED 55509.0452546296 55287 55509.0637731482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y PERSEUS 49.9406 41.5199 150.56470121 -13.25852998 66.581 55417.3825925926 55418.010625 105009010 33624.2 40000 33624.2 33624.2 0 33624.2 2 2 0 2 1 0 0 37659.6 37659.6 54254 0 PROCESSED 55428.0437037037 55287 55428.0593171296 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y PERSEUS 49.9557 41.5028 150.58408011 -13.26656036 259.7325 55595.0249421296 55595.9578472222 105009020 40461.1 40000 40469.1 40461.1 0 40477.1 3 3 0 3 1 0 0 29594.3 29594.3 80593.9 1 PROCESSED 55610.2551967593 55287 55610.273587963 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y PERSEUS_1_4_WIN 49.9403 41.521 150.56388564 -13.25773608 66.5805 55418.0106365741 55418.6467476852 105010010 27372.7 20000 27372.7 27380.4 0 27386.4 2 2 0 2 1 0 0 33712.7 33712.7 54955.9 1 PROCESSED 55428.0581481482 55287 55428.0721759259 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y PERSEUS_1_4_WIN 49.9552 41.5037 150.58324921 -13.26601613 259.969 55594.4623958333 55595.0245138889 105010020 21092.6 20000 21096.3 21096.3 0 21092.6 2 2 0 2 1 0 0 16573 16573 48559.9 0 PROCESSED 55610.2520486111 55287 55610.2645717593 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y N132D 81.279 -69.6505 280.31295018 -32.77613267 32.9954 55404.1821296296 55405.1411226852 105011010 35849.5 30000 35849.5 35849.5 0 35849.5 2 2 0 2 1 0 0 32540.9 32540.9 82839.8 1 PROCESSED 55414.0839236111 55287 55414.1006828704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055005 We propose a observation of N132D for the calibration of the XIS in the AO5 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y CRAB_80OFF_0DEG 83.6952 20.686 185.71797799 -6.44521522 87.4149 55452.6214467593 55453.046712963 105012010 19241.5 20000 19241.5 19241.5 0 19241.5 2 2 0 2 1 0 0 17364.4 17364.4 36736 0 PROCESSED 55463.1437962963 55287 55463.4094212963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_80OFF_22.5DEG 83.1525 20.7619 185.38009186 -6.83349718 86.9209 55453.0474189815 55453.4918518518 105013010 18989.1 20000 18989.1 18989.1 0 18989.1 1 1 0 1 1 0 0 13723 13723 38376 0 PROCESSED 55463.1640509259 55287 55463.4117013889 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_80OFF_45DEG 82.6663 21.0307 184.90557346 -7.07161845 87.0482 55453.4925578704 55453.9550115741 105014010 20599.2 20000 20607.2 20607.2 0 20599.2 2 2 0 2 1 0 0 19812.1 19812.1 39937.9 2 PROCESSED 55463.1749189815 55287 55463.4144675926 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_50OFF_45DEG 83.0202 21.413 184.76043538 -6.58765564 87.6753 55431.8338194445 55432.0682291667 105015010 10549.2 10000 11277.2 10549.2 0 11277.6 2 2 0 2 1 0 0 10191.7 10191.7 20245.9 1 PROCESSED 55446.2122800926 55287 55446.446875 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_50OFF_135DEG 82.9576 22.5813 183.73915584 -6.0064164 86.6565 55432.0694907407 55432.3105555556 105016010 6489.4 10000 6489.4 6497.4 0 6497.4 2 2 0 2 1 0 0 3638.1 3638.1 20822 0 PROCESSED 55446.2337268518 55287 55446.4488425926 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_50OFF_225DEG 84.2344 22.6444 184.32067652 -4.97776831 87.1427 55432.3115856482 55432.5827777778 105017010 12345.6 10000 12353.6 12345.6 0 12361.6 1 1 0 1 1 0 0 12151 12151 23423.9 0 PROCESSED 55447.2142824074 55287 55447.4086921296 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_50OFF_315DEG 84.2968 21.4693 185.35120349 -5.55324373 87.1743 55432.5838078704 55432.8980555556 105018010 14432.3 10000 14432.3 14456.3 0 14440.3 1 1 0 1 1 0 0 12415.6 12415.6 27143.9 1 PROCESSED 55447.2415509259 55287 55447.4099884259 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_0DEG 83.6859 20.9369 185.49975653 -6.31874712 87.2696 55446.25 55446.4605439815 105019010 9657.5 10000 9657.5 9657.5 0 9657.5 1 1 0 1 1 0 0 7899.5 7899.5 18183.9 0 PROCESSED 55460.9539583333 55287 55461.3910763889 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_45DEG 82.8482 21.2156 184.84096902 -6.82899548 86.9607 55446.4614351852 55446.6875694444 105020010 9450.4 10000 9458.4 9450.4 0 9458.4 2 2 0 2 1 0 0 7906.9 7906.9 19533.9 0 PROCESSED 55460.9663888889 55287 55461.3925231482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_90DEG 82.4629 21.9742 184.00329077 -6.72000946 87.3211 55446.6885532407 55446.9076967593 105021010 10912 10000 10921.9 10920 0 10912 2 2 0 2 1 0 0 10033.9 10033.9 18930 0 PROCESSED 55460.9870486111 55287 55461.3931944444 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_135DEG 82.7613 22.7517 183.49649927 -6.06655162 87.038 55446.9086805556 55447.1314236111 105022010 9248.2 10000 9248.2 9248.2 0 9248.2 2 2 0 2 1 0 0 7939.3 7939.3 19237.9 0 PROCESSED 55466.1589814815 55287 55466.4006365741 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_180DEG 83.5739 23.1022 183.60559643 -5.24730073 87.2466 55447.1322685185 55447.3557291667 105023010 11470.6 10000 11470.6 11478.6 0 11478.6 1 1 0 1 1 0 0 10091.3 10091.3 19295.9 0 PROCESSED 55461.0497453704 55287 55461.3950810185 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_225DEG 84.3921 22.8458 184.22714627 -4.7474889 85.6608 55447.3571296296 55447.5793402778 105024010 9404.2 10000 9412.2 9404.2 0 9420.2 1 1 0 1 1 0 0 7822.5 7822.5 19191.9 0 PROCESSED 55461.0795949074 55287 55461.3963541667 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_270DEG 84.7966 22.0949 185.06495422 -4.82832438 86.3168 55447.5802777778 55447.7918287037 105025010 8891 10000 8891 8891 0 8891 1 1 0 1 1 0 0 8535 8535 18273.9 0 PROCESSED 55461.1209143518 55287 55461.3998032407 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y CRAB_65OFF_315DEG 84.4913 21.2878 185.60226135 -5.4958009 87.6059 55447.7930902778 55448.0217824074 105026010 11382 10000 11390 11390 0 11382 2 2 0 2 1 0 0 9884.1 9884.1 19750 0 PROCESSED 55461.1300578704 55287 55461.4004050926 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055006 For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. CALIBRATION 1 A TAKEI YOH NULL NULL JAP 5 AO5 CALIBRATION OF STRAY LIGHT SPE Y PERSEUS_CI_6 49.9577 41.5001 150.58689381 -13.26798644 252.2456 55614.2081365741 55615.187662037 105027010 45272.2 40000 45905.5 45272.2 0 45905.5 2 2 0 2 1 0 0 41885.9 41885.9 84609.8 0 PROCESSED 55624.2063194444 55287 55624.2249421296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y PERSEUS_1_4_WIN_CI_6 49.9565 41.5014 150.58538691 -13.26739774 252.427 55613.7422106482 55614.2078009259 105028010 20636.3 20000 20636.3 20636.3 0 20636.3 1 1 0 1 1 0 0 17845 17845 40215.9 0 PROCESSED 55624.1538657407 55287 55624.1639814815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055004 We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 5 AO5 CALIBRATION OF X-RAY IMAGING SPECTROMETER XIS Y CRAB 83.6359 22.0094 184.56318415 -5.78488405 269.6199 55641.8131828704 55643.1459490741 105029010 614.6 40000 614.6 614.6 0 614.6 2 2 0 2 1 0 0 36940.8 36940.8 115139.9 0 PROCESSED 55652.144375 55287 55652.1669097222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 055002 We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV. CALIBRATION 1 A NAKAZAWA KAZUHIRO NULL NULL JAP 5 AO5 AO-5 CRAB CALIBRATION XIS Y LOCKMAN HOLE 162.9265 57.2528 149.71315343 53.19882847 305.9894 55685.7406712963 55686.7675925926 106001010 42278 40000 42278 43590.5 0 44442.7 2 2 0 1 1 0 0 57821.4 57821.4 88709.8 0 PROCESSED 55768.7908217593 55652 55768.8116898148 2.6.16.30 3 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS N E0102-72 CI 6 15.9973 -72.0342 301.56226334 -45.06065755 3.8307 55662.8284490741 55663.3522569444 106002010 20386.2 30000 20386.2 20386.2 0 20386.2 2 2 0 2 1 0 0 17842 17842 45247.9 0 PROCESSED 55687.536400463 55652 55690.5690625 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y E0102-72 16.0024 -72.0368 301.56029587 -45.05795518 69.5441 55741.0977314815 55741.5828009259 106002020 28782 30000 28790 28798 0 28782 1 1 0 1 1 0 0 24611.5 24611.5 41903.9 1 PROCESSED 55775.2410069444 55652 55775.250150463 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y E0102-72 16.001 -72.0295 301.56019202 -45.06526758 183.1599 55848.6463310185 55849.0905092593 106002030 32817.5 30000 32825.5 32817.5 0 32825.5 2 2 0 2 1 0 0 29913.7 29913.7 38361.9 0 PROCESSED 55872.9987615741 55652 55873.0106597222 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y E0102-72 16.0145 -72.0334 301.55469199 -45.06108873 340.2388 56003.3836574074 56004.1619444445 106002040 32378 30000 32394 32378 0 32394 2 2 0 2 1 0 0 30718 30718 67244 0 PROCESSED 56019.2667592593 55652 56019.2768518518 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y E0102-72 CI 2 15.9944 -72.0366 301.5637608 -45.05832492 4.3228 55663.352962963 55663.8890740741 106002050 20814.3 20000 20825.2 20822.2 0 20814.3 2 3 0 2 1 0 0 19623.9 19623.9 46318 0 PROCESSED 55687.5378356482 55652 55690.5705439815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y E0102-72_1_4_WIN 16.0104 -72.0348 301.55661541 -45.05977973 4.7976 55663.8897337963 55664.4098726852 106003010 16829.5 30000 16829.5 18277.5 0 18277.5 2 2 0 2 1 0 0 16956.4 16956.4 44931.9 0 PROCESSED 55687.5426041667 55652 55690.5713310185 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y E0102-72_1_4_WIN 16.0013 -72.0289 301.56000261 -45.06585975 183.5797 55849.0910763889 55849.5446643518 106003020 31657.1 30000 31657.1 31753.1 0 31769.1 4 3 0 3 1 0 0 24464.3 24464.3 39183.9 0 PROCESSED 55873.0320949074 55652 55873.0426736111 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y CYGNUS_LOOP_P8 313.9841 31.4885 75.30130763 -8.86579122 62.5162 55721.2910763889 55721.5835532407 106004010 11551.1 10000 11559.1 11567.1 0 11551.1 1 1 0 1 1 0 0 10646.2 10646.2 25255.9 0 PROCESSED 55748.5317476852 55652 55757.6943287037 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y CYGNUS_LOOP_P8 314.0101 31.4557 75.29000417 -8.90377623 240.0029 55915.0575231482 55915.3196527778 106004020 11990 10000 11990 11990 0 11990 2 2 0 2 1 0 0 12321.2 12321.2 22643.9 0 PROCESSED 55932.0868402778 55652 55932.095162037 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PERSEUS 49.9433 41.526 150.56297877 -13.25232631 83.8173 55769.5188888889 55770.5467939815 106005010 40838.2 40000 40854.2 40838.2 0 40963.1 2 3 0 2 1 0 0 36688.5 36688.5 88801.9 1 PROCESSED 55792.3044212963 55652 55792.3246990741 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS N PERSEUS 49.9531 41.5016 150.58309121 -13.26863527 261.9986 55964.8470138889 55965.9169328704 106005020 46813.8 40000 46813.8 46813.8 0 46821.8 3 2 0 2 1 0 0 45202.5 45202.5 92427.8 0 PROCESSED 56019.2486805556 55652 56019.2664583333 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PERSEUS_CI_2 49.9439 41.5251 150.56387356 -13.25282951 84.2575 55768.5049768518 55769.518275463 106006010 40145.3 40000 40153.3 40161.3 0 40145.3 3 2 0 2 1 0 0 35470.3 35470.3 87505.9 0 PROCESSED 55792.212650463 55652 55792.2315740741 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PERSEUS_1_4_WIN 49.9438 41.5162 150.5688507 -13.26029585 67.7327 55796.234849537 55796.7167824074 106007010 20971.3 20000 20971.3 21003.2 0 20985.5 2 3 0 2 1 0 0 18760.7 18760.7 41633.9 2 PROCESSED 55809.1854398148 55652 55809.1967013889 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PERSEUS_1_4_WIN 49.954 41.5015 150.58372556 -13.26834695 262.0009 55965.9169444444 55966.4167824074 106007020 20856.9 20000 20880.9 20872.9 0 20856.9 3 3 0 3 1 0 0 21425.5 21425.5 43173.9 1 PROCESSED 55991.4404976852 55652 55991.4500810185 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PERSEUS_1_4_WIN_CI_2 49.9427 41.5184 150.56689856 -13.25891455 67.7307 55795.7574305556 55796.234837963 106008010 23202.3 20000 23210.3 23202.3 0 23218.3 3 2 0 2 1 0 0 22067.8 22067.8 41244 0 PROCESSED 55806.3383333333 55652 55806.3485069445 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PERSEUS_1_4_WIN_CI_2 49.95042 41.51169 150.57565427 -13.261325 -99 NULL NULL 106008020 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 55652 NULL NULL NULL NULL 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS N PERSEUS_1_4_WIN_CI_2 49.95042 41.51169 150.57565427 -13.261325 -99 NULL NULL 106008030 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 55652 NULL NULL NULL NULL 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS N RXJ1856.5-3754 284.1491 -37.9147 358.59438145 -17.21743909 269.0594 55856.467037037 55857.327962963 106009010 39312.3 40000 39312.3 39320.3 0 39312.3 2 2 0 2 1 0 0 35512.7 35512.7 74370.1 1 PROCESSED 55873.9707175926 55652 55873.9976041667 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y N132D 81.27 -69.6453 280.30751952 -32.78013136 312.914 55676.4828935185 55677.0820138889 106010010 26045.3 25000 26045.3 26045.3 0 26045.3 2 2 0 2 1 0 0 23421 23421 51753.9 0 PROCESSED 55697.1299768518 55652 55697.1447685185 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y N132D 81.2448 -69.6458 280.30994764 -32.78867022 111.8253 55841.4446759259 55841.8703935185 106010020 23903 25000 23903 23903 0 23903 2 2 0 2 1 0 0 22252.9 22252.9 36763.9 0 PROCESSED 55858.3557175926 55652 55858.3789814815 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065001 This is the proposal for the XIS calibration observations in the AO6 term. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 6 AO6-CAL XIS CALIBRATION OBSERVATIONS XIS Y PKS2155-304 329.71 -30.2187 17.74059687 -52.23913549 58.7962 55677.0907291667 55678.5925925926 106011010 60569.3 60000 60577.3 60583 0 60569.3 3 2 0 2 1 0 0 49583.6 49583.6 129709.8 1 PROCESSED 55697.2141898148 55652 55697.2337152778 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065002 This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. CALIBRATION 1 A ISHIDA MANABU NULL NULL JAP 6 AO6-CAL COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON XIS Y CRAB 83.6298 22.0234 184.54825576 -5.78216614 87.1025 55805.2472916667 55806.2585532407 106012010 509.9 40000 509.9 509.9 0 509.9 2 2 0 2 1 0 0 36558.9 36558.9 87353.9 1 PROCESSED 55847.5962268518 55652 55851.4353356482 2.7.16.30 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065003 We propose to observe the Crab in order to calibrate the HXD response functions. CALIBRATION 1 A FUKAZAWA YASUSHI NULL NULL JAP 6 AO6-CAL CALIBRATION OF HXD RESPONSE FUNCTIONS XIS Y CRAB 83.6357 22.0122 184.56070723 -5.78354183 269.6254 55985.4765740741 55986.5585532407 106013010 521.7 40000 521.7 521.7 0 521.7 2 2 0 2 1 0 0 36421.7 36421.7 93465.8 1 PROCESSED 55995.2314351852 55652 55995.2489699074 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065004 We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. CALIBRATION 1 A FUKAZAWA YASUSHI NULL NULL JAP 6 AO6-CAL CALIBRATION OF THE HXD RESPONSE FUNCTIONS XIS Y CRAB 83.6352 22.0094 184.56283497 -5.78543222 269.6994 56000.0051967593 56001.1391435185 106014010 607 40000 607 607 0 607 2 2 0 2 1 0 0 44787.9 44787.9 97955.8 1 PROCESSED 56019.3102430556 55652 56019.3369907407 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065004 We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. CALIBRATION 1 A FUKAZAWA YASUSHI NULL NULL JAP 6 AO6-CAL CALIBRATION OF THE HXD RESPONSE FUNCTIONS XIS Y CRAB 83.6348 22.004 184.56721998 -5.78863608 269.6984 56012.5465393518 56013.5182407407 106015010 533.6 40000 533.6 533.6 0 533.6 3 2 0 2 1 0 0 24545 24545 83940.9 1 PROCESSED 56023.2521875 55652 56023.2694212963 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 065004 We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. CALIBRATION 1 A FUKAZAWA YASUSHI NULL NULL JAP 6 AO6-CAL CALIBRATION OF THE HXD RESPONSE FUNCTIONS XIS Y LOCKMAN HOLE 162.9375 57.26667 149.68932697 53.19392671 -99 NULL NULL 107001010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS Y E0102-72 16.0127 -72.0346 301.55559389 -45.0599301 14.0258 56039.926099537 56040.7294212963 107002010 30438.2 30000 30470.2 30438.2 0 30462.2 2 2 0 2 1 0 0 28052.8 28052.8 69401.9 0 PROCESSED 56054.2591203704 56018 56054.2693634259 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS Y E0102-72 16.00833 -72.03131 301.55717515 -45.06330557 -99 NULL NULL 107002020 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N E0102-72 16.00833 -72.03131 301.55717515 -45.06330557 -99 NULL NULL 107002030 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N E0102-72 16.00833 -72.03131 301.55717515 -45.06330557 -99 NULL NULL 107002040 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N E0102-72_1_4_WIN 16.00833 -72.03131 301.55717515 -45.06330557 -99 NULL NULL 107003010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS Y E0102-72_1_4_WIN 16.00833 -72.03131 301.55717515 -45.06330557 -99 NULL NULL 107003020 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N CYGNUS_LOOP_P8 313.99579 31.47519 75.29734567 -8.8819535 -99 NULL NULL 107004010 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N CYGNUS_LOOP_P8 313.99579 31.47519 75.29734567 -8.8819535 -99 NULL NULL 107004020 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N PERSEUS 49.95042 41.51169 150.57565427 -13.261325 -99 NULL NULL 107005010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N PERSEUS 49.95042 41.51169 150.57565427 -13.261325 -99 NULL NULL 107005020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N PERSEUS_1_4_WIN 49.95042 41.51169 150.57565427 -13.261325 -99 NULL NULL 107006010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N PERSEUS_1_4_WIN 49.95042 41.51169 150.57565427 -13.261325 -99 NULL NULL 107006020 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N RXJ1856.5-3754 284.1441 -37.9006 358.60662879 -17.20863504 88.5024 56019.1209143518 56020.3237384259 107007010 42087.7 40000 42095.7 42087.7 0 42095.7 2 2 0 2 1 0 0 37740.3 37740.3 103914 1 PROCESSED 56034.2854398148 56018 56034.3014699074 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS Y RXJ1856.5-3754 284.14629 -37.9085 358.59958333 -17.21311871 -99 NULL NULL 107007020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N N132D 81.25917 -69.64417 280.30698796 -32.78403883 -99 NULL NULL 107008010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N N132D 81.25917 -69.64417 280.30698796 -32.78403883 -99 NULL NULL 107008020 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N PSK2155-304 329.71696 -30.22558 17.73050588 -52.24586776 -99 NULL NULL 107009010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075001 This is the proposal for the XIS calibration observations in the AO7 cycle. CALIBRATION 1 A TSUJIMOTO MASAHIRO NULL NULL JAP 7 AO7 XIS CALIBRATION OBSERVATIONS XIS N PKS2155-304 329.71696 -30.22558 17.73050588 -52.24586776 -99 NULL NULL 107010010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075002 This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. CALIBRATION 1 A ISHIDA MANABU NULL NULL JAP 7 AO7 COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON XIS Y CRAB 83.63321 22.0145 184.55751251 -5.78426048 -99 NULL NULL 107011010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075003 We propose to observe the Crab in order to calibrate the HXD response functions. CALIBRATION 1 A FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 CALIBRATION OF HXD RESPONSE FUNCTIONS XIS N CRAB 83.63321 22.0145 184.55751251 -5.78426048 -99 NULL NULL 107012010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 075004 We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. CALIBRATION 1 A FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 CALIBRATION OF THE HXD RESPONSE FUNCTIONS XIS N AE AQUARII 310.0457 -0.9355 45.22275468 -24.45710482 264.8759 53673.9022685185 53676.043275463 400001010 70528.9 100000 70528.9 70616.9 70568.9 70544.9 3 3 3 3 1 0 0 59453.8 59453.8 184956.9 2 PROCESSED 54328.3910763889 54247 54036.9851388889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001004 We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. GALACTIC POINT SOURCES 4 A TERADA YUKIKATSU NULL NULL JAP 0 SWG SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU NULL N AE AQUARII 310.0612 -0.931 45.23545862 -24.46836188 250.6241 54033.2319907407 54034.3829282407 400001020 47974.3 50000 47974.3 48595.6 48131.6 48310.3 2 2 2 2 1 0 0 45538.4 45538.4 99423.9 1 PROCESSED 54327.126712963 54526 54109.7083449074 2.0.6.13 8 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001004 We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. GALACTIC POINT SOURCES 4 A TERADA YUKIKATSU NULL NULL JAP 0 SWG SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU HXD N GX 349+2 256.427 -36.366 349.14511841 2.78820606 85.6584 53808.5453240741 53809.2216782407 400003010 25230.8 50000 25230.8 25233.2 25230.8 25230.8 1 1 1 1 1 0 0 20050.7 20050.7 58434 2 PROCESSED 54327.3834375 54247 54041.9132060185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001026 We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. GALACTIC POINT SOURCES 4 A TAKAHASHI HIROMITSU NULL NULL JAP 0 SWG SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) HXD N GX 349+2 256.4194 -36.3657 349.14166441 2.79326977 78.9359 53813.9267708333 53814.6043402778 400003020 28117.7 50000 28117.7 28131.7 28120.4 28120.4 2 2 2 2 1 0 0 25657.3 25657.3 58538 0 PROCESSED 54327.4043634259 54247 54042.1657407407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001026 We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. GALACTIC POINT SOURCES 4 A TAKAHASHI HIROMITSU NULL NULL JAP 0 SWG SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) HXD N SS CYG 325.6789 43.5736 90.55119171 -7.12024619 276.5788 53676.0503703704 53676.9856944444 400006010 39451.2 40000 39451.2 39451.2 39451.2 39451.2 2 2 2 2 1 0 0 32047.2 32047.2 80810 1 PROCESSED 54325.1179282407 54247 54036.9898148148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001043 Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. GALACTIC POINT SOURCES 4 A ISHIDA MANABU NULL NULL JAP 0 SWG SS CYG OBSERVATION IN QUIESCENCE NULL N SS CYG 325.6842 43.5739 90.55430501 -7.12254626 256.8767 53692.6066203704 53693.8646759259 400007010 56043 60000 56059 56179 56043 56059 2 2 2 2 1 0 0 54357.2 54357.2 108665.8 2 PROCESSED 54328.1064351852 54247 54037.9128472222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001044 Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. GALACTIC POINT SOURCES 4 A ISHIDA MANABU NULL NULL JAP 0 SWG-TOO SS CYG OBSERVATION IN OUTBURST XIS N X1630-472 248.4828 -47.3401 336.93914719 0.29801709 78.3341 53774.6318981482 53775.1390972222 400010010 22190.2 200000 22190.2 22190.2 22190.2 22190.2 1 1 1 1 1 0 0 22247 22247 43816 0 PROCESSED 54327.217337963 54247 54040.9540856482 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N X1630-472 248.4706 -47.343 336.93140696 0.30212129 69.0657 53781.9791087963 53782.5474305556 400010020 21429 200000 21429 21485 21429 21429 2 2 2 2 1 0 0 17022.3 17022.3 49101.9 0 PROCESSED 54322.9506828704 54247 54041.4892013889 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N X1630-472 248.4772 -47.3405 336.93627828 0.30053306 75.5959 53794.9708333333 53795.6968055556 400010030 21521.6 200000 21521.6 21521.6 21521.6 21521.6 2 2 2 2 1 0 0 19032.8 19032.8 62718 0 PROCESSED 54323.0049884259 54247 54041.5956018518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N X1630-472 248.5414 -47.3441 336.96314137 0.26612574 120.5775 53802.0758796296 53802.7300231482 400010040 21248.1 200000 21248.1 21249.9 21249.9 21249.9 3 3 3 3 1 0 0 20477.8 20477.8 56512 0 PROCESSED 54320.7897222222 54247 54041.7698726852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N X1630-472 248.5239 -47.3401 336.95804041 0.27755382 107.6616 53809.226412037 53809.743912037 400010050 23167.1 200000 23175.1 23176.9 23176.8 23167.1 2 1 2 2 1 0 0 18860.5 18860.5 44706 0 PROCESSED 54324.0568981482 54247 54041.9302662037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N X1630-472 248.5405 -47.3458 336.96147829 0.2654214 120.3 53817.4260300926 53817.9313425926 400010060 21654.1 200000 21662.1 21654.1 21654.1 21654.1 2 1 2 2 1 0 0 22761.9 22761.9 43655.9 1 PROCESSED 54324.1960532407 54247 54042.1043287037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001058 We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL JAP 0 SWG-TOO FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES HXD N 4U1626-67 248.0601 -67.4675 321.78071552 -13.09322804 103.0359 53803.0543518518 53805.818275463 400015010 102639.2 100000 102654 102639.2 102647.2 102654 2 2 2 2 1 0 0 93393.2 93393.2 238781.9 3 PROCESSED 54330.2336574074 54247 54042.4663657407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001081 The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase, GALACTIC POINT SOURCES 4 A ANGELINI LORELLA NULL NULL JAP 0 SWG 4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINE XIS N CH CYG 291.1621 50.2424 81.86550652 15.56609243 185.7481 53739.5736458333 53740.2919560185 400016020 33305.8 25000 33307.5 33337.8 33315.5 33305.8 2 2 2 2 1 0 0 28461.5 28461.5 62056 1 PROCESSED 54323.9210185185 54247 54039.6712268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001082 CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. GALACTIC POINT SOURCES 4 A MUKAI KOJI NULL NULL JAP 0 SWG SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI XIS N CH CYG 291.1168 50.2494 81.85997028 15.59541424 38.1861 53883.3112962963 53884.1502199074 400016030 35144 35000 35152 35160 35160 35144 1 1 1 1 1 0 0 37459 37459 72447.9 1 PROCESSED 54323.2026157407 54258 54109.7043981482 2.0.6.13 8 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001082 CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. GALACTIC POINT SOURCES 4 A MUKAI KOJI NULL NULL JAP 0 SWG SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI XIS N JUPITER 226.5694 -16.1887 343.96536778 35.7224308 118.4901 53790.7643402778 53791.7940277778 401001010 37759.4 36000 37767.4 37759.4 37767.4 37767.4 2 2 2 2 1 0 0 32836.1 32836.1 88936.1 1 PROCESSED 54323.0172569444 54401 53905.533900463 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C ELSNER RONALD NULL NULL USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N JUPITER 226.5948 -16.1928 343.98613419 35.70433361 118.4906 53791.7941319445 53792.7940277778 401001020 37704 36000 37704 37704 37704 37704 1 1 1 1 1 0 0 32778.1 32778.1 86360 1 PROCESSED 54326.9105208333 54401 53905.5035416667 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C ELSNER RONALD NULL NULL USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N JUPITER 226.6157 -16.1957 344.00356707 35.68981432 118.4907 53792.7940856482 53793.8599421296 401001030 40791.2 36000 40799.2 40791.2 40799.2 40799.2 2 2 2 2 1 0 0 35536.3 35536.3 92073.9 0 PROCESSED 54322.9911574074 54401 53905.5868055556 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C ELSNER RONALD NULL NULL USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N JUPITER 226.6349 -16.1983 344.01962259 35.67652355 118.4908 53793.86 53794.9585532407 401001040 42255.8 36000 42263.8 42263.8 42263.8 42255.8 2 2 2 2 1 0 0 35706.7 35706.7 94905.9 2 PROCESSED 54324.1065625 54401 53906.5712615741 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C ELSNER RONALD NULL NULL USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N XB1323-619 201.6454 -62.1418 307.02498182 0.45033402 99.5731 54109.4794907407 54110.9168402778 401002010 55936.8 50000 55936.8 55936.8 0 55936.8 2 2 0 2 1 0 0 81817.3 81817.3 124176.9 1 PROCESSED 54324.7906365741 54735 54133.0271759259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010002 XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting. GALACTIC POINT SOURCES 4 C DOTANI TADAYASU NULL NULL JAP 1 AO1 BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619 XIS Y SS 433 287.9531 4.9906 39.69950989 -2.2379409 78.6445 53829.6109606482 53830.5327662037 401003010 38676.7 40000 38676.7 38676.7 38676.7 38676.7 2 2 2 2 1 0 0 28241.1 28241.1 79634 1 PROCESSED 54323.8806365741 54394 53906.1478125 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010031 SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. GALACTIC POINT SOURCES 4 A KAWAI NOBUYUKI NULL NULL JAP 1 AO1 SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE XIS N SS 433 287.9527 4.99 39.69879316 -2.23786427 78.6446 53833.4611458333 53834.4579166667 401004010 40197.6 40000 40221.6 40197.6 40229.6 40213.6 2 2 2 2 1 0 0 30474.9 30474.9 86110 2 PROCESSED 54327.1886458333 54400 53906.5501736111 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010031 SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. GALACTIC POINT SOURCES 4 A KAWAI NOBUYUKI NULL NULL JAP 1 AO1 SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE XIS N G11.2-0.3 272.8676 19.433 46.34586116 17.29738119 77.6432 53834.4626041667 53835.6634143518 401010010 43984.6 50000 43992.6 43984.6 43992.6 43992.6 2 2 2 2 1 0 0 37387.9 37387.9 83679.9 1 PROCESSED 54327.0387152778 54397 53905.4671875 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010049 The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU. GALACTIC POINT SOURCES 4 C HAYATO ASAMI NULL NULL JAP 1 AO1 CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3 XIS N CYGNUS X-3 308.2593 40.981 79.93230299 0.62160244 252.424 54052.0902893518 54054.3676388889 401011010 99744.5 100000 99746.2 99746.2 0 99744.5 2 2 0 2 1 0 0 95389.3 95389.3 196745 1 PROCESSED 54331.2167824074 54456 54088.9545023148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010058 We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3. GALACTIC POINT SOURCES 4 C KITAMOTO SHUNJI NULL NULL JAP 1 AO1 WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU SPE Y LMC X-2 80.025 -71.9941 283.14092563 -32.7117801 313.3022 53849.381712963 53850.7731365741 401012010 56152 60000 56165.7 56165.7 56152 56160 2 2 2 2 1 0 0 73408 73408 120193.8 1 PROCESSED 54329.0935185185 54394 53907.6288078704 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010090 We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not. GALACTIC POINT SOURCES 4 B TAKAHASHI HIROMITSU NULL NULL JAP 1 AO1 DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2 HXD N SGR1806-20 272.1595 -20.349 10.0481975 -0.20823053 88.7483 54189.6305555556 54190.0627199074 401021010 19288.9 20000 19288.9 19595 0 19356.3 1 1 0 1 1 0 0 16507.1 16507.1 37327.9 1 PROCESSED 54323.026099537 54561 54209.5169212963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010124 We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 1 AO1-TOO PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" HXD N SGR1900+14 286.803 9.3875 43.07594962 0.80149907 86.5533 53826.3631597222 53826.9113310185 401022010 17056.2 20000 17704.6 21707.4 21655.5 17056.2 1 2 1 1 1 0 0 14360.4 14360.4 47336 1 PROCESSED 54323.156400463 54394 53906.0977893518 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010124 We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 1 AO1-TOO PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" HXD N HESS J1837-069 279.4395 -6.8651 25.2664546 -0.10276403 102.6144 54164.5341898148 54165.4286342593 401026010 42191.1 40000 42191.1 42199.1 0 42207.1 2 2 0 2 1 0 0 37702.1 37702.1 77259.9 1 PROCESSED 54322.861087963 54750 54171.2613425926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010131 The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 1 AO1 INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL HXD Y 1E1207.4-5209 182.5062 -52.436 296.5458403 9.92149786 302.4939 53946.5682060185 53948.2603587963 401030010 96351.9 120000 96351.9 102278.4 96367.9 96351.9 3 2 3 3 1 0 0 94049.8 94049.8 135379.9 1 PROCESSED 54328.1902430556 54750 54132.8187268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010152 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. GALACTIC POINT SOURCES 4 B YOSHIDA ATSUMASA NULL NULL JAP 1 AO1 A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 XIS N 1E1207.4-5209 182.4916 -52.442 296.53791481 9.91413144 148.6893 54146.2087384259 54147.6390509259 401030020 49826.6 50000 50073.4 49826.6 0 50089.4 1 2 0 1 1 0 0 44446.8 44446.8 123576 2 PROCESSED 54329.2028009259 54750 54153.9886458333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010152 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. GALACTIC POINT SOURCES 4 B YOSHIDA ATSUMASA NULL NULL JAP 1 AO1 A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 XIS Y AB DOR 82.2835 -65.427 275.26967334 -33.00819219 154.6774 54060.0265277778 54061.4586111111 401031010 53451.7 80000 53451.7 53459.7 0 53461.4 2 2 0 2 1 0 0 48033.4 48033.4 123708 1 PROCESSED 54324.929212963 54502 54133.0222916667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011021 We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. GALACTIC POINT SOURCES 4 B AUDARD MARC NULL NULL USA 1 AO1 NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES HXD N AB DOR 82.2881 -65.4658 275.31538375 -33.00189818 204.2849 54108.0647569444 54109.4724421296 401031020 49096.5 45000 49096.5 49096.5 0 49096.5 2 2 0 2 1 0 0 44961.1 44961.1 121619.9 2 PROCESSED 54324.0499074074 54502 54133.0127083333 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011021 We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. GALACTIC POINT SOURCES 4 B AUDARD MARC NULL NULL USA 1 AO1 NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES HXD N HR 9024 357.4125 36.4308 109.27773456 -24.79729068 49.8624 53939.0616782407 53940.6016087963 401032010 58775.7 60000 58799.7 58775.7 58783.7 58791.7 2 2 2 2 1 0 0 56011.6 56011.6 133039.8 1 PROCESSED 54324.8656597222 54401 53950.2624074074 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011022 Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. GALACTIC POINT SOURCES 4 B TESTA PAOLA NULL NULL USA 1 AO1 GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS XIS N SIGMA^2 CRB 243.6552 33.7881 54.56402364 46.14689859 281.1207 53969.4764467593 53972.1925231482 401034010 109160.4 110000 109190.4 109160.4 109168.4 109176.4 2 2 2 2 1 0 0 98837.6 98837.6 234653.9 3 PROCESSED 54330.9158217593 54526 54021.2578587963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011025 Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD. GALACTIC POINT SOURCES 4 B BROWN ALEXANDER NULL NULL USA 1 AO1 SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM HXD N BETA LYR 282.5094 33.3738 63.19462876 14.79594569 59.4704 53862.545474537 53862.9952083333 401036010 20251.5 20000 20267.5 20251.5 20267.5 20267.5 2 2 2 2 1 0 0 9894.7 9894.7 38851.9 1 PROCESSED 54323.0649884259 54401 53913.8191550926 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011031 The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 1 AO1 AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE XIS N BETA LYR 282.5098 33.3716 63.19266924 14.79477853 53.4974 53867.1260185185 53867.6252199074 401036020 21496.2 20000 21496.2 21496.2 21496.2 21496.2 1 1 1 1 1 0 0 19164.2 19164.2 43119.9 2 PROCESSED 54323.1969212963 54401 53914.2784143518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011031 The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 1 AO1 AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE XIS N BETA LYR 282.5093 33.3719 63.19278609 14.79528012 53.4973 53871.4311226852 53871.8571875 401036030 18195.4 20000 18195.4 18195.4 18195.4 18195.4 2 2 2 2 1 0 0 19842.1 19842.1 36807.9 0 PROCESSED 54320.7847337963 54401 53920.4164351852 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011031 The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 1 AO1 AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE XIS N 1RX J154814.5-452845 237.0511 -45.4226 332.46961393 7.07040697 85.7358 54132.6368518518 54135.3543865741 401037010 99454.1 100000 99454.1 99462.1 0 99470.1 2 2 0 2 1 0 0 86855.2 86855.2 234783.8 3 PROCESSED 54329.9169212963 54702 54139.4767939815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011102 Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. GALACTIC POINT SOURCES 4 A MUKAI KOJI NULL NULL USA 1 AO1 BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION HXD Y 1RXS J213344.1+51072 323.4354 51.1973 94.50909334 -0.42447705 94.0452 53854.2853009259 53856.2501736111 401038010 81924.1 80000 81924.1 81924.1 81924.1 81924.1 2 2 2 2 1 0 0 62888.1 62888.1 169726.1 3 PROCESSED 54327.5816550926 54391 53908.1887962963 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011102 Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. GALACTIC POINT SOURCES 4 A MUKAI KOJI NULL NULL USA 1 AO1 BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION HXD N V893 SCO 243.8144 -28.6275 348.06577336 15.88028883 274.6746 53973.4024189815 53974.056412037 401041010 18497.8 20000 18497.8 18497.8 18497.8 18497.8 2 2 2 2 1 0 0 16140.3 16140.3 56482 0 PROCESSED 54322.6723726852 54526 54053.4763888889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011103 The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies. GALACTIC POINT SOURCES 4 B MUKAI KOJI NULL NULL USA 1 AO1 CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE XIS N T CRB 239.8773 25.9106 42.36027985 48.16117824 268.9321 53984.9474652778 53986.0911921296 401043010 46303.3 50000 46311.3 46311.3 46319.3 46303.3 2 2 2 2 1 0 0 45431.4 45431.4 98815.9 1 PROCESSED 54324.1068981482 54526 54053.4340856482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011106 Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism. GALACTIC POINT SOURCES 4 A SOKOLOSKI JENNIFER NULL NULL USA 1 AO1 THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES XIS N 4U 1705-44 257.2295 -44.1004 343.32321952 -2.34240238 264.0794 53976.2429166667 53976.7731712963 401046010 18315.5 20000 18315.5 18315.5 18315.5 18315.5 2 2 2 2 1 0 0 15371.5 15371.5 45809.9 0 PROCESSED 54322.587349537 54526 54021.306087963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011112 We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. GALACTIC POINT SOURCES 4 A YOUNG ANDREW NULL NULL USA 1 AO1 REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 XIS N 4U 1705-44 257.2281 -44.1019 343.32141433 -2.34248879 264.0666 53996.5173611111 53996.8619675926 401046020 17134 20000 17342 17134 17334 17334 1 1 1 1 1 0 0 15447.7 15447.7 29767.9 0 PROCESSED 54323.9647569444 54526 54020.9055555556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011112 We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. GALACTIC POINT SOURCES 4 A YOUNG ANDREW NULL NULL USA 1 AO1 REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 XIS N 4U 1705-44 257.2313 -44.1028 343.32206131 -2.34487049 297.0793 54014.4242708333 54015.0891087963 401046030 20065 20000 20065 20065 20065 20065 2 2 2 2 1 0 0 17919.6 17919.6 57423.9 2 PROCESSED 54322.900462963 54526 54021.6765162037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011112 We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. GALACTIC POINT SOURCES 4 A YOUNG ANDREW NULL NULL USA 1 AO1 REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 XIS N 4U 1820-30 275.9207 -30.3623 2.78792233 -7.91550172 265.9754 53992.9234606482 53993.6605902778 401047010 25700.8 37000 25700.8 25810.9 25723.9 25714.8 2 1 2 2 1 0 0 31878.2 31878.2 63633.9 1 PROCESSED 54329.4727662037 54526 54021.2227083333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011113 The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. GALACTIC POINT SOURCES 4 B MILLER JON NULL NULL USA 1 AO1 A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES XIS N SERPENS X-1 279.9934 5.0285 36.11311789 4.83561165 256.1423 54032.2853819444 54033.2259143518 401048010 37157.8 37000 37157.8 37269.8 37205.8 37165.8 2 1 2 2 1 0 0 31069.5 31069.5 81239.9 2 PROCESSED 54330.1792939815 54526 54056.4719328704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011113 The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. GALACTIC POINT SOURCES 4 B MILLER JON NULL NULL USA 1 AO1 A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES XIS N CYGNUS X-2 326.1653 38.3323 87.3318132 -11.3049847 76.3142 53871.8636805556 53872.7293171296 401049010 39390.3 37000 39390.3 39406.3 39390.3 39390.3 2 1 2 2 1 0 0 36880.4 36880.4 74786 1 PROCESSED 54330.792962963 54401 53927.6429166667 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011113 The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. GALACTIC POINT SOURCES 4 B MILLER JON NULL NULL USA 1 AO1 A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES XIS N 4U 1636-536 250.2262 -53.7541 332.91086545 -4.81751491 91.2457 54140.3877546296 54140.99125 401050010 24232 19000 24232 24232 0 24232 2 1 0 2 1 0 0 21689.5 21689.5 52136 0 PROCESSED 54322.7352083333 54525 54151.5052893518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A HOMAN JEROEN NULL NULL USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y 4U 1636-536 250.2273 -53.7542 332.91122007 -4.81806999 91.2447 54153.2955787037 54154.3544560185 401050020 40096 38000 40096 40104 0 40096 2 1 0 2 1 0 0 35550 35550 91477.9 0 PROCESSED 54328.4423032407 54525 54158.392037037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A HOMAN JEROEN NULL NULL USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y 4U 1636-536 250.2272 -53.754 332.91133194 -4.81789372 91.2454 54160.0424421296 54160.8931597222 401050030 38719.3 38000 38727.4 38719.3 0 38719.4 2 1 0 2 1 0 0 48145.9 48145.9 73498 1 PROCESSED 54327.3161921296 54695 54167.6400462963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A HOMAN JEROEN NULL NULL USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y 4U 1636-536 250.2277 -53.7538 332.91167841 -4.81798429 93.2445 54186.4802777778 54187.3043287037 401050040 32130.4 38000 32130.4 32138.4 0 32130.4 2 1 0 2 1 0 0 27784.2 27784.2 71177.9 1 PROCESSED 54324.2956597222 54695 54209.541412037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A HOMAN JEROEN NULL NULL USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y 4U 1636-536 250.2259 -53.7533 332.911352 -4.8168543 100.7755 54188.4720717593 54188.7856944445 401050050 12241.8 38000 12249.8 12241.8 0 12249.8 2 1 0 2 1 0 0 11804 11804 27088 0 PROCESSED 54320.8789236111 54695 54200.4687731482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A HOMAN JEROEN NULL NULL USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y 4U 1822-37 276.4461 -37.1042 356.85149319 -11.29112534 258.4537 54010.4563888889 54011.5189699074 401051010 37743.4 40000 37768.2 37768.2 37743.4 37743.4 2 2 2 2 1 0 0 33178.5 33178.5 91805.9 0 PROCESSED 54324.6250347222 54695 54024.6539814815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011121 We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe. GALACTIC POINT SOURCES 4 B COTTAM JEAN NULL NULL USA 1 AO1 ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37 XIS Y IGRJ16465-4507 251.6303 -45.1738 340.00343338 0.10772124 284.9562 53987.3839814815 53987.9203009259 401052010 22527.9 20000 22535.9 22527.9 22535.9 22535.9 2 2 2 2 1 0 0 24645.4 24645.4 46332 0 PROCESSED 54320.9010648148 54526 54021.113287037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N SWIFTJ2000.6+3210 300.0869 32.2033 68.99570836 1.1443147 87.4233 53837.6619212963 53837.9139351852 401053010 12438.4 20000 12444 12451.2 12451.2 12438.4 1 1 1 1 1 0 0 9876.7 9876.7 21767.9 0 PROCESSED 54320.5594444445 54775 53927.3549189815 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N SWIFTJ2000.6+3210 300.1137 32.1218 68.93835501 1.08211502 255.6072 54039.0205671296 54039.3029976852 401053020 12748.4 10000 12756.4 12748.4 12756.4 12756.4 2 2 2 2 1 0 0 11727 11727 24393.9 0 PROCESSED 54320.6820717593 54775 54056.1959953704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD Y IGRJ16493-4348 252.3173 -43.8652 341.31911758 0.57823277 287.444 54013.8822916667 54014.4204166667 401054010 21199.8 20000 21215.8 21215.8 21199.8 21207.8 3 3 3 3 1 0 0 20219.7 20219.7 46463.9 1 PROCESSED 54322.6086574074 54695 54025.4796412037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD Y SWIFTJ1010.1-5747 152.7309 -57.8539 282.8705066 -1.37559689 290.7012 53891.2175 53891.5544560185 401055010 19171.7 20000 19171.7 19171.7 19171.7 19171.7 2 2 2 2 1 0 0 17877.8 17877.8 29087.9 0 PROCESSED 54320.6983333333 54401 53926.1075347222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N IGRJ16195-4945 244.8541 -49.816 333.49117084 0.29973526 284.0301 53998.8508333333 53999.7231481482 401056010 39148.6 40000 39148.6 39148.6 39148.6 39148.6 2 2 2 2 1 0 0 42265.2 42265.2 75357.9 1 PROCESSED 54322.8721875 54526 54020.9227199074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N 4U1907+09 287.4013 9.8378 43.74739314 0.48531727 60.2599 53857.2580324074 53858.7322222222 401057010 58440.3 60000 58440.3 58456.3 58448.3 58456.3 2 2 2 2 1 0 0 38821.5 38821.5 127353.9 1 PROCESSED 54326.7703587963 54401 53913.4367476852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011133 We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 1 AO1 THE BROAD BAND SPECTRUM OF 4U1907+09 XIS N 4U1700-37 255.9894 -37.8441 347.75582102 2.17172645 269.6945 53991.447662037 53992.918912037 401058010 81442.5 80000 81456.9 81470.4 81442.5 81454.4 3 3 3 3 1 0 0 82109.3 82109.3 127109 1 PROCESSED 54329.710150463 54526 54053.5428240741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011135 The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse. GALACTIC POINT SOURCES 4 A KALLMAN TIMOTHY NULL NULL USA 1 AO1 IRON LINE VARIABILITY IN 4U1700-37 XIS N CYGNUS X-1 299.6124 35.133 71.28577556 3.01567368 256.2202 54038.1501273148 54038.8225 401059010 27706.8 30000 27706.8 27737.8 27706.8 27706.8 2 1 2 2 1 0 0 27689.2 27689.2 58083.9 0 PROCESSED 54325.0852662037 54526 54063.4924884259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011141 We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 B NOWAK MICHAEL NULL NULL USA 1 AO1 ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA HXD N GX 339-4 255.7025 -48.7916 338.93635594 -4.32587966 86.7489 54143.2316087963 54146.2003009259 401068010 77205.3 100000 83893.5 77205.3 0 82113.8 2 2 0 2 1 0 0 94026 94026 256484 4 PROCESSED 54332.1519907407 54535 54167.7751851852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011146 Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme. GALACTIC POINT SOURCES 4 A MILLER JON NULL NULL USA 1 AO1-TOO SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST XIS N SGR 1806-20 272.166 -20.4729 9.94279657 -0.27364584 269.9473 53987.9261921296 53989.1668287037 401092010 48915.5 50000 48915.5 48923.5 48931.5 48931.5 1 1 1 1 1 0 0 55408.5 55408.5 107175.9 1 PROCESSED 54322.8112615741 54526 54021.1112615741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012017 The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters. GALACTIC POINT SOURCES 4 B MEREGHETTI SANDRO NULL NULL EUR 1 AO1 COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE HXD N ALGOL 47.0831 40.8965 149.0355551 -14.93487401 244.4771 54167.6197222222 54169.6132986111 401093010 102164.2 105000 102164.2 102164.2 0 102164.2 2 2 0 2 1 0 0 102472.9 102472.9 172192.8 1 PROCESSED 54329.1126041667 54736 54186.3983564815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012024 Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD. GALACTIC POINT SOURCES 4 C GUEDEL MANUEL NULL NULL EUR 1 AO1 A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL HXD Y IGR J16318-4848 247.9691 -48.8061 335.63186461 -0.44896472 266.5948 53961.4825 53964.3488310185 401094010 97253.8 100000 97269.8 97253.8 97269.8 97269.8 2 2 2 2 1 0 0 87112.8 87112.8 247605.9 5 PROCESSED 54330.6531365741 54526 54020.9181597222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012034 We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848. GALACTIC POINT SOURCES 4 B WILMS JOERN NULL NULL EUR 1 AO1 OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION XIS N XB 1916-053 289.7027 -5.2415 31.35614078 -8.46800846 250.2538 54047.242974537 54048.1119791667 401095010 38464.7 40000 39096.7 39088.7 38464.7 39096.7 2 2 2 2 1 0 0 37485.7 37485.7 75082 2 PROCESSED 54324.2446296296 54735 54088.866087963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012038 We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV. GALACTIC POINT SOURCES 4 A DIAZ TRIGO MARIA NULL NULL EUR 1 AO1 BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS XIS Y HESS J1731-347 263.0179 -34.7706 353.53173388 -0.68198005 79.8005 54154.7807060185 54155.7432291667 401099010 40618.9 38000 40626.9 40618.9 0 40626.9 2 2 0 2 1 0 0 34647.9 34647.9 83155.9 0 PROCESSED 54327.1666550926 54528 54160.3931944444 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012042 The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator. GALACTIC POINT SOURCES 4 A PUEHLHOFER GERD NULL NULL EUR 1 AO1 THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347 XIS N 1E 1841-045 280.3141 -4.8735 27.4352849 0.03686802 77.3227 53844.4525462963 53847.1328009259 401100010 97962.2 100000 97962.2 97970.2 97970.9 97970.9 2 2 2 2 1 0 0 63474 63474 231539.9 2 PROCESSED 54328.5835185185 54401 53907.2806597222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014204 Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data. GALACTIC POINT SOURCES 4 A HARRUS ILANA NORII MIKIO USJ 1 AO1 SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73 HXD N HESSJ1813-178 273.3946 -17.7704 12.87014503 0.01155473 90.9367 54160.8999768518 54162.2814699074 401101010 63839.1 65000 63847.1 63839.1 0 63847.1 2 2 0 2 1 0 0 57756.1 57756.1 119351.9 1 PROCESSED 54326.8273726852 54736 54167.6346990741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014214 Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies. GALACTIC POINT SOURCES 4 B REIMER OLAF EBISAWA KEN USJ 1 AO1 IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE? HXD Y EX HYA 193.0706 -29.2994 303.15288952 33.57198642 300.0004 54299.8912152778 54302.4377199074 402001010 100515.7 100000 100523.7 100515.7 0 100523.7 2 2 0 2 1 0 0 91113.5 91113.5 219959.9 1 PROCESSED 54339.478912037 54707 54339.5139467593 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020008 The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. GALACTIC POINT SOURCES 4 A ISHIDA MANABU NULL NULL JAP 2 AO2 MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS HXD Y V1223 SGR 283.7445 -31.105 5.0082738 -14.31987205 79.9528 54203.4803240741 54204.9418055556 402002010 60706 60000 60706 60706 0 60706 2 2 0 2 1 0 0 46286.1 46286.1 126271.9 2 PROCESSED 54327.481412037 54744 54210.6596875 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020008 The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. GALACTIC POINT SOURCES 4 A ISHIDA MANABU NULL NULL JAP 2 AO2 MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS HXD Y 1RXSJ174459.5-172640 266.2467 -17.4406 9.76958181 6.08973572 101.0461 54555.6304050926 54556.5834953704 402003010 43579.3 40000 43595.3 43579.3 0 43603.3 1 1 0 1 1 0 0 29591.6 29591.6 82343.9 1 PROCESSED 54570.1429282407 54937 54570.1529282407 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020015 We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 2 AO2 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS Y 1RXSJ165256.3-264503 253.236 -26.7533 355.1420085 10.81079439 277.5876 54337.0024421296 54338.0419444444 402004010 49582.2 40000 49582.2 49582.2 0 49582.2 2 2 0 2 1 0 0 46662.1 46662.1 89777.9 2 PROCESSED 54404.494212963 54723 54350.4155092593 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020015 We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 2 AO2 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS Y 1RXS J070407.9+26250 106.0341 26.4126 190.27497025 14.29877104 282.0717 54548.4868865741 54549.9862384259 402008010 58315.7 50000 58323.7 58315.7 0 58323.7 1 1 0 1 1 0 0 49476.6 49476.6 129527.8 0 PROCESSED 54566.3128240741 54933 54566.326712963 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020029 Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically. GALACTIC POINT SOURCES 4 C ISHIDA MANABU NULL NULL JAP 2 AO2 OBSERVATIONS OF SOFT INTERMEDIATE POLARS XIS Y 1RXS J180340.0+40121 270.932 40.2098 66.8583442 25.77561005 157.538 54478.0290972222 54479.1877777778 402009010 53090.7 50000 53090.7 53090.7 0 53090.7 1 1 0 1 1 0 0 44348.9 44348.9 100095.9 3 PROCESSED 54490.0612847222 54864 54490.0707291667 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020029 Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically. GALACTIC POINT SOURCES 4 C ISHIDA MANABU NULL NULL JAP 2 AO2 OBSERVATIONS OF SOFT INTERMEDIATE POLARS XIS Y 4U 0142+61 26.4803 61.7944 129.32255084 -0.39946076 40.959 54325.1695949074 54327.5209259259 402013010 99674.4 100000 99674.4 99674.4 0 99674.4 2 2 0 2 1 0 0 101609.6 101609.6 203129.7 4 PROCESSED 54404.5831944445 54730 54347.6221296296 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020058 Recently, high energy pulsed x-ray emissions from anomalous x-ay pulsears have been founded. This emissions extend to neary 100 keV with photon index ~1, and the emission mechanism is unknown. In order to trace this enigmatic component, we propose the observation of the anomalous x-ray pulsar 4u 0142+61 with 100 ksec exposures. The main aim of this observation is to examine how high energy this emission extend to. Because the these emissions are almost 100% pulsed component, so using the pulse on-off method, we can achive the ultimate sensitivity not depending on the reproducibility of the background but depending only on the photon statistics. If the spectrum have the strong break neary ~250 keV, this emissions have originated as the compton scatterd photons in the star surface. GALACTIC POINT SOURCES 4 A ENOTO TERUAKI NULL NULL JAP 2 AO2 THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61 HXD Y PSR B1259-63 195.6821 -63.8856 304.1741357 -1.04108664 280.935 54288.622025463 54289.062662037 402014010 21863.4 20000 21871.4 21863.4 0 21871.4 1 1 0 1 1 0 0 26860 26860 38063.9 1 PROCESSED 54328.4817361111 54696 54328.4884722222 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6782 -63.8867 304.17237227 -1.04211039 282.6534 54290.6852083333 54291.1876041667 402014020 19481.7 20000 19481.7 19481.7 0 19481.7 2 2 0 2 1 0 0 26911.1 26911.1 43378 1 PROCESSED 54328.4960416667 54696 54328.5032060185 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6777 -63.8873 304.1721261 -1.04270018 282.6527 54292.6291319444 54293.1910763889 402014030 22721.7 20000 22721.7 22721.7 0 22721.7 2 2 0 2 1 0 0 24280.8 24280.8 48545.9 0 PROCESSED 54339.0197106482 54707 54339.0273842593 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6732 -63.8823 304.17036556 -1.03761834 285.8945 54294.6568865741 54295.3459953704 402014040 22914.9 20000 22914.9 22914.9 0 22914.9 2 2 0 2 1 0 0 21070.6 21070.6 59495.9 1 PROCESSED 54339.3026273148 54709 54339.4142592593 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6556 -63.8839 304.16255435 -1.03887935 293.4832 54304.2811226852 54304.6877777778 402014050 19702.3 20000 19702.3 19702.3 0 19702.3 1 1 0 1 1 0 0 17754.9 17754.9 35127.9 0 PROCESSED 54339.2103587963 54707 54339.2175347222 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6402 -63.8787 304.15600524 -1.03339065 289.9992 54315.2640856482 54316.0419444444 402014060 24038.8 20000 24038.8 24038.8 0 24038.8 2 2 0 2 1 0 0 21580.8 21580.8 67195.9 1 PROCESSED 54404.5138425926 54722 54347.6946527778 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6594 -63.8834 304.16424752 -1.0384525 292.9998 54330.0581481482 54330.6877777778 402014070 20481.2 20000 20481.2 20481.2 0 20482.9 2 2 0 2 1 0 0 19470.3 19470.3 54364 0 PROCESSED 54404.5158680556 54724 54356.2228472222 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y PSR B1259-63 195.6089 -63.8685 304.14267075 -1.0226082 321.9333 54348.2308449074 54348.6043287037 402014080 18332.7 20000 18340.7 18348.7 0 18332.7 1 1 0 1 1 0 0 22351.3 22351.3 32260 0 PROCESSED 54404.5153356482 54724 54356.1999537037 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y LS 5039 276.5633 -14.9109 16.82651822 -1.31880921 270.412 54352.6780555556 54358.4725 402015010 203239.9 200000 203239.9 203239.9 0 203239.9 2 2 0 2 1 0 0 181095 181095 442087.9 4 PROCESSED 54384.6553009259 54745 54384.7259027778 2.1.6.14 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020062 The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system. GALACTIC POINT SOURCES 4 A TAKAHASHI TADAYUKI NULL NULL JAP 2 AO2 SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039 HXD Y HETEJ1900.1-2455 285.0506 -24.9802 11.25454685 -12.90928139 259.4192 54389.5913425926 54390.5071064815 402016010 41759.1 40000 41778.8 41759.1 0 41775.1 2 2 0 2 1 0 0 39906.3 39906.3 79105.8 1 PROCESSED 54403.1128935185 54771 54403.1292708333 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020068 We propose a 40 ks observation of the accreting millisecond pulsar HETE J1900.1-2455, which was discovered by HETE-2 only recently. Good sensitivity in 10-100keV and enough timing resolution of HXD on Suzaku allow us to measure the light curve and the phase resolved spectra of its hard X-ray pulsation, with which we study the physical parameters of the Comptonizing plasma that is considered as the source of the hard X-ray emission of accreting millisecond pulsars. With XIS, we study the radiation from the accretion disk and the neutron star surface, and search for spectral features such as emission lines or absorption edges, which will provide information on the binary environment. GALACTIC POINT SOURCES 4 B SUZUKI MOTOKO NULL NULL JAP 2 AO2 HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455 HXD Y 4U 1700+24 256.6316 23.9071 45.07419011 32.98144858 280.149 54334.7787615741 54335.875162037 402023010 50244.5 50000 50252.5 50260.5 0 50244.5 2 2 0 2 1 0 0 45326.8 45326.8 94715.8 2 PROCESSED 54404.5649884259 54723 54350.4606481482 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020105 We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV. GALACTIC POINT SOURCES 4 B NAGAE OSAMU NULL NULL JAP 2 AO2 STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24 HXD Y CYG OB2 ASSOCIATION 308.2175 41.2935 80.16491027 0.83267098 220.3949 54452.9185532407 54453.843912037 402030010 41114.7 40000 41114.7 41114.7 0 41114.7 2 2 0 2 1 0 0 37918.1 37918.1 79943.9 0 PROCESSED 54460.6387962963 54828 54460.6521643518 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020150 Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. GALACTIC POINT SOURCES 4 C KITAMOTO SHUNJI NULL NULL JAP 2 AO2 STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 XIS Y TEVJ2032+4130 308.0461 41.5016 80.25613164 1.05964615 221.0839 54451.984212963 54452.9176157407 402031010 40043.9 40000 40043.9 40043.9 0 40043.9 2 2 0 2 1 0 0 37309.1 37309.1 80641.9 1 PROCESSED 54460.6387384259 54828 54460.6569675926 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020150 Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. GALACTIC POINT SOURCES 4 C KITAMOTO SHUNJI NULL NULL JAP 2 AO2 STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 XIS Y EV LAC 341.7127 44.3232 100.60502245 -13.08073089 256.1601 54432.9692013889 54434.4655208333 402032010 68949.3 100000 68949.3 69133.3 0 69127.5 2 1 0 2 1 0 0 65011.3 65011.3 129232.8 2 PROCESSED 54441.0700231482 54808 54441.0876851852 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021013 We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare. GALACTIC POINT SOURCES 4 C HWANG UNA NULL NULL USA 2 AO2 FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LAC XIS Y SIGMA GEM 115.843 28.9438 191.13214337 23.30670736 104.4403 54394.4090162037 54397.9690162037 402033010 142889.7 125000 142889.7 142993.6 0 142985.6 2 2 0 2 1 0 0 124447.1 124447.1 307541.6 1 PROCESSED 54407.7917824074 54776 54407.830474537 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021014 Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission on RS CVn binaries. We propose a 125 ksec (3-4 day elapsed time) observation of the RS CVn binary Sigma Gem. Our goals are i) to better characterize its hard (>10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data, and iv) compare long duration flares on Sigma Gem with the 6 hour flares of Sigma2 CrB. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability at 10-25 keV provided by HXD. GALACTIC POINT SOURCES 4 C BROWN ALEXANDER NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL STRUCTURE ON THE RS CVN BINARY SIGMA GEM (K0III +?) HXD Y HD432 2.3072 59.1394 117.5327944 -3.28915956 247.7181 54469.7038310185 54470.5154513889 402034010 38240.6 40000 38248.6 38240.6 0 38248.6 2 2 0 2 1 0 0 35050.3 35050.3 70120 1 PROCESSED 54542.2134722222 54908 54483.4635532407 2.2.7.18 4 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021016 Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. GALACTIC POINT SOURCES 4 C AYRES THOMAS NULL NULL USA 2 AO2 ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS XIS Y HD432 2.3079 59.1397 117.53319828 -3.2889222 246.0535 54471.6956944444 54472.297349537 402034020 26984.4 27000 26984.4 26984.4 0 26984.4 1 1 0 1 1 0 0 24601 24601 51975.9 0 PROCESSED 54483.3790740741 54871 54483.3863773148 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021016 Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. GALACTIC POINT SOURCES 4 C AYRES THOMAS NULL NULL USA 2 AO2 ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS XIS Y ZETA OPH 249.2878 -10.5628 6.28378927 23.59180747 94.9452 54540.8758912037 54543.8543287037 402038010 105583.7 100000 105591.7 105591.7 0 105583.7 2 2 0 2 1 0 0 79981.3 79981.3 257317.8 2 PROCESSED 54553.3433217593 54922 54553.3785300926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021022 Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability. GALACTIC POINT SOURCES 4 C WALDRON WAYNE NULL NULL USA 2 AO2 MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPH XIS Y ETA CARINAE 161.2181 -59.7282 287.59637986 -0.67920855 289.0006 54274.2459259259 54275.9015509259 402039010 58396.1 50000 58404.1 58396.1 0 58404.1 2 2 0 2 1 0 0 51552 51552 143009.9 1 PROCESSED 54322.4959953704 54695 54322.5140856482 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021026 XMM-Newton observations in 2003 suggest that X-ray emission from Eta Carinae has a hard X-ray component above 10 keV in addition to the thermal emission with kT ~3-5 keV. The excess is apparently strongest near the 2-10 keV X-ray maximum, and possibly produced by very hot plasma or 1st-order Fermi acceleration of particles which then inverse Compton-upscatter UV seed photons from the stellar photospheres. We propose a 50 ksec observation of Eta Carinae with the Suzaku telescope during AO2, compare the X-ray spectrum with earlier observations and determine the level of emission at E >9 keV. GALACTIC POINT SOURCES 4 B HAMAGUCHI KENJI NULL NULL USA 2 AO2 HARD X-RAY EMISSION FROM ETA CARINAE HXD Y RT CRU 188.7055 -64.6161 301.15157727 -1.80180428 281.609 54283.5270023148 54284.2433333333 402040010 50880.6 50000 50880.6 50880.6 0 50880.6 2 2 0 2 1 0 0 42850.6 42850.6 61887.9 0 PROCESSED 54328.4465972222 54695 54328.4668055556 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021102 Symbiotic stars are interacting binaries in which a white dwarf (WD) accretes from the wind of a red giant. Their X-ray emission is typically very soft. Recently, however, 4 symbiotics have been detected out to almost 100 keV. Suzaku observations of two of these sources revealed that the hard X-rays emanated from an extremely hot thermal plasma. One means of producing such hot gas is accretion onto a near Chandrasekhar-mass WD. We propose to use the unique capabilities of Suzaku to test this hypothesis. We will use broad-band X-ray spectral fitting to determine the temperature of the hot plasma, hard X-ray timing studies to search for or constrain rapid variations due to either magnetic or non-magnetic accretion, and Fe line diagnostics to investigate the role of scattering. GALACTIC POINT SOURCES 4 B SOKOLOSKI JENNIFER NULL NULL USA 2 AO2 ARE HARD X-RAY SYMBIOTICS PROGENITORS OF TYPE IA SUPERNOVAE? HXD Y VY AQR 318.0426 -8.8307 41.59091784 -35.22055705 252.6652 54414.6528587963 54415.3855787037 402043010 25447.3 20000 25447.3 25447.3 0 25447.3 2 2 0 2 1 0 0 22360.5 22360.5 63299.9 2 PROCESSED 54423.1616203704 54790 54423.1702314815 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021105 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 2 AO2 BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE XIS Y SW UMA 129.1769 53.4845 164.80593722 36.96002764 98.2716 54410.2367708333 54410.6252199074 402044010 16899.1 20000 16907.1 16899.1 0 16907.1 1 1 0 1 1 0 0 13896.9 13896.9 33551.9 1 PROCESSED 54417.6038657407 54784 54417.2697569444 2.1.6.16 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021105 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 2 AO2 BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE XIS Y SS AUR 93.3423 47.7333 166.0127795 13.79596984 289.1089 54529.7508796296 54530.180775463 402045010 19471.4 20000 19471.4 19471.4 0 19471.4 1 1 0 1 1 0 0 17378 17378 37135.9 0 PROCESSED 54539.2152083333 54905 54539.2223726852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021105 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 2 AO2 BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE XIS Y BZ UMA 133.4243 57.801 159.01672768 38.83001001 307.4767 54549.9926388889 54550.4446064815 402046010 29746.6 20000 29754.6 29754.6 0 29746.6 2 2 0 2 1 0 0 24921.2 24921.2 39045.9 0 PROCESSED 54566.2147800926 54933 54566.2225231482 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021105 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 2 AO2 BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE XIS Y GX17+2 274.0087 -14.1006 16.37694194 1.24456043 269.7113 54362.2773032407 54362.8543402778 402050010 19095.9 20000 19095.9 19104.4 0 19095.9 2 1 0 2 1 0 0 16044.5 16044.5 49849.9 0 PROCESSED 54384.4371527778 54751 54384.4487037037 2.1.6.14 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021111 Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 2 AO2 OBSERVING THE SPECTRUM AND HALO OF GX17+2 HXD Y GX17+2 274.0098 -14.0991 16.37876929 1.24433559 268.3778 54370.5988078704 54371.2502199074 402050020 23011.7 20000 23019.7 23025.8 0 23011.7 3 2 0 3 1 0 0 19048.8 19048.8 56276 0 PROCESSED 54402.3354976852 54769 54402.3511921296 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021111 Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 2 AO2 OBSERVING THE SPECTRUM AND HALO OF GX17+2 HXD Y 4U1705-44 257.2319 -44.0961 343.32770356 -2.34122442 265.637 54348.6112847222 54349.0140509259 402051010 13343.6 15000 13343.6 13343.6 0 13343.6 1 1 0 1 1 0 0 9370.6 9370.6 34791.9 1 PROCESSED 54404.5443865741 54773 54356.2627430556 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021113 We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2 X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS XIS Y 4U1705-44 257.2347 -44.0965 343.32858118 -2.34307771 294.8341 54381.763275463 54382.2015509259 402051020 21971.3 15000 21979.3 21981 0 21971.3 1 1 0 1 1 0 0 15688 15688 37856 1 PROCESSED 54402.6262847222 54770 54402.6586226852 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021113 We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2 X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS XIS Y 4U1705-44 257.2244 -44.1021 343.31966899 -2.34047423 86.9924 54516.9847569444 54517.6182175926 402051030 25995.6 15000 26051.6 25995.6 0 26051.6 2 2 0 2 1 0 0 20820.5 20820.5 54723.9 1 PROCESSED 54535.186875 54901 54535.2030439815 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021113 We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2 X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS XIS Y 4U1705-44 257.2229 -44.1035 343.31790137 -2.34044351 107.4157 54543.8610532407 54544.5210532407 402051040 20074.4 15000 20074.4 20074.4 0 20082.4 2 1 0 2 1 0 0 13411.3 13411.3 57017.9 1 PROCESSED 54553.1792708333 54922 54553.1912268518 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021113 We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2 X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS XIS Y AQL X-1 287.816 0.5784 35.71219982 -4.14539755 284.0925 54371.6493402778 54372.062662037 402053010 13825.2 15000 13825.2 13825.2 0 13825.2 2 1 0 2 1 0 0 13745 13745 35704 0 PROCESSED 54402.3403009259 54769 54402.3541550926 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y AQL X-1 287.8179 0.5789 35.71351779 -4.14685757 277.9777 54376.9927777778 54377.3516087963 402053020 15132.6 15000 15140.6 15142.3 0 15132.6 1 1 0 1 1 0 0 11890.8 11890.8 30999.9 1 PROCESSED 54403.9097800926 54771 54403.9157175926 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y AQL X-1 287.8182 0.5791 35.71383379 -4.14703266 264.9589 54382.2112384259 54382.6877893518 402053030 19711.7 15000 19719.7 19727.7 0 19711.7 2 2 0 2 1 0 0 17552.2 17552.2 41162 0 PROCESSED 54402.5631944444 54770 54402.5719328704 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y AQL X-1 287.8171 0.5794 35.71359616 -4.14591745 272.6027 54388.3395833333 54388.7225 402053040 17915.7 15000 17915.7 17915.7 0 17915.7 2 2 0 2 1 0 0 17668.2 17668.2 33080 0 PROCESSED 54402.3989814815 54769 54402.4060648148 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y AQL X-1 287.8181 0.5776 35.7124509 -4.14763067 265.5384 54392.3838310185 54392.7918287037 402053050 17889.9 15000 17889.9 17889.9 0 17889.9 1 1 0 1 1 0 0 16927.8 16927.8 35231.9 1 PROCESSED 54402.4102083333 54769 54402.4178935185 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y AQL X-1 287.8172 0.5775 35.71194856 -4.14687642 265.833 54397.9824074074 54398.5072222222 402053060 21364.8 15000 21460.8 21460.8 0 21364.8 2 2 0 2 1 0 0 21402.2 21402.2 45343.9 0 PROCESSED 54407.3665856482 54776 54407.3747222222 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y AQL X-1 287.8217 0.5796 35.71588636 -4.14991498 243.6715 54403.2743171296 54403.66 402053070 17536.2 15000 17584.2 17604 0 17536.2 1 1 0 1 1 0 0 14332.2 14332.2 33319.9 0 PROCESSED 54409.1263310185 54776 54409.1320138889 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021114 We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. GALACTIC POINT SOURCES 4 A REMILLARD RONALD NULL NULL USA 2 AO2-TOO X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS XIS Y 2S 0921-630 140.6632 -63.3 281.84517925 -9.33739383 20.5636 54340.7614351852 54341.8335532407 402057010 43213.1 40000 43213.1 43221.1 0 43221.1 2 2 0 2 1 0 0 15856.8 15856.8 92615.8 0 PROCESSED 54404.5875231482 54721 54353.4365625 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021118 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL USA 2 AO2 PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 XIS Y 2S 0921-630 140.6643 -63.2995 281.84516955 -9.33669084 18.1705 54342.4079166667 54343.5134722222 402058010 45693.7 40000 45693.7 45693.7 0 45693.7 2 2 0 2 1 0 0 43346.3 43346.3 95499.8 2 PROCESSED 54404.5950578704 54724 54356.2760763889 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021118 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL USA 2 AO2 PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 XIS Y 2S 0921-630 140.6655 -63.298 281.84446964 -9.33525426 8.3442 54335.887025463 54336.9932175926 402059010 43131 40000 43131 43131 0 43131 2 2 0 2 1 0 0 37162.2 37162.2 95559.8 0 PROCESSED 54404.6173263889 54721 54350.5504861111 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021118 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL USA 2 AO2 PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 XIS Y 2S 0921-630 140.666 -63.2982 281.84477381 -9.33523447 8.344 54338.0511226852 54339.16 402060010 40342.3 40000 40350.3 40342.3 0 40350.3 1 1 0 1 1 0 0 35646.4 35646.4 95799.9 2 PROCESSED 54404.6289814815 54721 54350.5629398148 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021118 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. GALACTIC POINT SOURCES 4 A COTTAM JEAN NULL NULL USA 2 AO2 PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 XIS Y IGR J17544-2619 268.6038 -26.3314 3.23518966 -0.33446224 84.5765 54544.5263425926 54547.2640509259 402061010 103417.3 72000 103811.5 103827.5 0 103417.3 2 2 0 2 1 0 0 65565.6 65565.6 236505.9 3 PROCESSED 54566.5757175926 54933 54566.6106134259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021121 Supergiant Fast X-ray Transients are a newly-discovered class of x-ray binary with short outbursts and late O to early B supergiant companions. They are not persistently bright, but the nature of their low-level variability is not well known. Similarly short outbursts are also seen in bright HMXBs with supergiant companions such as Cyg X-1 and Vel X-1. The mechanism of these outbursts is unknown in all cases. We propose long pointings to the two best-studied SFXTs and a third object, XTE J1743-363, which seems to be transitional between SFXTs and persistent supergiant HMXBs. We will characterize their variability at low flux levels, both to understand the accretion mechanism and to enable surveys of archival data for new SFXTs. GALACTIC POINT SOURCES 4 C SMITH DAVID NULL NULL USA 2 AO2 CHARACTERIZING THE SPECTRUM AND VARIABILITY OF THE SUPERGIANT FAST X-RAY TRANSIENTS XIS Y IGR J00370+6122 9.2836 61.3722 121.21895683 -1.4519667 87.6081 54273.499849537 54274.230775463 402064010 34908.9 30000 35384.4 35400.4 0 34908.9 2 2 0 2 1 0 0 33804.6 33804.6 63141.9 2 PROCESSED 54322.4609259259 54695 54322.4714236111 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021122 We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 2 AO2 LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS XIS Y IGR J16207-5129 245.1895 -51.5038 332.45599844 -1.05021687 88.1855 54499.8231365741 54500.7841898148 402065010 0 0 0 0 0 0 0 0 0 0 1 0 0 49595.5 49595.5 83031.9 1 PROCESSED 54515.4883333333 54883 54515.6347800926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021122 We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 2 AO2 LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS XIS Y IGR J16207-5129 245.1891 -51.5041 332.45561032 -1.05025433 89.5006 54526.8661111111 54527.7502199074 402065020 32612.7 30000 32709.5 32713.3 0 32612.7 2 2 0 2 1 0 0 28331.2 28331.2 76375.9 0 PROCESSED 54535.197974537 54901 54535.208599537 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021122 We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 2 AO2 LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS XIS Y IGR J17391-3021 264.795 -30.3419 358.06793122 0.44854091 89.216 54518.4950115741 54519.3961226852 402066010 36465.7 30000 36545.7 36593.7 0 36465.7 2 2 0 2 1 0 0 31259.1 31259.1 77819.8 1 PROCESSED 54525.4924537037 54892 54525.5064699074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021122 We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 2 AO2 LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS XIS Y 4U 1907+09 287.4001 9.8965 43.79892996 0.51344636 85.3836 54209.4191666667 54211.2612731482 402067010 80628.3 65000 80628.3 80636.3 0 80636.3 2 2 0 2 1 0 0 73268.5 73268.5 159147.9 2 PROCESSED 54329.3797685185 54702 54216.2674189815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021123 The HMXB 4U 1907+09 shows a rich phenomenology: two cyclotron lines, an uncommonly weak iron line, intermittent X-ray fading, and a recent torque reversal. Compared to other persistent supergiant X-ray pulsars it has been less well observed, although it is a prime target to study the interaction of the neutron star's X-rays with the stellar wind and the accretion column. The latter has been confirmed by our 60ks AO1 observation which allowed for the first detection of a soft excess below 2keV as well as the determination of the paramters of the fundamental cyclotron line with unprecedented accuracy. Due to an unusually low source state during the AO1 exposure, however, an additional observation of 65ks is needed to perform the first phase resolved analysis of this interesting source. GALACTIC POINT SOURCES 4 B POTTSCHMIDT KATJA NULL NULL USA 2 AO2 THE BROAD BAND SPECTRUM OF 4U 1907+09 HXD N EXO 2030+375 308.0118 37.6951 77.17399477 -1.17458429 56.3502 54234.8591666667 54236.1565277778 402068010 57607.1 40000 57607.1 57607.1 0 57607.1 2 2 0 2 1 0 0 53395.4 53395.4 112067.8 2 PROCESSED 54328.8249768518 54702 54242.497962963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021124 We propose a 40 ks Suzaku observation to confirm EXO 2030+375's recently discovered ~10 keV cyclotron feature and constrain its second harmonic at ~20 keV. EXO 2030+375 is a 42-second Be/X-ray pulsar in an eccentric 46-day orbit. If confirmed the ~10 keV cyclotron feature will be the lowest in energy known for an accreting pulsar and will provide the missing piece to make EXO 2030+375 an ideal candidate to observationally test accretion theory. In addition, we will measure EXO 2030+375's spin frequency, study its pulse shape versus energy, and perform phase resolved spectroscopy. Suzaku will allow these studies to reach lower energies and provide high quality spectra at lower luminosities than in any previous observations. GALACTIC POINT SOURCES 4 A WILSON COLLEEN NULL NULL USA 2 AO2 CONSTRAINING CYCLOTRON FEATURES IN A NORMAL OUTBURST OF EXO 2030+375 HXD Y 4U2206+54 331.9811 54.5897 100.6432606 -1.04691755 90.2357 54236.1620949074 54237.812662037 402069010 103976.8 100000 103984.8 103990.6 0 103976.8 3 3 0 3 1 0 0 99784.2 99784.2 142581.9 1 PROCESSED 54327.6385300926 54695 54242.76625 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021125 4U 2206+54 is a high mass X-ray binary which is suspected to contain a neutron star accreting from the wind of its companion BD +53 2790. However, there has been no confirmed detection of X-ray pulsations, and while several authors have reported hints of a cyclotron line in the energy spectra near 30 keV, none have reported significant detections. We propose Suzaku observations to search for long-period pulsations with the XIS, and possible confirmation of the cyclotron line using HXD/PIN. GALACTIC POINT SOURCES 4 A FINGER MARK NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF THE PECULIAR HMXB 4U 2206+54 HXD Y CIRCINUS X-1 230.1633 -57.1695 322.11384942 0.03740334 115.206 54530.1953240741 54531.5523032407 402070010 46411.3 43000 46411.3 46411.3 0 46411.3 2 2 0 2 1 0 0 41821.3 41821.3 117196 0 PROCESSED 54550.2286226852 54916 54550.2459953704 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021128 We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source. GALACTIC POINT SOURCES 4 A LEE JULIA NULL NULL USA 2 AO2 CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHT XIS Y GRS 1915+105 288.7933 10.9535 45.37037141 -0.21130356 67.354 54227.6113657407 54229.0717476852 402071010 65656.8 37000 65656.8 65803.9 0 65672.8 1 2 0 1 1 0 0 56897.3 56897.3 126168 1 PROCESSED 54331.8102083333 54702 54235.5321759259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021132 We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme. GALACTIC POINT SOURCES 4 A MILLER JON NULL NULL USA 2 AO2-TOO THE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105 XIS Y CYG X-1 299.5792 35.2719 71.39034122 3.11120593 84.3565 54220.8163657407 54221.783587963 402072010 45320.4 30000 45320.4 45328.4 0 45320.4 2 1 0 2 1 0 0 40187.3 40187.3 83566 2 PROCESSED 54405.9677430556 54773 54228.1718518518 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021133 We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 A NOWAK MICHAEL NULL NULL USA 2 AO2 CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA HXD Y CYG X-1 299.5451 35.2618 71.3671857 3.12971485 59.9371 54237.8204050926 54238.6480787037 402072020 33356.8 30000 33356.8 33364.9 0 33356.8 2 1 0 2 1 0 0 32563.7 32563.7 71503.9 1 PROCESSED 54324.0259143518 54695 54245.0149884259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021133 We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 A NOWAK MICHAEL NULL NULL USA 2 AO2 CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA HXD Y SWIFT J1753.5-0127 268.3714 -1.4588 24.89300861 12.1795145 261.3846 54362.8585185185 54365.4377777778 402088010 94600.5 93000 94608.5 94616.5 0 94600.5 2 2 0 2 1 0 0 81739 81739 222836 3 PROCESSED 54404.7412268518 54743 54371.6366319444 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021147 While the spectrally hard state represents the most common mode of accretion in black hole X-ray binaries, the nature of its accretion flow is poorly understood. We recently discovered cool accretion disks extending close to the innermost stable circular orbit in the hard states of two black hole transients. Such disks could give rise to strong reflection features, but instead these are weak or not detected. We propose a 70 ks Suzaku observation of Swift J1753.5-0127 (one of the two transients), which is currently in a prolonged hard state. Our goal is to put tight constraints on the strength of the reflection features and increase our understanding of the geometry of the spectrally hard component. Understanding accretion onto compact objects is fundamental to NASA's "SEU" theme. GALACTIC POINT SOURCES 4 A HOMAN JEROEN NULL NULL USA 2 AO2 CONSTRAINING REFLECTION FEATURES IN THE HARD STATE OF BLACK HOLE X-RAY BINARIES XIS Y TW HYA 165.4619 -34.7081 278.67685486 22.95004903 99.3673 54429.0615625 54429.6946064815 402089020 20009.6 11000 20009.6 20017.6 0 20025.6 1 1 0 1 1 0 0 17550 17550 54687.9 2 PROCESSED 54434.1323611111 54804 54434.1387268518 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022007 We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. GALACTIC POINT SOURCES 4 B SCHMITT JURGEN NULL NULL EUR 2 AO2 ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS XIS Y SU AUR 73.9934 30.5715 172.51103259 -7.93275707 85.9197 54339.1713541667 54340.7502199074 402090010 57303.4 55000 57311.4 57303.4 0 57311.4 2 2 0 2 1 0 0 54384.8 54384.8 136401.8 1 PROCESSED 54404.664525463 54723 54350.6381597222 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022007 We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. GALACTIC POINT SOURCES 4 A SCHMITT JURGEN NULL NULL EUR 2 AO2 ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS XIS Y EXO 0748-676 117.1051 -67.7525 279.97237585 -19.82332654 158.0884 54459.2369560185 54460.2919444444 402092010 45898.8 40000 45912.6 45898.8 0 45904.6 2 2 0 2 1 0 0 43574.7 43574.7 91135.8 1 PROCESSED 54483.1704050926 54854 54483.1839351852 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022014 We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity. GALACTIC POINT SOURCES 4 C DIAZ TRIGO MARIA NULL NULL EUR 2 AO2 BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS XIS Y SGR 1806-20 272.1687 -20.4711 9.94559743 -0.27498509 268.1397 54387.2332060185 54388.333599537 402094010 52247.7 50000 52247.7 52271.7 0 52263.7 2 2 0 2 1 0 0 50089.5 50089.5 95059.9 1 PROCESSED 54403.9442361111 54771 54403.9548611111 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022016 Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts. GALACTIC POINT SOURCES 4 C MEREGHETTI SANDRO NULL NULL EUR 2 AO2 CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTON HXD Y GT MUS 174.8799 -65.348 295.52044001 -3.51633969 94.8564 54446.4736689815 54449.187662037 402095010 93308.7 80000 93308.7 93308.7 0 93308.7 2 2 0 2 1 0 0 94696.5 94696.5 234469.9 3 PROCESSED 54460.7354976852 54828 54460.7707060185 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022020 We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku. GALACTIC POINT SOURCES 4 B MAGGIO ANTONIO NULL NULL EUR 2 AO2 BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCE HXD Y HD161103 266.1888 -27.2272 1.35850162 1.05434609 105.2351 54884.7946643518 54886.7057175926 403001010 71524.9 60000 71532.9 71524.9 0 71540.9 2 2 0 2 1 0 0 59664.7 59664.7 165085.8 1 PROCESSED 54962.5615625 55330 54903.6732523148 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030005 We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN. GALACTIC POINT SOURCES 4 B MIURA JUNICHIRO NULL NULL JAP 3 AO3 SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES XIS Y HD110432 190.599 -63.0744 301.908501 -0.22062002 344.9423 54718.9065740741 54719.7050231482 403002010 25333.2 25000 25333.2 25333.2 0 25333.2 2 2 0 2 1 0 0 21343.6 21343.6 68977.9 0 PROCESSED 54777.5247337963 55148 54780.4451736111 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030005 We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN. GALACTIC POINT SOURCES 4 B MIURA JUNICHIRO NULL NULL JAP 3 AO3 SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES HXD Y 1RXS J070407.9+26250 106.0316 26.4199 190.26714041 14.29962915 96.1437 54749.1266319444 54750.3682175926 403003010 53551.9 50000 53551.9 53551.9 0 53551.9 2 2 0 2 1 0 0 41140.5 41140.5 107231.9 0 PROCESSED 54780.5096064815 55148 54780.5445949074 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030009 Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically. GALACTIC POINT SOURCES 4 B ISHIDA MANABU NULL NULL JAP 3 AO3 OBSERVATIONS OF SOFT INTERMEDIATE POLARS XIS Y 1RXS J062518.2+73343 96.3307 73.5671 140.86801575 24.12512545 262.0383 54570.0388310185 54571.1252777778 403004010 50326.7 50000 50326.7 50326.7 0 50326.7 2 2 0 2 1 0 0 50125.3 50125.3 93848.8 0 PROCESSED 54581.21875 54953 54581.2328472222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030009 Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically. GALACTIC POINT SOURCES 4 B ISHIDA MANABU NULL NULL JAP 3 AO3 OBSERVATIONS OF SOFT INTERMEDIATE POLARS XIS Y 1E 1048.1-5937 162.5452 -59.8394 288.24102095 -0.47209541 101.4368 54800.9597337963 54802.5927083333 403005010 100423.1 100000 100443 100423.1 0 100423.1 2 2 0 2 1 0 0 68104.9 68104.9 141081.9 0 PROCESSED 54812.030462963 55178 54812.0471875 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030013 Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs. GALACTIC POINT SOURCES 4 C TAKATA JUMPEI NULL NULL JAP 3 AO3 X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU HXD Y MARS-P1 102.8773 25.1625 190.24974394 11.19384085 298.0037 54559.3414814815 54559.4099421296 403006010 2904.8 100000 2904.8 2912.8 0 2912.8 1 1 0 1 1 0 0 2909.6 2909.6 5911.9 0 PROCESSED 54577.0394791667 54953 54577.0446875 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P2 102.9198 25.1641 190.26475308 11.2294146 298.0203 54559.4100925926 54559.493275463 403006020 4854.6 100000 4854.6 4886.6 0 4870.6 1 1 0 1 1 0 0 3612.1 3612.1 7183.9 0 PROCESSED 54577.0255208333 54953 54577.0304976852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P3 102.9612 25.1565 190.28784034 11.26022306 298.032 54559.4933796296 54559.5766087963 403006030 3886 100000 3886 3910 0 3894 1 1 0 1 1 0 0 3113.4 3113.4 7183.9 0 PROCESSED 54577.0439236111 54953 54577.0484259259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P4 103.0016 25.1536 190.30618657 11.29219101 298.0476 54559.5767592593 54559.6599421296 403006040 2288.2 100000 2288.2 2288.2 0 2288.2 1 1 0 1 1 0 0 2010 2010 7183.9 0 PROCESSED 54577.0485648148 54953 54577.0528935185 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P5 103.045 25.1496 190.32670814 11.32616716 298.0638 54559.6600462963 54559.7432407407 403006050 1956.2 100000 1956.2 1956.2 0 1956.2 2 2 0 2 1 0 0 1992.6 1992.6 7167.9 0 PROCESSED 54577.128599537 54953 54577.1345486111 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P6 103.0844 25.143 190.34808199 11.3557719 298.0743 54559.7434375 54559.8265972222 403006060 1939 100000 1939 1939 0 1939 1 1 0 1 1 0 0 1804.6 1804.6 7181.9 0 PROCESSED 54577.1330208333 54953 54577.1376388889 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P7 103.127 25.1401 190.36726484 11.38956433 298.0907 54559.8267476852 54559.9029861111 403006070 2502.8 100000 2513.9 2510.8 0 2502.8 1 1 0 1 1 0 0 1650.6 1650.6 6584 0 PROCESSED 54577.1437731482 54953 54577.1486342593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P8 103.1682 25.1356 190.38738197 11.42154102 298.1062 54559.9031365741 54560.0072222222 403006080 2748.9 100000 2753.8 2757.8 0 2748.9 2 2 0 2 1 0 0 2286.4 2286.4 8984 0 PROCESSED 54577.1581712963 54953 54577.1637615741 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P9 103.2195 25.1275 190.41473742 11.46031922 298.1247 54560.0073726852 54560.0766666667 403006090 2150.6 100000 2150.6 2174.6 0 2150.6 1 1 0 1 1 0 0 1891.9 1891.9 5975.9 0 PROCESSED 54577.1380439815 54953 54577.1428009259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P10 103.2518 25.125 190.42954859 11.48582895 298.135 54560.0767708333 54560.16 403006100 3771.6 100000 3795.6 3771.6 0 3796 1 1 0 1 1 0 0 4001.4 4001.4 7183.9 0 PROCESSED 54577.1489814815 54953 54577.1537847222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P11 103.2936 25.1207 190.44969799 11.5184009 298.1493 54560.1601041667 54560.2433333333 403006110 4619.8 100000 4627.8 4619.8 0 4635.8 1 1 0 1 1 0 0 4074.9 4074.9 7183.9 0 PROCESSED 54577.1689930556 54953 54577.1745023148 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P12 103.3358 25.1148 190.47148034 11.55063865 298.1645 54560.2434837963 54560.3266666667 403006120 3455 100000 3455 3455 0 3455 1 1 0 1 1 0 0 2678 2678 7175.9 0 PROCESSED 54577.1742939815 54953 54577.1789467593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P13 103.3779 25.1101 190.49210676 11.58330245 298.1799 54560.3267708333 54560.41 403006130 4251.8 100000 4267.8 4251.8 0 4267.8 1 1 0 1 1 0 0 3529 3529 7183.9 0 PROCESSED 54577.924525463 54953 54577.9292939815 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P14 103.4188 25.1057 190.5119865 11.61511049 298.1941 54560.410150463 54560.4933333333 403006140 4825.2 100000 4849.2 4825.2 0 4857.2 1 1 0 1 1 0 0 3721.4 3721.4 7175.9 0 PROCESSED 54577.9381712963 54953 54577.9434722222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P15 103.4611 25.1019 190.53184536 11.64832678 298.2083 54560.4934375 54560.5766666667 403006150 3831 100000 3839 3831 0 3847 1 1 0 1 1 0 0 3192.8 3192.8 7183.9 1 PROCESSED 54577.9287268518 54953 54580.5809837963 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P16 103.503 25.0968 190.55275085 11.68067717 298.2223 54560.5768171296 54560.66 403006160 2326.2 100000 2326.2 2326.2 0 2326.2 2 2 0 2 1 0 0 2134 2134 7179.9 0 PROCESSED 54577.9426851852 54953 54577.9478935185 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P17 103.5439 25.0908 190.5741012 11.71183533 298.237 54560.6601041667 54560.743287037 403006170 1978.2 100000 1978.2 1978.2 0 1978.2 1 1 0 1 1 0 0 1959.6 1959.6 7182 0 PROCESSED 54578.0356481482 54953 54578.0406597222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P18 103.5869 25.0943 190.58743765 11.74868918 298.2592 54560.7434837963 54560.8264351852 403006180 1861.8 100000 1861.8 1861.8 0 1861.8 1 1 0 1 1 0 0 1939.6 1939.6 7153.9 0 PROCESSED 54578.0477893518 54953 54578.0530555556 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P19 103.6272 25.0809 190.61541806 11.77628093 298.2673 54560.8266319444 54560.9098842593 403006190 2839.8 100000 2839.8 2848.2 0 2843.8 2 2 0 2 1 0 0 1844.1 1844.1 7190 0 PROCESSED 54578.0419791667 54953 54578.0465625 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P20 103.6685 25.0732 190.63848879 11.80707935 298.2779 54560.9100347222 54560.9932175926 403006200 1849 100000 1849 1849 0 1849 1 1 0 1 1 0 0 1222 1222 7183.9 0 PROCESSED 54578.0525115741 54953 54578.0575231482 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P21 103.7101 25.0688 190.65860601 11.8395058 298.2947 54560.9933217593 54561.0765509259 403006210 2880.8 100000 2880.8 2880.8 0 2880.8 1 1 0 1 1 0 0 3451.6 3451.6 7183.9 0 PROCESSED 54578.0568634259 54953 54578.0612847222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P22 103.7541 25.0677 190.67657625 11.87528798 298.3117 54561.0767013889 54561.1598842593 403006220 4024.6 100000 4040.6 4024.6 0 4047.6 1 1 0 1 1 0 0 4102 4102 7183.9 0 PROCESSED 54578.0618402778 54953 54578.0665625 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P23 103.7955 25.0599 190.69976585 11.90614711 298.325 54561.1600347222 54561.2432175926 403006230 4518.8 100000 4526.8 4518.8 0 4534.8 1 1 0 1 1 0 0 3686.8 3686.8 7183.9 0 PROCESSED 54578.1137384259 54953 54578.1176157407 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P24 103.8389 25.0556 190.72046804 11.94011608 298.3401 54561.2433680556 54561.3265509259 403006240 3423 100000 3423 3423 0 3423 1 1 0 1 1 0 0 2511 2511 7183.9 0 PROCESSED 54578.1186226852 54953 54578.1234375 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P25 103.8803 25.0503 190.74132534 11.97202775 298.3546 54561.3266550926 54561.4098842593 403006250 4261.2 100000 4269.2 4261.2 0 4269.2 1 1 0 1 1 0 0 3251.1 3251.1 7183.9 0 PROCESSED 54578.1278819444 54953 54578.1323032407 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P26 103.921 25.0474 190.75967691 12.00436516 298.3671 54561.4100347222 54561.4932175926 403006260 4797.6 100000 4813.6 4797.6 0 4821.6 1 1 0 1 1 0 0 3762.2 3762.2 7183.9 0 PROCESSED 54578.132650463 54953 54578.1374074074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y MARS-P27 103.964 25.0399 190.78318678 12.0366945 298.3836 54561.4933217593 54561.5418171296 403006270 1099.8 100000 1107.8 1099.8 0 1115.8 1 1 0 1 1 0 0 1093.5 1093.5 4183.9 0 PROCESSED 54578.1206134259 54953 54578.1251273148 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A EZOE YUICHIRO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y AM HERCULES 274.126 49.8084 77.81082077 25.81903319 234.8814 54768.8590162037 54771.3043287037 403007010 108496.5 100000 108504.5 108504.5 0 108496.5 2 2 0 2 1 0 0 94467.1 94467.1 211257.7 3 PROCESSED 54788.3710532407 55156 54788.4722222222 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030021 We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object. GALACTIC POINT SOURCES 4 C TERADA YUKIKATSU NULL NULL JAP 3 AO3 NON THERMAL EMISSION FROM THE POLAR AM HERCULES HXD Y AM HERCULES BGD 282.0964 47.9785 77.40285415 20.2844947 234.9986 54771.3072106482 54772.3438310185 403008010 44360.1 40000 44368.1 44360.1 0 44392.1 2 2 0 2 1 0 0 40411.5 40411.5 89551.9 1 PROCESSED 54788.1131018518 55154 54788.4288541667 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030021 We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object. GALACTIC POINT SOURCES 4 C TERADA YUKIKATSU NULL NULL JAP 3 AO3 NON THERMAL EMISSION FROM THE POLAR AM HERCULES XIS Y ARCHES CLUSTER 266.4808 -28.778 0.16960578 0.02569084 109.9998 54911.0857407407 54913.7681712963 403009010 110793.3 100000 110793.3 110793.3 0 110793.3 2 2 0 2 1 0 0 91657.8 91657.8 231741.7 3 PROCESSED 54962.9976388889 55330 54924.3822106482 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030029 We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring. GALACTIC POINT SOURCES 4 B TSUJIMOTO MASAHIRO NULL NULL JAP 3 AO3 A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER XIS Y GX 339-4 255.6944 -48.7333 338.97952784 -4.28620483 84.7264 54908.0786226852 54908.9613310185 403011010 43040.8 40000 43055.4 43040.8 0 43061.4 1 1 0 1 1 0 0 35391.4 35391.4 76257.9 1 PROCESSED 54962.5393865741 55330 54917.4333796296 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030046 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD Y GX 339-4 255.7293 -48.7348 338.99236079 -4.30539701 107.9544 54915.3430555556 54916.2711111111 403011020 39079.2 40000 39116.5 39079.2 0 39116.5 1 1 0 1 1 0 0 34785.2 34785.2 80165.8 0 PROCESSED 54963.1574537037 55330 54930.1609490741 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030046 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD Y GX 339-4 255.7297 -48.7352 338.99220289 -4.30584956 108.3513 54920.4773958333 54921.5216435185 403011030 39638.4 40000 39663.3 39638.4 0 39663.3 2 2 0 2 1 0 0 35068.6 35068.6 90186 0 PROCESSED 54962.832349537 55330 54931.0610416667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030046 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD Y LS I+61 303_1 40.1455 61.188 135.69810374 1.0510579 270.0003 54853.9515856482 54854.8648032407 403015010 40551.4 40000 40551.4 40551.4 0 40551.4 2 2 0 2 1 0 0 25731.2 25731.2 78868 0 PROCESSED 54959.5385185185 55329 54880.5343865741 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A FUKAZAWA YASUSHI NULL NULL JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y LS I+61 303_2 40.1457 61.1877 135.69831419 1.05082335 270.0006 54856.6966087963 54858.1766666667 403016010 61066.7 60000 61078.4 61066.7 0 61078.4 2 2 0 2 1 0 0 26659.1 26659.1 127839.8 1 PROCESSED 54962.0981481482 55329 54880.5522106482 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A FUKAZAWA YASUSHI NULL NULL JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y LS I+61 303_3 40.2018 61.1949 135.72005286 1.06843757 246.2753 54872.1842592593 54873.7252199074 403017010 68627.3 60000 68627.3 68627.3 0 68627.3 2 2 0 2 1 0 0 65068.5 65068.5 133121.8 1 PROCESSED 54962.3298958333 55330 54893.4210300926 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A FUKAZAWA YASUSHI NULL NULL JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y HESS J0632+057 98.2456 5.8062 205.66072349 -1.43796588 289.8173 54579.6856828704 54580.6877199074 403018010 44076 40000 44076 44076 0 44076 2 2 0 2 1 0 0 41475.8 41475.8 86565.8 0 PROCESSED 54594.1453472222 54961 54594.1596990741 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030080 We propose a 40 ks observation on HESS J0632+057, the newly discovered TeV gamma-ray source in the interacting region of Monoceros SNR and Rosette Nebula. Although this point-like source is found inside the error circle of an unidentified EGRET source 3EG J0634+0521, it has no clear counterpart at other wavelengths. Two sources, a weak X-ray source 1RXS J063258.3+05487 and a Be-star MCW 148, are found inside the error circle of HESS. The aim of the Suzaku observation is to obtain a clue to solve the yet feasible three scenarios of the TeV gamma-ray source. GALACTIC POINT SOURCES 4 A KOKUBUN MOTOHIDE NULL NULL JAP 3 AO3 INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGION XIS Y LMC X -3 84.7048 -64.0785 273.57060216 -32.09537201 185.5067 54822.3015856482 54823.8675694444 403020010 73973.8 60000 73973.8 73981.8 0 73987.5 2 2 0 2 1 0 0 70050.5 70050.5 135283.8 1 PROCESSED 54840.1787615741 55206 54840.5013310185 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030102 Ionized iron K absorption lines are commonly observed from high state black hole binaries. Thus the highly ionized plasma are thought to be generally associated with optically thick accretion disks. Huge outflow by the plasma has been confirmed by some of these objects, and thus such plasma is thought to have an important role on accretion flow. In order to establish generality of the plasma by detecting the absorption lines, and to distinguish whether creation mechanism of the plasma is determined by X-ray luminosity or there is another key parameter, we propose Suzaku observation of luminous persistent black hole binary LMC X-3, with exposure of 60ks. This observation will enable us to find critical parameters which determine the creation of the accretion disk wind. GALACTIC POINT SOURCES 4 C KUBOTA AYA NULL NULL JAP 3 AO3 SEARCH FOR IRON K ABSORPTION LINES FROM LMC X-3 XIS Y RX J1712.6-2414 258.1492 -24.2444 359.8664305 8.74215246 94.4586 54889.4875925926 54892.2710532407 403021010 110481.3 100000 110489.3 110481.3 0 110489.3 2 2 0 2 1 0 0 89458.4 89458.4 240441.8 4 PROCESSED 54963.440462963 55330 54908.5588310185 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030106 We propose to observe a peculiar Intermediate Polar, RX J1712.6-2414, which has no accretion disk around the white dwarf. This source shows the X-ray modulation only at the beat period and broad Fe-K emission lines in the phase-averaged spectrum. Our goal is to obtain a clear picture about the accretion flow geometry, which can explain the timing and spectral properties, utilizing the fine phase-resolved spectra. Furthermore, we examine the non-thermal emission from the source, since the magnetized white dwarf is a promising candidate of particle acceleration sites. GALACTIC POINT SOURCES 4 B MORI HIDEYUKI NULL NULL JAP 3 AO3 ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414 XIS Y YY DRA 175.8686 71.6187 130.35712902 44.51671754 282.0676 54632.7758217593 54633.4098842593 403022010 29185.1 30000 29185.1 29185.1 0 29185.1 2 2 0 2 1 0 0 27474.3 27474.3 54777.9 1 PROCESSED 54644.1413541667 55013 54644.1517592593 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030107 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 C YUASA TAKAYUKI NULL NULL JAP 3 AO3 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y TV COL 82.3326 -32.8641 236.83580562 -30.63495041 295.9146 54573.7555555556 54574.6668634259 403023010 35836.7 40000 35836.7 35836.7 0 35836.7 2 2 0 2 1 0 0 30102.3 30102.3 78729.9 0 PROCESSED 54587.0541666667 54953 54587.0666550926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030107 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 C YUASA TAKAYUKI NULL NULL JAP 3 AO3 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y IGR J16194-2810 244.8908 -28.0663 349.1669856 15.58223604 95.1879 54867.1762152778 54868.4314236111 403024010 45568.7 50000 45568.7 45573.8 0 45568.7 2 2 0 2 1 0 0 38785.9 38785.9 108435.8 1 PROCESSED 54962.2222685185 55329 54880.5743518518 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030121 We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source. GALACTIC POINT SOURCES 4 C NAGAE OSAMU NULL NULL JAP 3 AO3 ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810 HXD Y V709 CAS 7.1951 59.3013 120.03837674 -3.44309479 84.0816 54637.4334837963 54638.1542824074 403025010 35898.2 30000 35898.2 35898.2 0 35898.2 2 2 0 2 1 0 0 33382.3 33382.3 62267.9 0 PROCESSED 54648.0905555556 55014 54648.3358101852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y IGR J17303-0601 262.5864 -5.9814 17.93788623 15.02149808 100.7922 54878.4233217593 54879.3355787037 403026010 32963.5 30000 32963.5 32963.5 0 32963.5 2 2 0 2 1 0 0 27755.9 27755.9 78818 2 PROCESSED 54945.1581712963 55325 54893.4381018518 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y RX J1940.1-1025 295.0445 -10.4193 28.98688715 -15.49869645 79.7405 54572.8979976852 54573.743275463 403027010 32453.6 30000 32453.6 32453.6 0 32453.6 2 2 0 2 1 0 0 26465.7 26465.7 73021.9 2 PROCESSED 54587.0365740741 54953 54587.0481481482 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y IGR J17195-4100 259.8947 -41.0152 346.97641748 -2.13400756 97.0631 54880.4607175926 54881.3106481482 403028010 31645.6 30000 31645.6 31645.6 0 31645.6 2 2 0 2 1 0 0 26917.8 26917.8 73428 0 PROCESSED 54962.3079166667 55330 54895.5494328704 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y XSS J12270-4859 187.002 -48.8936 298.97017898 13.79783482 315.9792 54686.9674421296 54687.6480787037 403029010 29623.2 30000 29623.2 29623.2 0 29623.2 2 2 0 2 1 0 0 34580 34580 58791.9 0 PROCESSED 54707.1640856482 55073 54707.1730208333 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y WR140 305.2159 43.8446 80.96257668 4.11237193 190.1825 54844.5415162037 54846.500162037 403030010 89406.8 80000 89406.8 89406.8 0 89406.8 2 2 0 2 1 0 0 78055.7 78055.7 169196.9 1 PROCESSED 54959.633275463 55328 54861.8550115741 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030157 WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. GALACTIC POINT SOURCES 4 A MAEDA YOSHITOMO NULL NULL JAP 3 AO3 X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 HXD Y WR140 305.211 43.8318 80.94998516 4.10805919 199.7371 54835.3583449074 54836.4252199074 403031010 47266.4 40000 47266.4 47266.4 0 47282.4 2 2 0 2 1 0 0 45303 45303 92161.8 0 PROCESSED 54959.4302662037 55328 54850.2164583333 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030157 WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. GALACTIC POINT SOURCES 4 A MAEDA YOSHITOMO NULL NULL JAP 3 AO3 X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 HXD Y WR140 305.1942 43.809 80.92425741 4.10518752 220.5408 54812.4360069444 54813.5523148148 403032010 52910.6 40000 52910.6 52910.6 0 52910.6 3 3 0 3 1 0 0 48260.9 48260.9 96431.8 0 PROCESSED 54826.234375 55192 54826.2481365741 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030157 WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. GALACTIC POINT SOURCES 4 A MAEDA YOSHITOMO NULL NULL JAP 3 AO3 X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 HXD Y WR140 305.1135 43.9272 80.98919394 4.21991141 90.2945 54565.231400463 54565.7224305556 403033010 21625.3 20000 21625.3 21625.3 0 21625.3 2 2 0 2 1 0 0 18605.5 18605.5 42415.9 2 PROCESSED 54580.4079513889 54953 54580.4185648148 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030157 WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. GALACTIC POINT SOURCES 4 A MAEDA YOSHITOMO NULL NULL JAP 3 AO3 X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 HXD Y TAU SCO 248.9714 -28.2185 351.53328031 12.80600635 277.9748 54710.0436689815 54710.3697222222 403034010 14617.1 10000 14617.1 14617.1 0 14617.1 1 1 0 1 1 0 0 12085.5 12085.5 28135.9 0 PROCESSED 54777.4117476852 55148 54780.4170138889 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y TAU SCO 248.9731 -28.2173 351.53521528 12.80565459 288.7028 54717.0750115741 54717.3752777778 403034020 14521.5 10000 14529.5 14521.5 0 14537.5 1 1 0 1 1 0 0 9652.4 9652.4 25935.9 1 PROCESSED 54777.7685416667 55148 54780.6118171296 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y TAU SCO 248.9736 -28.2151 351.53721955 12.80675658 279.3712 54723.4207291667 54723.8119675926 403034030 12290.2 10000 12298.2 12298.2 0 12290.2 1 1 0 1 1 0 0 11028.2 11028.2 33799.9 0 PROCESSED 54777.7390393518 55148 54780.4631597222 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y TAU SCO 248.9733 -28.218 351.53478934 12.80506422 280.0312 54729.4179398148 54729.7578009259 403034040 13971.1 10000 13971.1 13971.1 0 13971.1 2 2 0 2 1 0 0 12891.2 12891.2 29350 0 PROCESSED 54777.8469328704 55148 54780.4954050926 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y TAU SCO 248.9722 -28.2177 351.53437371 12.80599439 271.5181 54696.3145833333 54696.6675810185 403034050 16313.6 10000 16350.4 16313.6 0 16358.4 1 1 0 1 1 0 0 13967 13967 30472 0 PROCESSED 54713.1859606482 55084 54713.1924189815 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y TAU SCO 248.9729 -28.218 351.53455344 12.80533126 274.2608 54703.1981597222 54703.5447222222 403034060 15018.3 10000 15026.3 15034.3 0 15018.3 1 1 0 1 1 0 0 12904.9 12904.9 29911.9 0 PROCESSED 54713.2685648148 55084 54713.2754976852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031121 We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. GALACTIC POINT SOURCES 4 A IGNACE RICHARD NULL NULL USA 3 AO3 X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO XIS Y ETA CARINAE 161.2297 -59.7314 287.60304523 -0.67930865 294 54627.0775 54627.649525463 403035010 35447.9 30000 35463.9 35447.9 0 35463.9 2 2 0 2 1 0 0 27210.2 27210.2 49415.9 1 PROCESSED 54637.2593518518 55003 54637.2680092593 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A HAMAGUCHI KENJI NULL NULL USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y ETA CARINAE 161.2769 -59.635 287.57915278 -0.58292483 99.9027 54810.21125 54811.2084953704 403036010 48501.6 30000 48501.6 48501.6 0 48501.6 2 2 0 2 1 0 0 42425.9 42425.9 86151.8 2 PROCESSED 54826.1197685185 55198 54828.3640972222 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A HAMAGUCHI KENJI NULL NULL USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y ETA CARINAE 161.3407 -59.6518 287.61551185 -0.58277566 142.0006 54856.1332291667 54856.6821064815 403037010 28805.3 30000 28805.3 28805.3 0 28805.3 1 1 0 1 1 0 0 17453.9 17453.9 47407.9 0 PROCESSED 54961.978599537 55328 54880.533587963 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A HAMAGUCHI KENJI NULL NULL USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y ETA CARINAE 161.3639 -59.6742 287.63630523 -0.59715454 170.6228 54877.528287037 54878.4119675926 403038010 35552.5 30000 35568.5 35552.5 0 35560.5 2 2 0 2 1 0 0 31119.3 31119.3 76323.9 1 PROCESSED 54962.3153240741 55328 54893.4307407407 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031124 X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). GALACTIC POINT SOURCES 4 A HAMAGUCHI KENJI NULL NULL USA 3 AO3 X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM HXD Y ASAS J002511+1217.2 6.2997 12.2847 112.91544003 -50.07604687 234.9156 54841.6813773148 54842.5468055556 403039010 33256 30000 33256 33256 0 33256 2 2 0 2 1 0 0 29873 29873 74752 1 PROCESSED 54959.7324884259 55328 54851.4143055556 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031144 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 3 AO3 BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 XIS Y KT PER 24.2933 50.9468 130.24865907 -11.27406186 260.9001 54843.8957060185 54844.5334953704 403041010 29195.7 20000 29195.7 29195.7 0 29195.7 2 2 0 2 1 0 0 28165.8 28165.8 55089.9 0 PROCESSED 54959.3597337963 55328 54854.0547916667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031144 Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 3 AO3 BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 XIS Y SS73 17 152.7399 -57.7545 282.81739372 -1.29143094 80.1552 54775.6877430556 54776.3072453704 403043010 24907 20000 24907 24907 0 24907 2 2 0 2 1 0 0 20809.1 20809.1 53519.9 0 PROCESSED 54791.5853935185 55157 54791.6362847222 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031145 SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission. GALACTIC POINT SOURCES 4 A SMITH RANDALL NULL NULL USA 3 AO3 SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17 HXD Y GX 301-2 186.5611 -62.8021 300.05773343 -0.07103063 326.712 54703.5522800926 54704.0036689815 403044010 11427.5 60000 11429.2 11430.6 0 11427.5 2 2 0 2 1 0 0 10714.8 10714.8 38993.9 0 PROCESSED 54720.2543981482 55218 54720.435462963 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031152 We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. GALACTIC POINT SOURCES 4 A ROTHSCHILD RICHARD NULL NULL USA 3 AO3 BROAD-BAND STUDY OF GX 301-2 HXD Y GX 301-2 186.689 -62.7212 300.10817936 0.01514837 109.0098 54836.4396296296 54838.0419328704 403044020 61813.6 50000 61813.6 61813.6 0 61813.6 2 2 0 2 1 0 0 54992.2 54992.2 138398.1 2 PROCESSED 54959.4139814815 55328 54851.4303125 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031152 We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. GALACTIC POINT SOURCES 4 A ROTHSCHILD RICHARD NULL NULL USA 3 AO3 BROAD-BAND STUDY OF GX 301-2 HXD Y VELA X-1 135.5377 -40.5514 263.06039339 3.93722667 314.5441 54634.1981134259 54635.9043287037 403045010 104709.6 100000 104723.4 104709.6 0 104715.4 2 2 0 2 1 0 0 96008.9 96008.9 147389.9 1 PROCESSED 54644.4374652778 55010 54644.4687847222 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031153 We propose to observe the well-known X-ray pulsar Vela X-1 (4U0900-40) using Suzaku in order to test models for the circumstellar environment by measuring teh spectrum and searching for variability in the iron line. The line is expected to exhibit changes in intensity and centroid energy as the X-ray beam sweeps around the wind an illuminates material with varying column density, ionization state, and vleocity. In addition we will study the variability in the cyclotron feature. We will compare our observations with detailed hydrodynamical simulations of the stellar wind and its interaction with the compact object. GALACTIC POINT SOURCES 4 A KALLMAN TIMOTHY NULL NULL USA 3 AO3 SPECTROSCOPY OF VELA X-1 (4U0900-40) AND SEARCHES FOR PULSE PHASE VARIABILITY XIS Y CENTAURUS X-3 170.3244 -60.5721 292.07802241 0.38603209 97.3521 54808.2886111111 54810.2085532407 403046010 97587.1 90000 97587.1 97587.1 0 97587.1 2 2 0 2 1 0 0 79656.2 79656.2 165853.7 0 PROCESSED 54822.5966319444 55188 54822.6243634259 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031154 We ask for a 90 ks observation (which will be performed within typically 180 ks taking Suzaku's duty cycle into account) of the accreting HMXB Centaurus X-3 to conduct the most sensitive study to date of the wide range of changes of its broad band spectrum over one 2.1 binary orbit and with pulse phase. Especially we will determine the evolution of the hydrogen absorption column over the orbit and test whether signatures of the tidal wake observed with RXTE can be confirmed. The variable Fe line complex will be studied. The cyclotron resonance scattering feature of Cen X-3 at ~30 keV is especially well suited to test new physical models describing phase-resolved line profiles, since it is very variable over the pulse, with the line centroid spanning an energy range from 28 to 39 keV. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 3 AO3 THE BROAD BAND SPECTRUM OF CEN X-3 OVER ORBIT AND PULSE PHASE HXD Y 1A1118-61 170.3073 -61.878 292.515895 -0.84430143 131.7127 54846.5144328704 54847.9029976852 403049010 49667.4 45000 49667.4 49667.4 0 49667.4 2 2 0 2 1 0 0 46815.9 46815.9 119953.8 0 PROCESSED 54959.5419560185 55328 54858.6603125 2.3.12.25 4 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031155 We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 3 AO3-TOO SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD Y 1A1118-61 170.3215 -61.8847 292.5244731 -0.84831529 142.606 54859.2344328704 54859.8925810185 403050010 44212.5 45000 44212.5 44212.5 0 44212.5 2 2 0 2 1 0 0 30915.4 30915.4 56859.9 0 PROCESSED 54962.0592708333 55328 54880.5326273148 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031155 We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 3 AO3-TOO SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD Y CEN X-4 224.5893 -31.6684 332.24097668 23.88258751 104.6233 54847.9102314815 54850.9717939815 403057010 146670.4 150000 146687.6 146670.4 0 146691.6 2 2 0 2 1 0 0 133618.5 133618.5 264453.9 2 PROCESSED 54959.9293518518 55328 54880.5460069444 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031161 Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL USA 3 AO3 UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4 XIS Y GX 340+0 251.4463 -45.6133 339.58535361 -0.07953483 81.21 54892.2765740741 54894.8168287037 403060010 107312.7 100000 107314.5 107312.7 0 107314.5 2 2 0 2 1 0 0 86104 86104 219446.7 1 PROCESSED 54963.2715162037 55329 54908.7293055556 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031164 In this proposal we request to observe accreting neutron stars sources GX 340+0, GX 3+1 and GX 13+1. The observational goal of the observations is to collect high-spectral resolution data in the region of K$_alpha$ iron line. Our scientific motivation is to put the origin of the line emission under additional theoretical scrutiny. We wish to compare the performance of the wind-reprocessing model to relativistic model in as many sources as possible. This proposal is a part of our broader effort to investigate the origin of iron emission line in Galactic X-ray binaries, which includes a parallel proposal to observe WD binaries. GALACTIC POINT SOURCES 4 B SHAPOSHNIKOV NIKOLAI NULL NULL USA 3 AO3 IRON KALPHA EMISSION LINE DIAGNOSTICS IN ACCRETING NEUTRON STARS XIS Y CYG X-2 326.1609 38.3293 87.3271497 -11.30495752 51.1203 54648.0669097222 54650.6154398148 403063010 72430.8 100000 102692.2 72430.8 0 89814.4 1 1 0 2 1 0 0 88133.1 88133.1 220167.8 0 PROCESSED 54664.8983101852 55031 54665.3170601852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031165 The nature of ultra-dense matter in neutron stars remains enigmatic. To probe this requires accurate neutron star radii and masses. We recently showed that broad iron lines in neutron star low-mass X-ray binaries (LMXBs) constrain the neutron star radius. LMXBs also provide us with another tool, kHz quasi-periodic oscillations (QPOs). Combining the inner disk velocity (from modeling the iron line) and the frequency of the kHz QPOs gives a method to measure the neutron star mass. We propose a 100 ks observation of Cyg X-2 with Suzaku to provide a detailed iron line profile. Combined with simultaneous observations with RXTE to determine the kHz QPO frequency, we will measure the neutron star mass. Cyg X-2 is the perfect test case as it already has a known mass from optical observations. GALACTIC POINT SOURCES 4 B CACKETT EDWARD NULL NULL USA 3 AO3 MEASURING NEUTRON STAR MASSES USING BROAD IRON LINES AND KHZ QPOS XIS Y CYG X-1 299.5797 35.2714 71.39012673 3.11059703 84.4565 54574.6816898148 54575.4238425926 403065010 33943.5 30000 33943.5 33978.2 0 33970.3 1 1 0 2 1 0 0 28955.6 28955.6 64118 0 PROCESSED 54587.1935416667 54957 54587.2117476852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031172 We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 A NOWAK MICHAEL NULL NULL USA 3 AO3 CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERA HXD Y GX 339-4 255.7095 -48.7885 338.94163546 -4.32765826 281.8009 54733.942650463 54736.0968055556 403067010 104994 100000 105018 104994 0 104994 2 2 0 2 1 0 0 114775.9 114775.9 186091.7 2 PROCESSED 54777.5706018518 55148 54780.5803935185 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031174 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with our multi-wavelength, radio to X-ray, program, Suzaku observations can constrain theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 3 AO3-TOO CONSTRAINING MODELS FOR BLACK HOLE ACCRETION IN THE HARD STATE XIS Y XTE J1759-220 269.9393 -22.0118 7.5831003 0.77858469 86.479 54566.5188773148 54567.6460532407 403072010 48961 50000 49361 49425 0 48961 2 2 0 2 1 0 0 43912.9 43912.9 97363.9 1 PROCESSED 54580.4644328704 54953 54580.4766550926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 032012 Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general. GALACTIC POINT SOURCES 4 B BOIRIN LAURENCE NULL NULL EUR 3 AO3 NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHER XIS Y V2129 OPH 246.9149 -24.3651 353.29078542 16.72506486 88.3342 54866.0202430556 54866.5821296296 403074010 21033.5 20000 21033.5 21033.5 0 21033.5 2 2 0 2 1 0 0 16533.1 16533.1 48533.9 0 PROCESSED 54962.2439583333 55329 54880.5317708333 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 032022 We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties. GALACTIC POINT SOURCES 4 B ROBRADE JAN NULL NULL EUR 3 AO3 ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS XIS Y ESO 137-G034 248.7664 -58.1298 329.07669192 -7.11373135 296.1293 54744.462650463 54746.6745833333 403075010 92052.5 90000 92061.3 92058.7 0 92052.5 2 2 0 2 1 0 0 83661.5 83661.5 191089.7 1 PROCESSED 54777.7021759259 55148 54780.6031828704 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 032025 Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas. GALACTIC POINT SOURCES 4 B GILLI ROBERTO NULL NULL EUR 3 AO3 ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNER HXD Y GK PER 52.8202 43.8404 151.00566373 -10.1477205 257.5144 54875.4415277778 54876.0899884259 403081010 30388.8 30000 30388.8 30388.8 0 30388.8 2 2 0 2 1 0 0 27399.9 27399.9 55997.9 2 PROCESSED 54962.3273842593 55330 54893.4257407407 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 033107 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 C YUASA TAKAYUKI HARRISON THOMAS JUS 3 AO3 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y AE AQUARII 310.0451 -0.9346 45.22328928 -24.45613885 265.1622 55120.7618518518 55124.2265393518 404001010 160454.6 160000 161451.9 161720.9 0 160454.6 2 2 0 2 1 0 0 136071.5 136071.5 299327.7 3 PROCESSED 55134.5131481482 55503 55134.5588194444 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040032 As picked up in the NASA press release in 2008, one of the most important results with Suzaku in three years was the first discovery of a possible non-thermal pulsation from a white dwarf AE Aquarii. This job was performed by our group. "Can magnetized white dwarfs accelerate particles like neutron stars?" This is the basic question of this study as a long standing mystery of Cosmic-ray origin for near 100 years. To ensure our result with Suzaku, we triggered the guest observation of AE Aquarii in TeV gamma-ray band with the recent powerful telescope, H.E.S.S., in their first GO program on 2009. Here, we propose the simultaneous observation with Suzaku and H.E.S.S, to distinguish the acceleration site in and/or outer of the binary system using X-ray and TeV gamma-ray flux informations. GALACTIC POINT SOURCES 4 A TERADA YUKIKATSU NULL NULL JAP 4 AO4 SUZAKU, H.E.S.S., OPTICAL SIMULTANEOUS OBSERVATION OF THE WHITE DWARF PULSAR, AE AQUARII HXD Y GS 1826-238 277.3735 -23.8572 9.22092987 -6.12003001 267.2862 55125.8488310185 55127.9502777778 404007010 102515.4 100000 102515.4 102531.4 0 102537.2 2 2 0 2 1 0 0 87999.6 87999.6 181541.8 2 PROCESSED 55166.3593171296 55534 55166.4220833333 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040035 We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations. GALACTIC POINT SOURCES 4 B YAMAOKA KAZUTAKA NULL NULL JAP 4 AO4 SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238 HXD Y UX ARIETIS 51.6466 28.6421 159.59610539 -22.97107378 272.6966 55229.7116666667 55231.7321064815 404008010 87799.3 90000 87799.3 87799.3 0 87799.3 2 2 0 2 1 0 0 79742.9 79742.9 174539.9 0 PROCESSED 55249.7969212963 55616 55249.830150463 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040036 We propose a hard X-ray observation of RS CVn-type active binary UX Arietis. Detection of nonthermal hard X-ray radiation is essentially important to solve the generation mechanism of stellar flares. UX Ari has a high coronal activity with a high temperature of ~2keV, and large stellar flares were frequently observed in the radio, UV, and X-ray band. Therefore, UX Ari is very suitable for hard X-ray observation of stellar flares. Large X-ray flares were observed by BeppoSAX, ASCA and Ginga sattellite, and hard X-ray emission upto ~50keV is detected by BeppoSAX. If a flare is large such as the events of former X-ray observations, we can detect the nonthermal hard X-ray emssion by Suzaku HXD. GALACTIC POINT SOURCES 4 C ISHIKAWA SHIN-NOSUKE NULL NULL JAP 4 AO4 STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETIS HXD Y RXJ0007.0+7302 1.8916 72.9843 119.68700382 10.38954096 241.7328 55204.6112847222 55207.0675231482 404011010 105373.9 100000 105373.9 105373.9 0 106971.4 2 2 0 1 1 0 0 58564.4 58564.4 212205.9 2 PROCESSED 55768.9294097222 55587 55768.9633333333 2.6.16.30 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 040054 We propose to observe the gamma-ray pulsar and itswind nebula (PWN) in the supernova remnant CTA1 with SUZAKU. Observations in X-ray wavebands are crucial to study non-thermal processes of PWNe. Its flux and spectral shape provide us important information about the energy distribution of the accelerated particles and the strength of the magnetic field. Observations made by Suzaku-HXD will constrain the X-ray spectrum above 20keV from the PWN for the first time. The high spectral resolution of XIS will allow us to search for metal lines, which tell us circumstance of the emission region. In addition, we will probably able to detect X-ray pulsation, which has notbeen detected yet, using XIS timing mode. GALACTIC POINT SOURCES 4 C TAKATA JUMPEI NULL NULL JAP 4 AO4 X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1 HXD N U SCO 245.6288 -17.8156 357.72079613 21.90901194 93.2747 55233.0102430556 55234.2918865741 404018010 46076.4 20000 46076.4 46076.4 0 46076.4 2 2 0 2 1 0 0 37611.7 37611.7 110719.9 1 PROCESSED 55250.138912037 55617 55250.1559375 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040057 We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. GALACTIC POINT SOURCES 4 A TAKEI DAI NULL NULL JAP 4 AO4-TOO TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION HXD Y U SCO 245.629 -17.8143 357.72199881 21.90970563 93.274 55236.514375 55237.1668865741 404018020 28936.9 20000 28936.9 28936.9 0 28936.9 2 2 0 2 1 0 0 18328.8 18328.8 56369.9 0 PROCESSED 55251.137349537 55619 55251.1498611111 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040057 We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. GALACTIC POINT SOURCES 4 A TAKEI DAI NULL NULL JAP 4 AO4-TOO TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION HXD Y U SCO 245.6292 -17.8133 357.72295453 21.91020567 93.2753 55239.299224537 55239.8259027778 404018030 26826 20000 26826 26826 0 26826 1 1 0 1 1 0 0 24903.7 24903.7 45472 1 PROCESSED 55253.1048263889 55619 55253.1155671296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040057 We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. GALACTIC POINT SOURCES 4 A TAKEI DAI NULL NULL JAP 4 AO4-TOO TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION HXD Y EUVE J0317-85.5 48.9864 -85.5003 299.84736337 -30.72881529 65.46 55028.6017476852 55030.1460185185 404019010 63084.3 60000 63084.3 63084.3 0 63084.3 2 2 0 2 1 0 0 56896.5 56896.5 133413.8 1 PROCESSED 55040.2354050926 55406 55040.2674305556 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040083 Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects. GALACTIC POINT SOURCES 4 B HARAYAMA ATSUSHI NULL NULL JAP 4 AO4 FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF HXD Y V603 AQL 282.2246 0.5976 33.17431822 0.83751501 93.9529 55267.0156597222 55267.9773032407 404020010 34917.3 30000 34930.9 34917.3 0 34930.9 2 2 0 2 1 0 0 30204.5 30204.5 83077.8 1 PROCESSED 55279.4289814815 55645 55279.4471296296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040095 The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 4 AO4 IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES XIS Y TT ARI 31.7181 15.2972 148.52228749 -43.79443 71.0668 55018.4424652778 55019.3023611111 404021010 35742.1 35000 35742.1 35779.6 0 35787.6 2 2 0 2 1 0 0 31794 31794 74257.8 1 PROCESSED 55029.2174884259 55399 55029.236712963 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040095 The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 4 AO4 IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES XIS Y Z CAM 126.2993 73.0997 141.39550179 32.62975748 289.0998 54931.1187152778 54931.9092476852 404022010 37663 35000 37663 37663 0 37663 2 2 0 2 1 0 0 36532.9 36532.9 68289.9 0 PROCESSED 54949.0999074074 55324 54949.4517824074 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040095 The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 4 AO4 IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES XIS Y HESS J0632+057 98.2448 5.8057 205.66080027 -1.43890266 289.9631 54941.5631944444 54944.1542708333 404027010 100034.3 100000 100034.3 100034.3 0 100034.3 2 2 0 2 1 0 0 82391.8 82391.8 223841.9 6 PROCESSED 54966.4980092593 55336 54966.5323958333 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040102 We propose a coordinate observation of HESS J0632+057 with Suzaku and VLA. This source is recently discovered as a fourth gamma-ray binary with HESS and XMM-Newton, and our results obtained in Suzaku AO-3 also confirmed a gradual variety of X-ray intensity, possibly associated with the binary period. With a combined observation with VLA, we will for the first time obtain a "real-time" variety from both of image and spectrum of this interesting source. GALACTIC POINT SOURCES 4 A KOKUBUN MOTOHIDE NULL NULL JAP 4 AO4 SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLA XIS Y BG CMI 112.8488 9.8847 208.51997296 13.31865509 292.793 54932.5078703704 54933.5710532407 404029010 47079.1 40000 47087.1 47079.1 0 47087.1 1 1 0 1 1 0 0 45034.6 45034.6 91808 2 PROCESSED 54949.3252777778 55324 54949.5279050926 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A YUASA TAKAYUKI NULL NULL JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y PQ GEM 117.7967 14.685 206.10344887 19.72488518 295.2889 54933.5737037037 54934.6329166667 404030010 46738.7 40000 46738.7 46738.7 0 46738.7 2 2 0 2 1 0 0 43247.9 43247.9 91507.9 0 PROCESSED 54949.3663773148 55324 54949.5317939815 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A YUASA TAKAYUKI NULL NULL JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y TX COL 85.7822 -41.0648 246.79781267 -29.77494364 322.4827 54963.6800578704 54965.2502199074 404031010 59781.8 40000 59789.8 59789.8 0 59781.8 2 2 0 2 1 0 0 51123 51123 135654 0 PROCESSED 54978.1891666667 55345 54978.2105439815 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A YUASA TAKAYUKI NULL NULL JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y FO AQR 334.4646 -8.2931 53.06192299 -49.11309098 76.4186 54987.3437152778 54988.5536921296 404032010 46084.6 40000 46084.6 46084.6 0 46084.6 2 2 0 2 1 0 0 33499.3 33499.3 104529.9 0 PROCESSED 54998.3063310185 55366 54998.3271064815 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A YUASA TAKAYUKI NULL NULL JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y AO PSC 343.7945 -3.1271 68.69841137 -53.28578539 60.9461 55004.4934143518 55005.3328587963 404033010 39654.4 40000 39654.4 39662.4 0 39662.4 2 2 0 2 1 0 0 35683.4 35683.4 72517.9 0 PROCESSED 55018.1524768518 55385 55018.165474537 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A YUASA TAKAYUKI NULL NULL JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y HD6903 17.4507 19.662 128.84764567 -42.9987034 70.0004 55031.3824305556 55032.3578703704 404034010 36813.5 35000 36829.5 36813.5 0 36821.5 2 2 0 2 1 0 0 29672.7 29672.7 84263.9 0 PROCESSED 55048.2899305556 55419 55048.3029976852 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041201 Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. GALACTIC POINT SOURCES 4 B AYRES THOMAS NULL NULL USA 4 AO4 ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP XIS Y HD72779 128.8308 19.5933 205.51018209 31.33811175 104.3214 55141.3245949074 55142.9515277778 404035010 71033.5 70000 71033.5 71033.5 0 71033.5 2 2 0 2 1 0 0 47461 47461 140555.9 0 PROCESSED 55166.1778819444 55532 55166.2074189815 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041201 Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. GALACTIC POINT SOURCES 4 B AYRES THOMAS NULL NULL USA 4 AO4 ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP XIS Y YY MEN 74.6207 -75.281 287.41045099 -33.23069192 7.2587 54996.0772916667 54998.5606365741 404036010 106949.8 100000 106957.8 106957.8 0 106949.8 2 2 0 2 1 0 0 104090.2 104090.2 214539.8 0 PROCESSED 55008.271087963 55378 55008.2997106482 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041202 The single K giant YY Men is one of the most active stars within 300 pc of the Sun, having produced 2 of the most powerful radio flares and 1 of the most powerful and long-duration optical flares ever detected. Its corona is one of the hottest and brightest known, with a *typical* X-ray luminosity of 32.0-32.5 (log erg/s) which most other cool stars only reach during major flares. We propose to obtain a 100-ksec observation of this hyperactive star to get a high S/N XIS exposure of its spectrum, particularly in the 5-10 keV region in which the XIS excels. We will study the He- and H-like Fe lines, search for 6.4 keV fluorescent emission, search for the presence of ultrahigh temperature and nonthermal spectral components, and look for correlations with simultaneous ATCA radio observations. GALACTIC POINT SOURCES 4 B DRAKE STEPHEN NULL NULL USA 4 AO4 THE EXTREME CORONAL PROPERTIES OF THE HYPERACTIVE K GIANT YY MEN XIS Y V773 TAU 63.5591 28.1916 168.22897578 -16.34488481 264.3183 55255.9666550926 55258.750162037 404037010 115405.7 120000 115405.7 115405.7 0 115405.7 2 2 0 2 1 0 0 95563 95563 240466.7 1 PROCESSED 55271.4577083333 55637 55271.499537037 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041203 Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence. GALACTIC POINT SOURCES 4 C OSTEN RACHEL NULL NULL USA 4 AO4 X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAU XIS Y ETA CARINAE 161.2306 -59.7313 287.60339978 -0.67900846 291.9998 54992.8234143518 54994.2918865741 404038010 51225.9 45000 51225.9 51233.9 0 51233.9 2 2 0 2 1 0 0 49118.6 49118.6 126839.8 0 PROCESSED 55006.223125 55378 55006.2447569444 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041204 The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. GALACTIC POINT SOURCES 4 A HAMAGUCHI KENJI NULL NULL USA 4 AO4 HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR HXD Y ETA CARINAE 161.2575 -59.6351 287.57052339 -0.58758586 87.8919 55156.1883449074 55157.3196643518 404039010 49388.7 45000 49388.7 49388.7 0 49388.7 2 2 0 2 1 0 0 34255.3 34255.3 97720.1 0 PROCESSED 55176.3471412037 55542 55176.3651388889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041204 The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. GALACTIC POINT SOURCES 4 A HAMAGUCHI KENJI NULL NULL USA 4 AO4 HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR HXD Y SKY(270, +25) 270.2558 25.1504 50.99920401 21.68976417 70.6538 55284.5620023148 55285.2994791667 404041010 1701.9 25000 1926.6 2094.4 0 1701.9 2 2 0 2 1 0 0 5621.1 5621.1 63713.9 1 PROCESSED 55369.1451273148 55284 55301.2652314815 2.5.16.28 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 041222 Suzaku has recently revealed relativistically broadened Fe Kalpha emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs that we have examined, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Only with the sensitivity of Suzaku, its high effective area in the Fe K band, and its broad bandpass has it been possible to robustly determine the shape of the lines. With a longer-term aim of completing a census of iron lines in neutron star LMXBs, we request a total of 200 ks to observe 5 neutron star low-mass X-ray binaries to study the relativistic broadening in the Fe Kalpha emission line profiles. GALACTIC POINT SOURCES 4 C CACKETT EDWARD NULL NULL USA 4 AO4 AN FE KALPHA EMISSION LINE SURVEY OF NEUTRON STAR LMXBS HXD Y 4U 1608-52 243.1847 -52.3651 330.96850701 -0.81056533 96.6085 55266.077650463 55267.0072222222 404044010 34010.1 30000 34010.1 34010.1 0 34010.1 2 2 0 2 1 0 0 30194 30194 80297.8 0 PROCESSED 55279.4317592593 55647 55279.4591666667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041223 The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL USA 4 AO4-TOO ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST HXD Y 4U 1608-52 243.1805 -52.3646 330.96698106 -0.80844416 94.0316 55270.6937615741 55271.6668287037 404044020 32718.1 30000 32718.1 32726.1 0 32718.1 2 1 0 2 1 0 0 26988 26988 84055.8 1 PROCESSED 55285.1012268518 55651 55285.1175462963 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041223 The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL USA 4 AO4-TOO ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST HXD Y 4U 1608-52 243.2309 -52.3757 330.98178647 -0.83761569 125.7606 55273.9986689815 55274.9154166667 404044030 31756.8 30000 31756.8 31756.8 0 31756.8 2 2 0 2 1 0 0 15309.4 15309.4 79193.8 0 PROCESSED 55286.243587963 55652 55286.259849537 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041223 The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL USA 4 AO4-TOO ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST HXD Y 4U 1608-52 243.1735 -52.4241 330.92310685 -0.84886634 127.9983 55277.989849537 55278.9140393518 404044040 16072.8 30000 16072.8 16072.8 0 16072.8 3 3 0 3 1 0 0 15655.7 15655.7 79843.9 2 PROCESSED 55298.7005902778 55665 55299.4128819444 2.5.16.28 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 041223 The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL USA 4 AO4-TOO ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST HXD Y A 0535+26 84.7195 26.3786 181.38803208 -2.61609461 86.1856 55067.9626273148 55069.1599421296 404054010 51866.8 45000 51870.6 51870.6 0 51866.8 2 2 0 2 1 0 0 42078 42078 103429.8 1 PROCESSED 55078.2009722222 55448 55078.219837963 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041232 We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 4 AO4-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD Y A 0535+26 84.7291 26.2457 181.50526016 -2.67952465 272.2555 55292.5024074074 55293.7029282407 404055010 3177.9 45000 3177.9 3460.4 0 3177.9 2 2 0 2 1 0 0 34392.8 34392.8 103715.8 1 PROCESSED 55323.348287037 55689 55323.4435532407 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 041232 We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 4 AO4-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD Y IGRJ16393-4643 249.7688 -46.7009 338.00177501 0.07896045 111.6627 55267.9865740741 55269.4508564815 404056010 50540 50000 50564 50540 0 50564 2 2 0 2 1 0 0 42256.5 42256.5 126467.8 1 PROCESSED 55279.4391898148 55647 55279.4686689815 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041234 Stellar winds play a critical role in several as yet poorly understood astrophysical processes. One of the best laboratories for studying winds is in wind fed Supergiant High Mass X-ray binaries. Using the neutron star (NS) as a backlight, variable absorption in X-rays measures column density variations in the secondary star wind. A recent explosion in the number of known HMXBs has defined two additional subclasses of HMXBs, potentially related through geometry and wind properties: 1) heavily obscured sources and 2) so-called Supergiant Fast X-ray Transients (SFXTs). We propose observations of 2 obscured sgHMXBs and 2 SFXTs to monitor the column density. This will test wind models and probe whether these subclasses are related to one another and to classical HMXBs through wind parameters. GALACTIC POINT SOURCES 4 C MORRIS DAVID NULL NULL USA 4 AO4 PROBING DONOR STAR WIND STRUCTURE IN HMXBS THROUGH VARIABLE ABSORPTION XIS Y GS 2023+338 306.0444 33.8015 73.0785131 -2.14854563 252.4521 55142.9636805556 55144.0550810185 404059010 42324.6 40000 42348.6 42324.6 0 42356.6 2 2 0 2 1 0 0 29140.4 29140.4 94283.9 1 PROCESSED 55155.0909837963 55531 55155.1065625 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041243 The quiescent state is the dominant accretion mode for black holes on all mass scales. Our knowledge of the X-ray spectrum is limited due to the characteristic low luminosity in this state. Here, we propose a 40 ks observation of the most luminous quiescent stellar mass black hole GS 2023+338 (V404 Cyg). These observations will allow us to detect hard X-ray emission from a quiescent stellar mass black hole for the first time, providing unique contraints on the nature of the accretion flow in this low luminosity state. GALACTIC POINT SOURCES 4 B REYNOLDS MARK NULL NULL USA 4 AO4 CONSTRAINING THE QUIESCENT ACCRETION FLOW AROUND A BLACK HOLE WITH SUZAKU HXD Y GRS 1758-258 270.2971 -25.679 4.56169204 -1.32563061 89.3817 55263.8983333333 55266.0711111111 404060010 82682.7 80000 82682.7 82682.7 0 82682.7 2 2 0 2 1 0 0 71178.9 71178.9 187709.7 1 PROCESSED 55279.5119560185 55647 55279.5468402778 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041244 We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state. GALACTIC POINT SOURCES 4 B REYNOLDS MARK NULL NULL USA 4 AO4 CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258 HXD Y LMC X-1 84.947 -69.7479 280.20680376 -31.50316575 10.0004 55033.776724537 55036.8953587963 404061010 129867.9 120000 129867.9 129867.9 0 129867.9 2 2 0 2 1 0 0 132597.6 132597.6 269395.6 4 PROCESSED 55048.6041319444 55419 55048.6509143518 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041245 We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. GALACTIC POINT SOURCES 4 A MCCLINTOCK JEFFREY NULL NULL USA 4 AO4 MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE XIS Y LMC X-3 84.7128 -64.0821 273.5746003 -32.09166858 184.4521 55186.5265162037 55190.9105555556 404062010 154424.2 150000 154434 154434 0 154424.2 2 2 0 2 1 0 0 101172.1 101172.1 352145.8 2 PROCESSED 55218.635787037 55587 55218.7384375 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041245 We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. GALACTIC POINT SOURCES 4 C MCCLINTOCK JEFFREY NULL NULL USA 4 AO4 MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE XIS Y XTE J1710-281 257.5483 -28.1282 356.35839186 6.92613447 86.2275 55278.9207638889 55281.1460300926 404068010 76138.5 75000 76138.5 76146.5 0 76146.5 3 3 0 3 1 0 0 23656.5 23656.5 192239.7 3 PROCESSED 55301.4782291667 55668 55301.5227662037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 042003 We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV. GALACTIC POINT SOURCES 4 C BOIRIN LAURENCE NULL NULL EUR 4 AO4 SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPS XIS Y 4U 1820-30 275.9267 -30.4234 2.73525617 -7.94773658 265.1815 55083.1120023148 55083.2015740741 404069010 3517.5 20000 3525.5 3517.5 0 3525.5 1 1 0 1 1 0 0 3712.4 3712.4 7738 0 PROCESSED 55109.0986574074 55475 55109.4203125 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1820-30 275.9248 -30.4209 2.73676025 -7.94514519 265.9319 55088.3645833333 55088.8141087963 404069020 21037.3 20000 21037.3 21037.3 0 21037.3 1 1 0 1 1 0 0 17170 17170 38831.9 0 PROCESSED 55099.5977199074 55469 55103.4457407407 2.4.12.26 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1820-30 275.9316 -30.4206 2.73970623 -7.95024046 261.8755 55096.0447453704 55096.8335416667 404069030 29225.4 20000 29225.4 29225.4 0 29225.4 2 1 0 2 1 0 0 25940.5 25940.5 68148 1 PROCESSED 55110.3776736111 55477 55110.3989699074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1820-30 275.9314 -30.4193 2.74079847 -7.94949913 261.8762 55102.6696759259 55103.5002662037 404069040 28699.4 20000 28699.4 28699.4 0 28699.4 3 2 0 3 1 0 0 24926.1 24926.1 71751.9 2 PROCESSED 55133.2057291667 55499 55133.2273263889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1820-30 275.9251 -30.4172 2.74021083 -7.94370371 265.2009 55111.1096643518 55111.700162037 404069050 21767.4 20000 21767.4 21767.4 0 21767.4 1 1 0 1 1 0 0 15674.3 15674.3 51003.9 0 PROCESSED 55127.2852777778 55496 55127.2938194445 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1820-30 275.9218 -30.4206 2.73584989 -7.94270191 269.3964 55116.6321064815 55117.1759143518 404069060 24668.7 100000 0 24668.7 0 24668.7 0 1 0 2 1 0 0 16950.5 16950.5 46978 0 PROCESSED 55131.3551273148 55507 55131.3693518518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1820-30 275.9205 -30.4212 2.7347979 -7.94197311 270.4164 55124.2356134259 55124.7925810185 404069070 24056.6 100000 24056.7 24072.6 0 24056.6 3 1 0 2 1 0 0 18903.5 18903.5 48107.9 0 PROCESSED 55134.2286805556 55503 55134.2427314815 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042004 Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL EUR 4 AO4 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y IGR J08408-4503 130.2449 -45.0216 264.03123634 -1.90203871 133.4432 55176.7452199074 55179.5002199074 404070010 92566 100000 92646 92566 0 92630 2 2 0 2 1 0 0 69434.4 69434.4 237989.8 2 PROCESSED 55200.3555555556 55567 55200.3941550926 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042007 We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class. GALACTIC POINT SOURCES 4 C SIDOLI LARA NULL NULL EUR 4 AO4 SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503 HXD Y GX 9+9 262.9404 -16.8929 8.57505694 9.06920034 97.5329 55271.6738773148 55273.9918981482 404071010 85187.1 75000 85208.7 85203.1 0 85187.1 2 1 0 2 1 0 0 61694.2 61694.2 200263.9 0 PROCESSED 55285.3728125 55652 55285.4179513889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042011 We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations. GALACTIC POINT SOURCES 4 B DIAZ TRIGO MARIA NULL NULL EUR 4 AO4 A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS HXD Y CYGNUS X-1 299.5964 35.2723 71.39800953 3.09942804 95.8123 54924.0537384259 54924.5654282407 404075010 15309.1 300000 15309.1 15318.8 0 15310.8 2 1 0 2 1 0 0 15537.4 15537.4 44203.9 1 PROCESSED 54949.2372685185 54922 54949.4917824074 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5895 35.2721 71.39489928 3.10413213 91.3103 54929.2562847222 54929.8224421296 404075020 21336.1 300000 21336.1 21336.1 0 21336.1 2 1 0 2 1 0 0 13125.8 13125.8 48914 0 PROCESSED 54949.2296180556 54922 54949.4903125 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5891 35.272 71.39464341 3.10435878 91.3113 54935.7650462963 54936.1473958333 404075030 17108.8 300000 17108.8 17116.8 0 17108.8 2 1 0 2 1 0 0 12986 12986 33027.9 1 PROCESSED 54949.3379282407 54922 54949.5303240741 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5791 35.2719 71.39029863 3.11127562 84.0536 54944.1674768518 54944.6252777778 404075040 18014 300000 18016.6 18014 0 18016.6 1 1 0 1 1 0 0 16327.7 16327.7 39550 0 PROCESSED 54966.2993055556 54922 54966.3125 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5814 35.2712 71.39067981 3.10930809 85.1433 54949.7099884259 54950.2175925926 404075050 20521.2 300000 20529.2 20535.4 0 20521.2 2 1 0 2 1 0 0 12401.3 12401.3 43845.9 0 PROCESSED 54976.1928819445 54922 54976.2030671296 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5392 35.2589 71.36219421 3.13231837 55.3254 54957.7006828704 54958.1356365741 404075060 19434.5 300000 19434.5 19450.5 0 19434.5 2 1 0 2 1 0 0 15279.5 15279.5 37557.9 0 PROCESSED 54976.076875 54922 54976.0885300926 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6653 35.165 71.33570459 2.99545336 212.8004 55182.0619328704 55182.5508564815 404075070 22101.9 300000 22101.9 22109.9 0 23664 1 1 0 1 1 0 0 3460.7 3460.7 42236 0 PROCESSED 55200.2251967593 54922 55200.4490046296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD N CYGNUS X-1 299.5434 35.2592 71.36423878 3.12954641 57.7977 54971.0242592593 54971.6043865741 404075080 21340.4 300000 21340.4 21348.4 0 21340.4 2 1 0 2 1 0 0 17495.4 17495.4 50119.9 1 PROCESSED 54991.970150463 54922 54992.6546875 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5373 35.2573 71.3600172 3.13281014 53.4895 54976.3582060185 54976.8259722222 404075090 20925.2 300000 20925.2 20933.2 0 20925.2 2 1 0 2 1 0 0 16116.4 16116.4 40412 1 PROCESSED 54992.0771527778 54922 54992.6651736111 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5337 35.2545 71.35609035 3.13386262 50.0944 54980.4956712963 54981.0586226852 404075100 28784.5 300000 28784.5 28784.5 0 28784.5 1 1 0 1 1 0 0 25738.9 25738.9 48631.9 1 PROCESSED 54994.3722569445 54922 54994.3872800926 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5294 35.2515 71.35169447 3.13529932 46.7675 54984.481400463 54984.9870833333 404075110 17450.2 300000 19037 17778.2 0 17450.2 1 1 0 1 1 0 0 15040.9 15040.9 43687.9 1 PROCESSED 54994.3906134259 54922 54994.4091087963 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.5272 35.2497 71.34921869 3.1358965 44.7834 54986.8208333333 54987.3356944444 404075120 16873.3 300000 16881.3 16889.4 0 16873.3 2 1 0 2 1 0 0 6764.7 6764.7 44477.9 1 PROCESSED 55000.9993171296 54922 55001.0163078704 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6021 35.1308 71.27949874 3.02171591 263.2299 55125.3772106482 55125.8404398148 404075130 20498.5 300000 20498.5 20506.5 0 20498.5 2 1 0 2 1 0 0 15163 15163 40015.9 0 PROCESSED 55134.2590509259 54922 55134.2701967593 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6086 35.1319 71.28321336 3.01775246 259.2069 55130.2652314815 55130.7481365741 404075140 23104.2 300000 23104.2 23128.2 0 23120.2 2 1 0 2 1 0 0 20011 20011 41716 0 PROCESSED 55141.3428935185 54922 55141.3539467593 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6206 35.1339 71.29004535 3.01042005 252.1788 55138.8946180556 55139.4106365741 404075150 22616.8 300000 22616.8 22624.8 0 22616.8 2 1 0 2 1 0 0 14061 14061 44575.9 1 PROCESSED 55149.4078703704 54922 55149.4202199074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6277 35.1371 71.29581116 3.00713364 246.5433 55145.8193981482 55146.4377199074 404075160 26022.2 300000 26022.2 26038.2 0 26026.5 2 1 0 2 1 0 0 18250.5 18250.5 53416 0 PROCESSED 55176.1865046296 54922 55176.2027430556 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6355 35.1397 71.30136328 3.00304649 241.2259 55152.2855092593 55152.9418287037 404075170 23448.5 300000 23448.5 23888.5 0 23880.5 2 1 0 2 1 0 0 18707.1 18707.1 56691.8 3 PROCESSED 55162.1854282407 54922 55162.2019212963 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6354 35.1397 71.30132058 3.00311627 241.1557 55159.514224537 55160.1328587963 404075180 21768.5 300000 21768.5 22480.5 0 22472.5 5 2 0 3 1 0 0 11406.4 11406.4 53435.8 0 PROCESSED 55176.2779976852 54922 55176.294849537 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6537 35.1518 71.31947353 2.99665901 225.8159 55166.2922453704 55166.8904398148 404075190 22415.5 300000 22415.5 22431.5 0 22423.5 2 1 0 2 1 0 0 13157.8 13157.8 51673.9 0 PROCESSED 55181.275150463 54922 55181.288912037 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD Y CYGNUS X-1 299.6549 35.1555 71.32314713 2.99775182 222.7295 55173.647349537 55174.1043287037 404075200 20016.6 300000 20016.6 21752.6 0 21859.3 1 1 0 1 1 0 0 17442.6 17442.6 39471.9 0 PROCESSED 55189.2589814815 54922 55189.2752430556 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 044131 In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. GALACTIC POINT SOURCES 4 A MILLER JON YAMADA SHIN USJ 4 AO4 A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE HXD N 1E 2259+586 345.2716 58.9493 109.11022544 -0.92895504 86.3239 54976.8335300926 54978.6446064815 404076010 122579.1 120000 122580.9 122580.9 0 122579.1 2 2 0 2 1 0 0 103446.2 103446.2 156463.8 1 PROCESSED 54992.1777546296 54922 54992.6935069444 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y SGR 1900+14 286.7986 9.3873 43.07377535 0.80526184 82.6704 54947.7664814815 54949.0807175926 404077010 53137.4 50000 53393.4 53393.4 0 53137.4 2 2 0 2 1 0 0 42101.1 42101.1 113547.9 1 PROCESSED 54973.2438078704 54922 54973.4547222222 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y SGR 0501+4516 75.2795 45.3414 161.49568149 1.98976538 93.3341 55060.8485069445 55061.8348842593 404078010 42675.3 40000 42675.3 42955.3 0 42891.3 2 2 0 2 1 0 0 27487.8 27487.8 85185.8 0 PROCESSED 55071.2445138889 54922 55071.2594328704 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y 4U0142+61 26.5176 61.8112 129.33625727 -0.37933599 61.041 55055.0703125 55057.3654976852 404079010 107412.9 100000 107412.9 107420.9 0 107422.7 2 2 0 2 1 0 0 99757.6 99757.6 198283.8 2 PROCESSED 55068.2751157407 54922 55068.3037268518 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y 1RXS J1708-4009 257.2032 -40.2034 346.44001394 -0.00188973 266.4021 55066.6841203704 55067.9466898148 404080010 60886.9 60000 60886.9 60894.9 0 60904.6 3 2 0 2 1 0 0 51531.3 51531.3 109075.8 1 PROCESSED 55078.1617476852 54922 55078.1751851852 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y PSR J1846-0258 281.5972 -2.9106 29.7662115 -0.20474108 86.0001 54936.8175578704 54939.6779398148 404081010 104345.1 100000 104345.1 104367.5 0 104353.1 2 2 0 2 1 0 0 76006.5 76006.5 247101.8 1 PROCESSED 54959.4243981482 54922 54959.5006018518 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y CYG X-1 299.59033 35.20161 71.33499876 3.06682766 -99 NULL NULL 405001010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050020 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 405002010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050020 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 405003010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050020 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 405004010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050020 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 405005010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050020 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM or MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N IGR J16167-4957 244.155 -49.97986 333.05429094 0.49667919 -99 NULL NULL 405006010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050025 The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system. GALACTIC POINT SOURCES 4 C YUASA TAKAYUKI NULL NULL JAP 5 AO5 ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES XIS Y IGR J15094-6649 227.3484 -66.8278 315.91945149 -7.50109233 90.4626 55588.7031365741 55589.5557638889 405007010 49461.2 50000 49483.2 49475.2 0 49461.2 2 2 0 2 1 0 0 48018.5 48018.5 73659.9 0 PROCESSED 55621.2159490741 55990 55621.2282291667 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050025 The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system. GALACTIC POINT SOURCES 4 C YUASA TAKAYUKI NULL NULL JAP 5 AO5 ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES XIS Y V773TAU 63.5571 28.1952 168.22500409 -16.34364304 260.6557 55610.1581712963 55611.9815277778 405011010 82246.3 80000 82254.3 82246.3 0 82254.3 2 2 0 2 1 0 0 72828.7 72828.7 157525.8 2 PROCESSED 55621.2758680556 55990 55621.2978703704 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050033 We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. GALACTIC POINT SOURCES 4 B TSUBOI YOHKO NULL NULL JAP 5 AO5 NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE XIS Y PSR J1429-5911 217.5051 -59.1899 315.26780851 1.30018252 101.124 55588.2265625 55588.7001157407 405012010 30382.4 30000 30390.4 30398.4 0 30382.4 1 1 0 1 1 0 0 28792.3 28792.3 40903.9 0 PROCESSED 55602.1319328704 55968 55602.1404513889 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050047 Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC POINT SOURCES 4 C KAWAI NOBUYUKI NULL NULL JAP 5 AO5 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y PSR J1044-5737 161.1338 -57.616 286.57019106 1.16750605 109.1973 55542.2984259259 55542.7292939815 405013010 22630 30000 22630 22630 0 22635.8 1 1 0 1 1 0 0 21960.3 21960.3 37200 0 PROCESSED 55550.9573726852 55917 55550.9648148148 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050047 Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC POINT SOURCES 4 C KAWAI NOBUYUKI NULL NULL JAP 5 AO5 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y PSR J0614-33 93.5386 -33.5015 240.50300829 -21.83180137 119.1484 55498.9719675926 55499.6140740741 405014010 31210.9 30000 31210.9 31210.9 0 31210.9 2 2 0 2 1 0 0 27331.4 27331.4 55449.9 0 PROCESSED 55509.025625 55875 55509.0359722222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050047 Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC POINT SOURCES 4 C KAWAI NOBUYUKI NULL NULL JAP 5 AO5 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y PSR J2055+2539 313.957 25.6505 70.67687842 -12.53222207 262.3229 55498.1479398148 55498.9578356482 405015010 31106.9 30000 31106.9 31106.9 0 31106.9 1 1 0 1 1 0 0 21458.1 21458.1 69967.9 0 PROCESSED 55523.9823611111 55890 55523.9927314815 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050047 Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC POINT SOURCES 4 C KAWAI NOBUYUKI NULL NULL JAP 5 AO5 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y PSR J1957+5036 299.4354 50.5474 84.58480161 10.99652902 216.5649 55543.4586689815 55544.0842939815 405016010 32469 30000 32485 32469 0 32485 2 2 0 2 1 0 0 25313.9 25313.9 54033.9 2 PROCESSED 55592.9227893518 55959 55592.9341782407 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050047 Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC POINT SOURCES 4 C KAWAI NOBUYUKI NULL NULL JAP 5 AO5 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y LS5039 276.56263 -14.84822 16.88169314 -1.28903495 -99 NULL NULL 405019010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050049 LS5039 belongs to a newly established category, gamma-ray binary. LS5039 shows striking orbital modulation in the photon index and the flux at TeV energies. We discovered that the X-ray emission is non-thermal due to Synchrotron emission. LS5039 is the first object that shows non-thermal X-ray emission modulated with the orbital period. We also discovered that the shape of the light curve resembles that of TeV gamma-ray. By using the archival data, we found that even fine structures in the light curve seems to repeat every orbit of the system. We propose to observe the source for 80 ks to confirm whether LS5039 shows exactly same non-thermal features in different orbits. GALACTIC POINT SOURCES 4 C TAKAHASHI TADAYUKI NULL NULL JAP 5 AO5 STUDY OF ORBITAL MODULATION OF GAMMA-RAY BINARY LS5039 HXD N V4641 SGR 274.84013 -25.40717 6.77395378 -4.7890572 -99 NULL NULL 405020010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050058 We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics:1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, RXTE/ASM and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planed simultaneously with RXTE, Fermi, AGILE and many radio and optical/NIR observatories. GALACTIC POINT SOURCES 4 A YAMAOKA KAZUTAKA NULL NULL JAP 5 AO5-TOO THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR HXD N V2487 OPH 262.9946 -19.3061 6.53905762 7.73892052 274.1277 55478.2880439815 55479.5827893518 405021010 56307.6 50000 56315.6 56307.6 0 56323.6 2 2 0 2 1 0 0 51358 51358 111832 2 PROCESSED 55488.1606018518 55854 55488.179224537 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050059 Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141. GALACTIC POINT SOURCES 4 A TERADA YUKIKATSU NULL NULL JAP 5 AO5 SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU HXD Y IGR J00234+6141 5.7092 61.7549 119.55446517 -0.92914674 80.286 55372.004375 55373.2397569445 405022010 81880 80000 81880 81880 0 81880 2 2 0 2 1 0 0 70036.4 70036.4 106697.9 1 PROCESSED 55414.1609375 55780 55414.1791666667 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050059 Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141. GALACTIC POINT SOURCES 4 A TERADA YUKIKATSU NULL NULL JAP 5 AO5 SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU HXD Y W43 281.9 -1.94264 30.76557057 -0.03224669 -99 NULL NULL 405023010 -99 90000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050082 We propose to observe a young stellar cluster W43 with Suzaku. This program aims to examine the possibility of new particle acceleration mechanism by powerful stellar wind. The immediate goals of this program are two-fold: (1) to detect super hard X-rays for the first time, and (2) to compare non-thermal X-ray luminosity with VHE gamma-ray luminosity. GALACTIC POINT SOURCES 4 C SUGAWARA YASUHARU NULL NULL JAP 5 AO5 THE FIRST DETECTION OF SUPERHARD X-RAYS FROM YOUNG STELLAR CLUSTER W43 HXD N 1E 1547.0-5408 237.7284 -54.3676 327.20000551 -0.18012949 271.1663 55415.1611921296 55415.9633796296 405024010 51672.8 50000 51672.8 51792.8 0 52152.9 2 2 0 1 1 0 0 42781.2 42781.2 69299.9 0 PROCESSED 55427.2331828704 55793 55427.247025463 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050099 Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks. GALACTIC POINT SOURCES 4 B NISHIOKA HIROYUKI NULL NULL JAP 5 AO5 OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE HXD N EMS0918 211.2948 -61.3938 311.64055354 0.22486043 106.822 55589.5588310185 55590.0834837963 405025010 24542.5 20000 24550.5 24542.5 0 24558.5 2 2 0 2 1 0 0 23281.1 23281.1 45309.9 1 PROCESSED 55602.1924652778 55972 55602.2015046296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050104 Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. GALACTIC POINT SOURCES 4 A TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS1150 263.083 -32.7212 355.27740066 0.39306698 91.2452 55611.9964930556 55612.6968055556 405026010 20918.6 20000 20918.6 20918.6 0 20918.6 1 1 0 1 1 0 0 17263.9 17263.9 60503.9 0 PROCESSED 55621.1311921296 55988 55621.1440740741 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050104 Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. GALACTIC POINT SOURCES 4 A TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS01095 252.3381 -45.0256 340.43907916 -0.17827348 87.5534 55603.1544328704 55603.7613310185 405027010 20933.2 20000 20934.4 20934.4 0 20933.2 2 2 0 2 1 0 0 16976.2 16976.2 52431.9 0 PROCESSED 55616.9640972222 55983 55617.4127430556 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050104 Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. GALACTIC POINT SOURCES 4 A TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS1308 293.0393 19.2567 54.62289289 0.10827332 90.0001 55313.4365740741 55313.9766203704 405028010 23898.7 20000 23906.7 23906.7 0 23898.7 3 2 0 2 1 0 0 23209 23209 46652 1 PROCESSED 55327.1675231482 55693 55327.1789930556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050104 Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. GALACTIC POINT SOURCES 4 A TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y V1280 SCO 254.4172 -32.3368 351.33470039 6.5596985 97.7451 55605.3662615741 55608.0501851852 405029010 99683 100000 99699 99683 0 99699 2 2 0 2 1 0 0 86930.6 86930.6 231873.9 2 PROCESSED 55617.0939814815 55983 55617.4142361111 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050110 We propose a 100 ks observation of the C-rich classical nova V1280 Sco. Using Suzaku's excellent spectral performance in the soft X-ray energy band, we aim to detect and to resolve emission lines from C, N, and O. GALACTIC POINT SOURCES 4 A TAKEI DAI NULL NULL JAP 5 AO5 X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCO XIS Y HD125599 215.4515 -48.0762 318.15137849 12.10713587 289.1653 55414.6760069444 55415.1571990741 405030010 31048 30000 31056 31056 0 31048 1 1 0 1 1 0 0 24859.9 24859.9 41567.9 0 PROCESSED 55427.163912037 55793 55427.1753819444 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050116 Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 5 AO5 QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION XIS Y HD130693 222.5749 -24.4173 334.71293898 31.01917553 104.6337 55580.6525925926 55581.2384375 405031010 21314.5 20000 21314.5 21314.5 0 21314.5 2 2 0 2 1 0 0 17462.5 17462.5 50605.9 2 PROCESSED 55598.9706134259 55965 55598.9831597222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050116 Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 5 AO5 QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION XIS Y XSS J16537-1905 253.8855 -18.1447 2.56699105 15.52634316 96.7569 55602.7046412037 55603.1488657407 405032010 20024.3 20000 20032.3 20040.3 0 20024.3 2 2 0 2 1 0 0 18152.8 18152.8 38343.9 0 PROCESSED 55616.932650463 55983 55617.4104282407 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050116 Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 5 AO5 QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION XIS Y XSS J17223-7301 259.6949 -73.4263 319.10640118 -19.70481928 106.6643 55302.152650463 55302.5939467593 405033010 33386.1 30000 33386.1 33386.1 0 33386.1 2 2 0 2 1 0 0 25588.9 25588.9 38127.9 0 PROCESSED 55326.1356828704 55692 55326.1437731482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050116 Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. GALACTIC POINT SOURCES 4 B EBISAWA KEN NULL NULL JAP 5 AO5 QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION XIS Y EG AND 11.168 40.673 121.54657283 -22.18054863 225.2111 55597.6281018518 55600.0030092593 405034010 100533.3 100000 100533.3 100541.3 0 100549.3 2 2 0 2 1 0 0 84658.9 84658.9 205171.9 3 PROCESSED 55614.2725 55983 55614.2972106482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051211 The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae. GALACTIC POINT SOURCES 4 C NELSON THOMAS NULL NULL USA 5 AO5 EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARS XIS Y 4 DRA 187.4841 69.1938 125.77229084 47.81569563 339.9969 55304.8913773148 55305.8557291667 405035010 42260.2 40000 42268.2 42268.2 0 42260.2 2 2 0 2 1 0 0 43792 43792 83277.8 1 PROCESSED 55327.2043981482 55693 55327.2173958333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051212 The symbiotic star, 4 Dra, has been poorly studied in X-rays. Based on the ROSAT data, we argue that it is a nearby, lower accretion rate analogue of the hard X-ray bright symibiotic stars that have been detected above 10 keV. We propose the first pointed observation of 4 Dra that covers the entire 0.4-10 keV band to test our interpretation: we expect it to be bright above 2 keV, with an optically thin thermal spectrum, likely with a strong and complex intrinsic absorber. If confirmed, 4 Dra may turn out to be a key object in the study of hard X-ray emitting symbiotic stars. GALACTIC POINT SOURCES 4 B MUKAI KOJI NULL NULL USA 5 AO5 THE FIRST LOOK AT THE SYMBIOTIC STAR 4 DRA ABOVE 2 KEV XIS Y V2491 CYG 295.7679 32.3068 67.2208484 4.33923679 253.6206 55503.4390162037 55505.2709837963 405036010 74400.4 70000 74400.4 74400.4 0 74400.4 2 2 0 2 1 0 0 57206.5 57206.5 158251.9 2 PROCESSED 55518.384525463 55885 55518.4178356482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051213 We propose to observe again one of the most luminous and intriguing classical novae of the last two years, after it has returned to quiescence. The goala are to understand how accretion is re-estabilished, investigate the claim that the white dwarf an intermediate polar (IP), estimate mass accretion are and white dwarf mass. IP are a class of X-ray sources that Suzaku is ideally suited to study, and we want to study the influence of the magnetic field on the nova evolution. GALACTIC POINT SOURCES 4 C ORIO MARINA NULL NULL USA 5 AO5 REVISITING AN X-RAY LUMINOUS NOVA NOVA AFTER THE ERUPTION XIS Y PSR B1259-63 195.6931 -63.8349 304.18120501 -0.9906484 99.8696 55566.8369212963 55569.3959722222 405037010 90040.7 80000 90040.7 90040.7 0 90040.7 2 2 0 2 1 0 0 74450.6 74450.6 221061.8 1 PROCESSED 55595.2265856482 55961 55595.2642939815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051221 We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL USA 5 AO5 SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 XIS Y PSR B1259-63 195.6913 -63.8356 304.18038114 -0.9913128 117.5773 55594.1927662037 55594.4487731482 405038010 21478.1 20000 21494.1 21478.1 0 21494.1 1 1 0 1 1 0 0 15677.4 15677.4 22111.9 0 PROCESSED 55607.1219212963 55974 55607.1295601852 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051221 We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. GALACTIC POINT SOURCES 4 A UCHIYAMA YASUNOBU NULL NULL USA 5 AO5 SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 XIS Y 4U 0115+63 19.63292 63.74 125.92365665 1.02574493 -99 NULL NULL 405039010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051231 We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 5 AO5-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD N CEP X-4 324.878 56.98611 99.01219478 3.31239245 -99 NULL NULL 405040010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051231 We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 5 AO5-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD N XTE J1946+274 296.4201 27.2906 63.14511565 1.35338176 267.925 55480.9086805556 55482.2446064815 405041010 50731.7 45000 50731.7 50731.7 0 50731.7 2 2 0 2 1 0 0 46557.1 46557.1 115373.9 1 PROCESSED 55491.0811226852 55867 55491.1017476852 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051231 We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 5 AO5-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD Y V 0332+53 53.7495 53.17319 146.05199466 -2.19402959 -99 NULL NULL 405042010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051231 We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 5 AO5-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD N A 0535+26 84.7275 26.31581 181.44506907 -2.64343705 -99 NULL NULL 405043010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051231 We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 5 AO5-TOO CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU HXD N 4U 1626-67 248.0734 -67.4643 321.7866399 -13.09493758 285.8172 55445.5409259259 55446.2376273148 405044010 20033.5 20000 20033.5 20057.5 0 20045.7 2 2 0 2 1 0 0 19537.2 19537.2 60179.9 0 PROCESSED 55456.2165162037 55822 55456.2336574074 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051234 Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist. GALACTIC POINT SOURCES 4 A FINGER MARK NULL NULL USA 5 AO5 THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSAL XIS Y 4U 1210-64 183.3036 -64.8719 298.88624165 -2.30082607 98.4956 55553.1591550926 55555.1488194444 405045010 79347.6 80000 79347.6 79347.6 0 79356.1 2 2 0 2 1 0 0 70751.2 70751.2 171879.9 0 PROCESSED 55595.0570717593 55961 55595.085474537 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051236 4U 1210-64 is a high mass X-ray binary with a stable 6.7 day period when the long-term (RXTE ASM) light curve is analyzed. However, we observed strong aperiodic variability in a series of pointed observations with the RXTE PCA, to the point of masking this 6.7 day period. Moreover, we have not detected a spin period, even though the accretor is most likely a neutron star. The strong variability is suggestive of accretion from a clumpy wind. We propose a 2-day Suzaku observation of this object (1) to search for unequivocal evidence for a neutron star, such as the spin period and cyclotron features; and (2) to measure the spectral shapes at different flux levels, to investigate the cause of the strong aperiodic variability. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 5 AO5 4U 1210-64: A HIGHLY VARIABLE X-RAY BINARY XIS Y 4U 0614+091 94.28042 9.13694 200.87736381 -3.36351731 -99 NULL NULL 405046010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051241 Suzaku has recently revealed relativistically broadened Fe K emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Both the sensitivity and broadband capability of Suzaku, make it possible to robustly determine the line shape. Here, we propose to observe two sources where no Fe K line was previously detected with older missions. Both sources are accreting at low Eddington fractions (<1%), hence we can test whether Fe K emission lines are ubiquitous in neutron star LMXBs at all luminosities, and explore whether the inner accretion disk is truncated at low Eddington fractions. GALACTIC POINT SOURCES 4 C CACKETT EDWARD NULL NULL USA 5 AO5 ARE FE KALPHA EMISSION LINES UBIQUITOUS IN NEUTRON STAR LMXBS? XIS N GX13+1 273.63192 -17.15589 13.51807927 0.10669908 -99 NULL NULL 405047010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051243 We recently proposed physical mechanisms to explain the 3 branches and 2 vertices of the accreting neutron stars known as Z sources. This work defines how the Eddington limit operates in the inner disk, and there is a need to investigate the inferred mass loss using other techniques. In parallel, we have used spectral analyses to reclassify GX13+1 as a Z source (Cyg X-2 sub-group). GX13+1 has exhibited strong, blue-shifted absorption lines (Chandra) and a moderate Fe emission line (RXTE). Observations of GX13+1 with Suzaku are intended: to refine the spectral model, to further test the models for each Z branches, to measure the profile and variations of the Fe emission line, and, most importantly, to determine whether the properties of the disk wind vary with position along the Z. GALACTIC POINT SOURCES 4 C REMILLARD RONALD NULL NULL USA 5 AO5 SPECTRAL EVOLUTION AND THE DISK WIND IN GX13+1 XIS N 4U 1728-34 262.9799 -33.9051 354.23908298 -0.18221646 278.0266 55473.517349537 55475.6876967593 405048010 50547.2 100000 50652.2 50547.2 0 50652.2 2 2 0 2 1 0 0 95360.6 95360.6 187467.8 3 PROCESSED 55487.4216898148 55867 55487.4662615741 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051244 Fe K-alpha lines have been detected in ten NS-LMXBs. Under the commonly accepted interpretation, they can be used to set tight constrains on the accretion disk geometry. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kHz QPOs. We have recently shown that simultaneous measurements of Fe lines and kHz QPOs in a NS-LMXB appear to contradict this picture. We propose to observe 4U 1728-34 with Suzaku five times for 20 ks, simultaneously with RXTE and ATCA. This program will allow us to study and compare the dynamics of the inner edge of the disk as inferred from the Fe line and the kHz QPOs, as well as the relation of both observables with the jet radio emission. GALACTIC POINT SOURCES 4 A LINARES MANUEL NULL NULL USA 5 AO5 ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. HXD Y 4U 1608-52 243.17917 -52.42306 330.92633867 -0.85047716 -99 NULL NULL 405049010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051245 The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL USA 5 AO5-TOO ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST XIS N AQL X-1 287.81687 0.58494 35.71842844 -4.14317601 -99 NULL NULL 405050010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051246 Long term optical/X-ray monitoring of X-ray binaries has revealed that the accretion flow pattern can be remarkably different during different outbursts of the same source, challenging standard disk-instability models. Of particular interest is the Low-Intensity State (LIS) in Aql X-1, where the optical-to-X-ray flux ratio is about a factor of 7 higher than that during normal outbursts explainable using the disk-instability model. Suzaku data, along with contemporaneous optical/IR and radio observations, will allow probing the nature of accretion flow in the LIS of Aql X-1. We request a 100 ksec ToO observation of Aql X-1 during a LIS to achieve our science goals. The observation will test the predictions of ADIOS models and constrain disk--jet coupling. GALACTIC POINT SOURCES 4 A MAITRA DIPANKAR NULL NULL USA 5 AO5-TOO SUZAKU OBSERVATIONS OF AQL X-1 DURING ITS LOW-INTENSITY STATE HXD N 4U 1630-47 248.5034 -47.402 336.90313759 0.24577164 279.8256 55432.911724537 55435.6134259259 405051010 99937.3 100000 99937.3 99937.3 0 99937.3 2 2 0 2 1 0 0 90451.2 90451.2 233397.6 2 PROCESSED 55449.390162037 55815 55449.4369560185 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051252 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 5 AO5-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS Y XTE J1752-223 268.06288 -22.34233 6.42317982 2.11424017 -99 NULL NULL 405052010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051252 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 5 AO5-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N XTE J1118+480 169.54542 48.03694 157.66026546 62.32060029 -99 NULL NULL 405053010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051252 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 5 AO5-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 405054010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051252 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 5 AO5-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N 4U 1543-47 236.78583 -47.66944 330.91865964 5.42579106 -99 NULL NULL 405055010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051252 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 5 AO5-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N GRS 1915+105 288.79833 10.94556 45.36563993 -0.21936861 -99 NULL NULL 405056010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051253 We propose a 25ks on-source (100ks total) ToO to observe a soft state of GRS 1915+105 at L<30% L Edd. This ToO will address several important science goals: (1) a measurement of the black hole spin via two independent methods (X-ray continuum fitting and broad iron line analysis), (2) the determination of the accretion disk-corona geometry via studies of fluorescence lines and Compton reflection components, and (3) investigation of the broad-band spectrum for input into photoionization models. GALACTIC POINT SOURCES 4 A LEE JULIA NULL NULL USA 5 AO5-TOO MEASURING THE GRS 1915+105 BLACK HOLE SPIN AND BROADBAND CONTINUUM PROPERTIES XIS N 4U 1957+11 299.8426 11.72 51.31417386 -9.31797438 71.6227 55320.4377777778 55321.4168055556 405057010 35796 35000 35804 35804 0 35796 2 2 0 2 1 0 0 30869.2 30869.2 84580 0 PROCESSED 55371.2334722222 55741 55375.7567013889 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051254 We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. GALACTIC POINT SOURCES 4 B NOWAK MICHAEL NULL NULL USA 5 AO5 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? XIS Y 4U 1957+11 299.8418 11.7197 51.31351001 -9.31745051 63.9325 55333.5190277778 55334.4675 405057020 34935.3 35000 34943.3 34951.3 0 34935.3 2 2 0 2 1 0 0 28262.5 28262.5 81911.8 0 PROCESSED 55347.2287037037 55714 55347.2466898148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051254 We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. GALACTIC POINT SOURCES 4 B NOWAK MICHAEL NULL NULL USA 5 AO5 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? XIS Y 4U 1957+11 299.8589 11.6979 51.30303986 -9.34292333 251.3459 55501.8275462963 55502.7001157407 405057030 35349.1 35000 35357.1 35349.1 0 35357.1 2 2 0 2 1 0 0 27169.7 27169.7 75362 0 PROCESSED 55515.2803125 55881 55515.3015046296 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051254 We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. GALACTIC POINT SOURCES 4 B NOWAK MICHAEL NULL NULL USA 5 AO5 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? XIS Y HER X-1 254.4936 35.2712 58.06646448 37.48255114 250.0637 55467.7830208333 55468.2362962963 405058010 21356.7 20000 21356.7 21356.7 0 21503.4 2 2 0 1 1 0 0 18932.3 18932.3 39159.9 0 PROCESSED 55477.2114930556 55843 55477.2237152778 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B STAUBERT R DIGER NULL NULL EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N HER X-1 254.4925 35.2707 58.06565994 37.48335671 250.2455 55468.7003356482 55469.2258912037 405058020 24303 20000 24303 24322.3 0 24467.7 2 2 0 1 1 0 0 22483.7 22483.7 45405.9 0 PROCESSED 55482.1187037037 55848 55482.4726967593 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B STAUBERT R DIGER NULL NULL EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N HER X-1 254.4632 35.2657 58.05457552 37.50615868 268.4858 55461.0002083333 55461.4494675926 405058030 19924 20000 19924 19924 0 20243.8 2 2 0 1 1 0 0 17507.3 17507.3 38811.9 0 PROCESSED 55470.1317708333 55836 55470.1508796296 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B STAUBERT R DIGER NULL NULL EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N HER X-1 254.4619 35.2659 58.05460857 37.50723847 268.3041 55461.7937037037 55462.2467476852 405058040 21740 20000 21740 21796 0 21870.4 1 1 0 1 1 0 0 19803 19803 39135.9 0 PROCESSED 55474.0823958333 55840 55474.0995486111 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052001 We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? GALACTIC POINT SOURCES 4 B STAUBERT R DIGER NULL NULL EUR 5 AO5 VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 HXD N MU COL 86.4962 -32.3107 237.28985275 -27.10600903 93.5874 55455.752337963 55456.3113541667 405059010 25961 20000 25961 25961 0 25961 1 1 0 1 1 0 0 21873.4 21873.4 48287.9 0 PROCESSED 55469.2321759259 55836 55469.2452314815 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052005 We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. GALACTIC POINT SOURCES 4 A OSKINOVA LIDIA NULL NULL EUR 5 AO5 STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU XIS Y 10 LAC 339.8111 39.0619 96.65409432 -16.97165842 81.7456 55344.5001967593 55345.0690162037 405060010 25028.4 25000 25028.4 25028.4 0 25028.4 2 2 0 2 1 0 0 21743.1 21743.1 49135.9 2 PROCESSED 55365.1720601852 55731 55365.1824305556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052005 We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. GALACTIC POINT SOURCES 4 A OSKINOVA LIDIA NULL NULL EUR 5 AO5 STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU XIS Y IGR J17348-2045 263.737 -20.747 5.68701621 6.37961854 -99 NULL NULL 405061010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052010 Soft gamma repeaters (SGRs) and the Anomalous X-ray pulsars (AXPs) constitute a small class of X-ray sources which are currently believed to host an ultra-magnetized neutron star, or magnetar. In this framework their bursting and persistent emission is powered by the decay of the ultra-strong field. Magnetar sources are rare (~15 known at present). Enlarging the sample of these objects is vital as it allows to test further models for their activity and as it will shed light on the links/differences among magnetars and other classes of isolated neutron stars. Our aim is to identify the two most promising magnetar candidates, selected among numerous unidentified INTEGRAL sources, because of their hard and peculiar X-ray spectrum and closeness to the galactic plane. GALACTIC POINT SOURCES 4 C PAVAN LUCIA NULL NULL EUR 5 AO5 CATCHING MAGNETAR CANDIDATES AMONG UNIDENTIFIED INTEGRAL SOURCES WITH SUZAKU XIS N GX 339-4 255.7015 -48.7852 338.94105133 -4.32146688 83.6944 55603.7634722222 55604.2349421296 405063010 22459.4 100000 22459.4 22459.4 0 22483.4 2 2 0 2 1 0 0 19328.7 19328.7 40727.9 0 PROCESSED 55616.9623032407 55983 55617.4120601852 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y GX 339-4 255.7013 -48.7848 338.94128957 -4.32111913 86.3597 55608.9686111111 55609.6501967593 405063020 21015.7 20000 21015.7 21015.7 0 21015.7 2 2 0 2 1 0 0 17595.8 17595.8 58883.9 0 PROCESSED 55621.143125 55988 55621.1561342593 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y GX 339-4 255.7016 -48.7831 338.94276391 -4.32024293 90.1024 55616.8233680556 55617.4487268518 405063030 19182 20000 19190 19198 0 19182 2 2 0 2 1 0 0 15684 15684 54025.9 1 PROCESSED 55628.1548032407 55996 55628.1679976852 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y GX 339-4 255.7013 -48.7851 338.94105066 -4.32130146 91.6296 55620.1778703704 55620.8022569445 405063040 21799 20000 21799 21807 0 21816.8 3 3 0 3 1 0 0 18850.2 18850.2 53923.9 0 PROCESSED 55642.1146527778 56009 55642.1310300926 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y GX 339-4 255.7041 -48.783 338.94384752 -4.32149031 92.8952 55627.5468518518 55628.0320138889 405063050 16992.5 20000 16992.5 20269.3 0 20269.3 2 2 0 2 1 0 0 15985.1 15985.1 41874.1 2 PROCESSED 55645.1978935185 56015 55645.2088078704 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS Y XTE J1817-330 274.43142 -33.01883 359.81722428 -7.99557413 -99 NULL NULL 405064010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 405065010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 405066010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS N XTE J1118+480 169.54542 48.03694 157.66026546 62.32060029 -99 NULL NULL 405067010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052015 We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 GALACTIC POINT SOURCES 4 A CABANAC CLEMENT NULL NULL EUR 5 AO5-TOO PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS XIS N J1832-084 278.15417 -8.45111 23.27208255 0.29793506 -99 NULL NULL 405068010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052021 The Galactic TeV sky is dominated by extended sources. Of the identified sources, only young pulsar wind nebulae (PWN) and binary systems are unresolved. TeV gamma-ray emission from these systems probes high energy particles very close to their acceleration sites. Binary systems offer additional diagnostic tools, e.g. through the modulation and the high density of the target photon field involved in the TeV-emitting Inverse Compton process. We propose Suzaku observations of a few TeV sources detected in ongoing H.E.S.S. observations of the Galactic plane, where a binary system counterpart is a plausible scenario for the TeV emission. The Suzaku data are necessary to confirm the nature of these new objects. GALACTIC POINT SOURCES 4 C PUEHLHOFER GERD NULL NULL EUR 5 AO5 TEV BINARIES: A COMMON PHENOMENON? XIS N IGR J16318-4848 247.967 -48.808 335.62953228 -0.44925356 -99 NULL NULL 405072010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052023 IGR J16318-4848 is a high mass X-ray binary with a column density of the order of 10^{24} cm^{-2}, which makes it one of the most extremely absorbed galactic objects. The absorption is strongly variable and thus mostly intrinsic to the source. The compact object (whose nature is still unknown) is deeply embedded in the stellar wind of its sgB GALACTIC POINT SOURCES 4 C BARRAGAN LAURA NULL NULL EUR 5 AO5 THE MYSTERIOUS SOURCE IGR J16318-4848 XIS N 4U 1909+07 287.7097 7.5883 41.89273161 -0.82371888 247.9131 55502.7037847222 55503.4337731482 405073010 29298.2 25000 29298.2 29298.2 0 29298.2 2 2 0 2 1 0 0 21391.1 21391.1 63051.9 0 PROCESSED 55515.2723032407 55882 55515.2869328704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052024 We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF. GALACTIC POINT SOURCES 4 A FUERST FELIX NULL NULL EUR 5 AO5 STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07 XIS Y FU ORIONIS 86.34333 9.07 197.10930446 -10.25127964 -99 NULL NULL 405074010 -99 150000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052025 Fluorescent 6.4 keV iron K alpha lines provide information on both the cool matter in the vicinity of bright X-ray sources and the sources themselves. The fluorescent line is a strong indicator of disk ionization, which is a pre-requisite for the efficient work of the magneto-rotational instability as the driver of the protostellar mass accretion process. We propose to obtain a deep Suzaku spectrum of FU Ori, the prototype of the young, strongly accreting eruptive stars called FUors. Our goal is to unambiguously detect the 6.4 keV fluorescent line and study the possible origin of the line in the circumstellar environment. Our results may provide evidence for a connection between disk ionization and accretion, supporting the role of MRI in young protostellar disks. GALACTIC POINT SOURCES 4 C ABRAHAM PETER NULL NULL EUR 5 AO5 STUDYING CIRCUMSTELLAR DISK IONIZATION IN A RAPIDLY-ACCRETING YOUNG STELLAR OBJECT VIA X-RAY FLUORESCENCE XIS N SGR 0501+4516 75.2625 45.3425 161.48747118 1.98100999 82.3996 55459.7272569444 55460.9897337963 405075010 59720.5 50000 59808.5 59812.3 0 59720.5 3 2 0 2 1 0 0 52935.7 52935.7 109065.8 0 PROCESSED 55470.1283449074 55287 55470.1458449074 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 5 AO5 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y 1RXS J1708-4009 257.2038 -40.2142 346.43162325 -0.00870489 267.1357 55466.6124074074 55467.7738425926 405076010 62810.9 60000 62818.9 62822.6 0 62810.9 3 2 0 2 1 0 0 59511.4 59511.4 100323.9 1 PROCESSED 55477.2603009259 55287 55477.2762268518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 5 AO5 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y GX 1+4 263.0071 -24.816 1.87675865 4.75818757 273.1727 55471.2801273148 55473.5140509259 405077010 99670 100000 99670.4 99670 0 99670.4 3 2 0 2 1 0 0 96525.9 96525.9 192609.1 0 PROCESSED 55487.3194444444 55287 55487.4199537037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 5 AO5 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y 4U 1538-522 235.59708 -52.38611 327.41949089 2.163702 -99 NULL NULL 405078010 -99 160000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 55287 NULL NULL NULL NULL 051232 Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donar star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star magnetic poles. In this proposal we request four, non-time constrained, 40 ks observations of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of changes of the broad band (0.1-100 keV) spectrum with respect to both binary and pulse phase. GALACTIC POINT SOURCES 4 C ROTHSCHILD RICHARD NULL NULL USA 5 AO5 THE FIRST SUZAKU OBSERVATIONS OF 4U 1538-522 HXD N GX 339-4 255.70583 -48.78961 338.93927787 -4.32641254 -99 NULL NULL 406001010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N GX 339-4 255.70583 -48.78961 338.93927787 -4.32641254 -99 NULL NULL 406001020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N GX 339-4 255.70583 -48.78961 338.93927787 -4.32641254 -99 NULL NULL 406001030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N XTE J1550-504 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 406002010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N XTE J1550-504 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 406002020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N XTE J1550-504 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 406002030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 406003010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 406003020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 406003030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 406004010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 406004020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 406004030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 406005010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 406005020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 406005030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060005 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST HXD N V4641 SGR 274.84013 -25.40717 6.77395378 -4.7890572 -99 NULL NULL 406006010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060006 We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique characteristics:1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, RXTE/ASM+PCA, MAXI and Swift/XRT+BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planed simultaneously with Swift, RXTE, many radio and optical/NIR observatories. GALACTIC POINT SOURCES 4 A YAMAOKA KAZUTAKA NULL NULL JAP 6 AO6-TOO THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR XIS N 1FGL J2339.7-0531 354.9077 -5.5469 81.34836456 -62.4702773 67.4026 55741.5915625 55743.8092361111 406007010 104091.4 100000 104091.4 104091.4 0 104099.4 2 2 0 2 1 0 0 92902.2 92902.2 191583.7 2 PROCESSED 55775.3742939815 56144 55775.4025925926 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060007 We propose to observe an unidentified Fermi source (1FGL J2339.7-0531) in the first-year Fermi catalog to search for the first ``radio-quiet'' Gamma-ray emitting millisecond pulsar. The Fermi source has a candidate X-ray counterpart from Chandra data and its X-ray and Gamma-ray properties are consistent with known Gamma-ray pulsars. This system is likely in a low-mass X-ray binary system based on optical observations. Both X-ray and optical observations show clear variability. We propose to observe the Chandra source with Suzaku to search for the possible orbital period and to study its X-ray spectrum in detail. The results will provide a better insight into the high-energy emission processes in the magnetosphere of millisecond pulsars. GALACTIC POINT SOURCES 4 A KONG ALBERT KATAOKA JUN JAP 6 AO6 REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCE XIS Y 4U1812-12 273.8053 -12.0935 18.04900466 2.37362039 267.159 55838.1400347222 55839.9168981482 406008010 62014.3 60000 62014.3 62014.3 0 62014.3 2 2 0 2 1 0 0 53544.1 53544.1 153509.9 1 PROCESSED 55858.2838194444 56226 55858.3124768518 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060012 Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state. GALACTIC POINT SOURCES 4 A SAKURAI SOKI NULL NULL JAP 6 AO6 REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU XIS Y VW HYI 62.2833 -71.2901 284.88594452 -38.13999051 181.9815 55894.1004513889 55895.1821759259 406009010 70083.4 60000 70091.4 70083.4 0 70091.4 2 2 0 2 1 0 0 64970.1 64970.1 93446.8 1 PROCESSED 55907.142025463 56274 55907.1562615741 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060023 SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 6 AO6-TOO TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE XIS Y VW HYI 62.3036 -71.2936 284.88553906 -38.13260514 212.7427 55924.6383796296 55925.1806828704 406009020 16159.3 20000 16159.3 16159.3 0 16159.3 2 2 0 2 1 0 0 13758.7 13758.7 46851.9 0 PROCESSED 55945.9016087963 56313 55945.9133912037 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060023 SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 6 AO6-TOO TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE XIS Y VW HYI 62.3086 -71.2914 284.88209314 -38.1323503 276.4367 55986.5687962963 55987.2501273148 406009030 20109.7 20000 20109.7 20109.7 0 20109.7 2 2 0 2 1 0 0 20571.2 20571.2 58857.9 1 PROCESSED 56018.9310185185 56385 56018.9417824074 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060023 SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 6 AO6-TOO TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE XIS Y VW HYI 62.29746 -71.29481 284.88814052 -38.13367962 -99 NULL NULL 406009040 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060023 SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. GALACTIC POINT SOURCES 4 B SAITOU KEI NULL NULL JAP 6 AO6-TOO TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE XIS Y AQL X-1 287.8271 0.5745 35.71381986 -4.15705073 244.5264 55852.1545486111 55853.110625 406010010 9494.8 40000 9596.8 9494.8 0 9596.8 2 1 0 1 1 0 0 35325 35325 82587.8 1 PROCESSED 55873.1044212963 56240 55873.1222337963 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060036 We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. GALACTIC POINT SOURCES 4 A YAMAOKA KAZUTAKA NULL NULL JAP 6 AO6-TOO SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE XIS Y AQL X-1 287.8264 0.5741 35.71314195 -4.15661165 244.5268 55855.5357986111 55856.4599884259 406010020 9940.6 40000 10041 9940.6 0 10041 1 1 0 1 1 0 0 37845.1 37845.1 79846 1 PROCESSED 55873.267037037 56241 55873.3025578704 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060036 We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. GALACTIC POINT SOURCES 4 A YAMAOKA KAZUTAKA NULL NULL JAP 6 AO6-TOO SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE XIS Y AQL X-1 287.8278 0.5718 35.71173466 -4.15890942 243.2618 55858.7269328704 55859.5786921296 406010030 8495 40000 8495 9538.3 0 9556.6 1 1 0 1 1 0 0 36476.8 36476.8 73581.9 2 PROCESSED 55874.1121759259 56241 55874.1380555556 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060036 We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. GALACTIC POINT SOURCES 4 A YAMAOKA KAZUTAKA NULL NULL JAP 6 AO6-TOO SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE XIS Y OAO1657-415 255.2026 -41.6667 344.36019061 0.31327103 285.9012 55830.3988425926 55832.6667939815 406011010 84729.9 80000 84733.7 84729.9 0 84741.7 2 2 0 2 1 0 0 74588.5 74588.5 195929.7 2 PROCESSED 55858.2466550926 56226 55858.2768518518 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060037 We propose Suzaku observation of accretion-powered pulsar OAO 1657-415 to study matter accretion onto the neutron star. This object is a unique high mass X-ray binary (HMXB) that shows intermediate characteristics between wind-fed accretion pulsars and disk-fed accretion pulsars. High S/N spectra obtained by XIS, HXD-PIN/GSO with short exposure time (1 ks) allow us to investigate short-time variability of physical states of the accretion column, which is close to the neutron star surface. The proposed observation also reveals the matter distribution in the HMXB by using a 6.4-keV iron fluorescence line and hard X-rays. The data at the phase of eclipse egress provide essential information about the stellar wind and atmosphere of the companion star to constrain its stellar type in question. GALACTIC POINT SOURCES 4 B ODAKA HIROKAZU NULL NULL JAP 6 AO6 WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415 XIS Y PSR J0726-2612 111.531 -26.2114 240.07877209 -4.64696128 117.9984 55881.5691782407 55882.6252546296 406012010 43757 100000 43757 43792 0 43792 2 2 0 2 1 0 0 39728.8 39728.8 91227.8 0 PROCESSED 55895.2231597222 56264 55895.2388078704 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060041 To study the origin of magnetars, a unique opportunity is provided by detecting an excess of thermal radiation in the radio pulsars which has dipolar magnetic fields as high as magnetars. The excess is caused by field decay as seen in magnetars. A question is raised whether the rotation powered pulsars can have active magnetic flux similar to magnetars. PSR J0726-2612 is a nearby (3kpc) radio pulsar with magnetic field as high as 10^13.5 G, and therefore is an ideal target. We propose 100ksec observation of this pulsar to discover magnetar-like thermal radiation, and determine the structure of the active magnetic flux tubes by phase alignment of rotational modulation of the X-ray radiation with radio pulses. GALACTIC POINT SOURCES 4 C SHIBATA SHINPEI NULL NULL JAP 6 AO6 CAN HIGH MAGNETIC FIELD RADIO PULSARS BE THE MAGNETAR ? XIS Y CYG X-1 299.5916 35.1745 71.31236822 3.05181611 279.5001 55839.9245023148 55840.9169328704 406013010 3702.7 40000 3832 3702.7 0 8031.2 1 1 0 1 1 0 0 32962.5 32962.5 85733.9 1 PROCESSED 55964.282662037 56226 55964.3073032407 2.7.16.31 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060057 We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks. GALACTIC POINT SOURCES 4 A YAMADA SHIN'YA NULL NULL JAP 6 AO6 REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS XIS Y RXJ2056.6+4940 314.1926 49.6559 89.31769097 2.74712249 241.0011 55887.7886805556 55888.5355208333 406014010 42373.1 40000 42381.1 42373.1 0 42373.1 2 2 0 2 1 0 0 44666.5 44666.5 64524 1 PROCESSED 55897.0875925926 56264 55897.0994791667 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060065 There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. GALACTIC POINT SOURCES 4 C ISO NAOKI NULL NULL JAP 6 AO6 SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART XIS Y RXJ0137.7+5814 24.46033 58.23644 129.02406462 -4.08536809 -99 NULL NULL 406015010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060065 There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. GALACTIC POINT SOURCES 4 C ISO NAOKI NULL NULL JAP 6 AO6 SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART XIS Y RXJJ0131.0+6120 22.780167 61.342639 127.67223223 -1.16334415 -99 NULL NULL 406016010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060065 There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. GALACTIC POINT SOURCES 4 C ISO NAOKI NULL NULL JAP 6 AO6 SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART XIS N 4U0114+65 19.4873 65.3067 125.69846298 2.57745686 71.642 55763.4307291667 55764.9453472222 406017010 106492.5 100000 106550.8 106558.8 0 106492.5 2 2 0 2 1 0 0 88506.1 88506.1 130821.9 1 PROCESSED 55785.0199652778 56152 55785.0443981482 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060071 We propose to observe an X-ray pulsar, 4U 0114+65 for 100 ks. This object is known to be a neutron star binary with an orbital period of 12 days and a long pulse priod of 10 ks. Our goals are to obtain time-averaged spectra of the XIS and HXD, and to quantify spectral changes between flare and quiescense phases, and to search for a cyclotron absorption line around ~ 60 keV. We also study pulse-phase resolved spectra. With these pieces of information, we aim at clarifying whether this source is a magnetar descendent or a neutron star with ordinary magnetic fields. GALACTIC POINT SOURCES 4 A SASANO MAKOTO NULL NULL JAP 6 AO6 SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIES XIS Y 1RXSJ171405.2-202747 258.52167 -20.46306 3.21688369 10.61566491 -99 NULL NULL 406018010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060085 We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 6 AO6 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ175911.0-344921 269.7922 -34.8194 356.38251758 -5.46102238 72.1205 55993.9029513889 55994.912650463 406019010 40181.3 40000 40181.3 40181.3 0 40181.3 2 2 0 2 1 0 0 34751 34751 87233.9 1 PROCESSED 56016.4702083333 56385 56016.6680787037 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060085 We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 6 AO6 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS Y 1RXSJ170047.8-314442 255.19917 -31.745 352.21410507 6.39819107 -99 NULL NULL 406020010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060085 We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 6 AO6 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 24M2791 334.9577 63.2629 106.81877019 5.23758822 230.0008 55947.3704513889 55948.0926388889 406023010 34601.7 30000 34617.7 34601.7 0 34609.7 2 2 0 2 1 0 0 35059.5 35059.5 62391.9 0 PROCESSED 55973.1002430556 56340 55973.1102893518 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060087 We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. GALACTIC POINT SOURCES 4 C OHNO MASANORI NULL NULL JAP 6 AO6 SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES XIS Y 1FGL J1715.2-3319 258.713 -33.4282 352.62684601 3.01774525 99.0737 56002.5629166667 56003.3750810185 406024010 32165 30000 32165 32165 0 32165 2 2 0 2 1 0 0 27984.8 27984.8 70166 0 PROCESSED 56019.2392013889 56386 56019.2516435185 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060087 We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. GALACTIC POINT SOURCES 4 C OHNO MASANORI NULL NULL JAP 6 AO6 SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES XIS Y 24M2216 272.27 -20.083 10.33112365 -0.1699965 -99 NULL NULL 406025010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060087 We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. GALACTIC POINT SOURCES 4 C OHNO MASANORI NULL NULL JAP 6 AO6 SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES XIS N SGR 1900+14 286.80933 9.322 43.02065561 0.7658283 -99 NULL NULL 406028010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060092 We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 6 AO6-TOO A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS HXD N AXP 1E 2259+586 345.28454 58.87903 109.08734924 -0.99573332 -99 NULL NULL 406029010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060092 We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 6 AO6-TOO A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS HXD N AXP 1RXS J1708-4009 257.20417 -40.15278 346.48106604 0.02773557 -99 NULL NULL 406030010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060092 We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 6 AO6-TOO A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS HXD N AXP 4U 0142+614 26.5682 61.7591 129.37061357 -0.42523158 40.384 55811.6552314815 55812.5731134259 406031010 38649.7 60000 38649.7 38649.7 0 38682.5 2 2 0 2 1 0 0 42196.4 42196.4 79292 0 PROCESSED 55848.166412037 56218 55851.4406828704 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060092 We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 6 AO6-TOO A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS XIS Y AXP 1E 1048.1-5937 162.53721 -59.88886 288.25965957 -0.51808465 -99 NULL NULL 406032010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060092 We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. GALACTIC POINT SOURCES 4 A NAKAGAWA YUJIN NULL NULL JAP 6 AO6-TOO A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS HXD N RS OPH 267.5535 -6.6951 19.81011082 10.37967032 94.9072 55987.2608796296 55988.855 406033010 69386 100000 69386 69386 0 69386 2 2 0 2 1 0 0 60089.9 60089.9 137719.8 0 PROCESSED 56008.3049421296 56375 56008.324224537 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060096 We propose a 100 ks observation of a recurrent novae remnant RS Ophiuchi. Using Suzaku's wide-energy coverage and excellent spectral performance, we aim to diagnose plasma and to discover non-thermal emission at a recurrent novae remnant. GALACTIC POINT SOURCES 4 C TAKEI DAI NULL NULL JAP 6 AO6 OBSERVATION OF A RECURRENT NOVA REMNANT RS OPHIUCHI XIS Y 1RXSJ013106.4+612035 22.7619 61.3591 127.66105316 -1.14841945 76.8129 55765.7032175926 55766.0182060185 406034010 13296.3 20000 13296.3 13296.3 0 13296.3 1 1 0 1 1 0 0 15882.9 15882.9 27199.9 0 PROCESSED 55784.9815740741 56374 55784.9886458333 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060097 We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. GALACTIC POINT SOURCES 4 B TAKAHASHI HIROMITSU NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES XIS Y 1RXSJ013106.4+612035 22.8032 61.3371 127.68400105 -1.16712133 215.0025 55993.5664930556 55993.889837963 406034020 12173.7 8000 12173.7 12173.7 0 12173.7 2 2 0 2 1 0 0 17897 17897 27921.9 0 PROCESSED 56008.1125231482 56374 56008.1191782407 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060097 We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. GALACTIC POINT SOURCES 4 B TAKAHASHI HIROMITSU NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES XIS Y 1RXSJ194246.3+103339 295.6976 10.5399 48.24168916 -6.37340779 280.0002 55848.1433564815 55848.635625 406035010 20488.9 20000 20488.9 20488.9 0 20488.9 3 2 0 2 1 0 0 17142 17142 42508 0 PROCESSED 55872.9892939815 56240 55873.0004861111 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060097 We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. GALACTIC POINT SOURCES 4 B TAKAHASHI HIROMITSU NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES XIS Y 1RXSJ135341.1-664002 208.4233 -66.67 309.05087215 -4.54070575 288.5314 55774.1593055556 55774.6939236111 406036010 23267.9 20000 23275.9 23267.9 0 23275.9 1 1 0 1 1 0 0 22424.1 22424.1 46183.9 0 PROCESSED 55799.4797569444 56166 55802.4628472222 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060097 We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. GALACTIC POINT SOURCES 4 B TAKAHASHI HIROMITSU NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES XIS Y HD162020 267.6611 -40.3282 350.73095661 -6.73195128 265.867 55808.0919560185 55808.4078703704 406037010 15922.9 15000 15922.9 15922.9 0 15922.9 1 1 0 1 1 0 0 15940.6 15940.6 27287.9 2 PROCESSED 55865.1100462963 56232 55865.1159953704 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y HD162020 267.6612 -40.3294 350.72995016 -6.73261971 268.3343 55816.4132291667 55816.727962963 406037020 15036.2 15000 15044.2 15044.2 0 15036.2 2 2 0 2 1 0 0 15582.9 15582.9 27183.9 0 PROCESSED 55848.161400463 56218 55851.4394444444 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y HD162020 267.6618 -40.3275 350.73183598 -6.73206134 259.9987 55824.6498958333 55825.1632407407 406037030 16230 15000 16238 16238 0 16230 2 2 0 2 1 0 0 13378.4 13378.4 44345.9 1 PROCESSED 55848.2738194444 56218 55851.4474884259 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y HD162020 267.6661 -40.3245 350.73610578 -6.73339029 259.9986 55833.0255208333 55833.4279513889 406037040 16729.7 15000 16737.7 16737.7 0 16729.7 1 1 0 1 1 0 0 15728.6 15728.6 34749.9 0 PROCESSED 55858.1306597222 56225 55858.1397453704 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y HD162020 267.6583 -40.31833 350.73847221 -6.72514943 -99 NULL NULL 406038010 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y HD162020 267.6599 -40.3316 350.72753331 -6.73286722 269.5018 55820.4672453704 55820.6918634259 406038020 8896 10000 8896 8896 0 8896 1 1 0 1 1 0 0 7851.9 7851.9 19399.9 0 PROCESSED 55848.2500810185 56218 55851.4444097222 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y HD162020 267.6631 -40.3218 350.73730077 -6.73005667 259.9987 55829.424212963 55829.6543865741 406038030 11481 10000 11481 11481 0 11481 1 1 0 1 1 0 0 8540.2 8540.2 19879.9 0 PROCESSED 55858.0724768518 56225 55858.0790162037 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061202 Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. GALACTIC POINT SOURCES 4 A PILLITTERI IGNAZIO NULL NULL USA 6 AO6 STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. XIS Y ETA CARINAE 161.2639 -59.6881 287.59810122 -0.63296206 310.0122 55766.0329398148 55766.9286226852 406039010 42030.2 50000 42030.2 42030.2 0 42030.2 1 1 0 1 1 0 0 49093.7 49093.7 77383.9 0 PROCESSED 55785.0159837963 56163 55785.0281712963 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061205 Eta Car is the nearest highly unstable extremely massive star and a key object for understanding how mass and angular momentum change as an extremely massive star heads towards hypernova. Periodic minima in X-rays and other wavebands show it as an extremely eccentric binary with a massive companion. A surprising change in the X-ray emission during the January 2009 X-ray minimum probably indicates a large-scale variation in the LBV primary's mass loss rate. We propose a Suzaku observation in AO6 to monitor the change of the absorption column in the line of sight and the non-thermal emission above 10 keV. The observation will help to study geometry of the binary orbit of Eta Car and the mechanism of the non-thermal emission. GALACTIC POINT SOURCES 4 B HAMAGUCHI KENJI NULL NULL USA 6 AO6 MONITORING DYNAMICAL MASS LOSS FROM ETA CAR WITH SUZAKU: APASTRON XIS Y GAMMA CASSIOPEIAE 14.1598 60.7356 123.56796459 -2.12972511 72.5084 55755.0038888889 55756.333587963 406040010 55394 50000 55394 55394 0 55394 2 2 0 2 1 0 0 56216.4 56216.4 114877.8 0 PROCESSED 55816.6477546296 56183 55816.6655208333 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061207 We propose a 50 ks Suzaku observation to obtain for the first time the hard X-ray spectrum of the classical Be star Gamma Cas. This star is a prototype of the "Gamma Cas stars" class, whose nature is not yet understood. Earlier XMM-Newton and Swift BAT observations gave a hint of the presence of the hard X-ray emission above 10 keV. The broadband Suzaku spectrum will allow to establish its X-ray emission mechanism - non-thermal emission or reflection of thermal emission from a neutral surface. On this basis, we will be able to discriminate the mechanisms between the magnetic disk dynamo and the accretion on a compact star. These new data will be pivotal in solving the enigma of Gamma Cas and revealing the true nature of this astrophysically important object. GALACTIC POINT SOURCES 4 C HAMAGUCHI KENJI NULL NULL USA 6 AO6 SUZAKU'S HARD LOOK AT GAMMA CASSIOPEIAE XIS Y 4 DRA 187.5655 69.216 125.72551845 47.79722512 145.5318 55874.1707291667 55875.0619328704 406041010 42258 40000 42258 42258 0 42258 2 2 0 2 1 0 0 39792.5 39792.5 76998 2 PROCESSED 55890.4815972222 56260 55890.6961458333 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061212 4 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 6 AO6 A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTION XIS Y V1082 SGR 286.8363 -20.7721 15.88147607 -12.67535412 81.3818 56009.1848148148 56010.4459375 406042010 39460.5 40000 39460.5 39460.5 0 39460.5 2 2 0 2 1 0 0 36017.1 36017.1 108924 2 PROCESSED 56023.1382986111 88068 56023.1564236111 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061217 V1082 Sgr is a BAT-detected cataclysmic variable with a 20 hr orbital period that exhibits high and low states. The high X-ray luminosity and the presence of the HeII 4686 lines in its optical spectrum have led to the suggestion that this is an intermediate polar (IP). We propose an exploratory 40 ks Suzaku observation with the aim of establishing if it is indeed an IP. If it is, then this system may provide a unique opportunity to study an IP in a low state, which has not been possible with other IPs. GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 6 AO6 AN UNUSUAL BAT-DETECTED CATACLYSMIC VARIABLE, V1082 SGR XIS Y AQL X-1 287.81687 0.58494 35.71842844 -4.14317601 -99 NULL NULL 406043010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061221 Long term optical/X-ray monitoring of X-ray binaries has revealed that the accretion flow pattern can be remarkably different during different outbursts of the same source, challenging standard disk-instability models. Of particular interest is the Low-Intensity State (LIS) in Aql X-1, where the optical-to-X-ray flux ratio is about a factor of 7 higher than that during normal outbursts explainable using the disk-instability model. Suzaku data, along with contemporaneous optical/IR and radio observations, will allow probing the nature of accretion flow in the LIS of Aql X-1. We request a 100 ksec ToO observation of Aql X-1 during a LIS to achieve our science goals. The observation will test the predictions of ADIOS models and constrain disk-jet coupling. GALACTIC POINT SOURCES 4 A MAITRA DIPANKAR NULL NULL USA 6 AO6-TOO SUZAKU OBSERVATIONS OF AQUILA X-1 DURING ITS LOW-INTENSITY STATE XIS N SERPENS X-1 279.98958 5.03583 36.11795416 4.84231882 -99 NULL NULL 406044010 -99 250000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061222 Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries. Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects at the inner accretion disk. But, the nature of these lines is still hotly debated. Recent work has suggested that pile-up can artificially broaden lines, while several narrow lines have been claimed in one source. To address these critical issues, we propose Suzaku and Chandra observations of Serpens X-1. Fast clocking modes will be used to achieve pile-up free spectra. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe line, while the high-resolution gratings spectra from Chandra will reveal any narrow components. GALACTIC POINT SOURCES 4 C MILLER JON NULL NULL USA 6 AO6 THE NATURE OF BROAD FE K EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES XIS N 4U 1624-490 247.01179 -49.1985 334.91501997 -0.26313779 -99 NULL NULL 406045010 -99 75000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061223 We propose a 75~ks (on-source, 165~ks total) Suzaku observation of the ``Big Dipper'' 4U~1624-490 to facilitate four important science goals: (1) determine the origin(s) of the persistent X-ray emission, (2) the properties and evolution of the obscuration local to 4U 1624-490, (3) study its broad Fe line properties to determine origin and possibly source geometry, and (4) a large angle scattering study of the X-ray halo to diagnose ISM grain properties (the line-of-sight position, size distribution and density of grains) near us in complement with our work with Chandra on halo studies at small angles to determine grain properties near the source. GALACTIC POINT SOURCES 4 C XIANG JINGEN NULL NULL USA 6 AO6 A SUZAKU STUDY OF THE BIG DIPPER 4U 1624-490, AND ITS SCATTERING HALO XIS N 4U 1954+31 298.9334 32.0803 68.38077131 1.91321277 261.2562 55857.3373263889 55858.7203009259 406046010 60216 60000 60224 60232 0 60216 3 2 0 2 1 0 0 57900.8 57900.8 119467.9 0 PROCESSED 55874.0883796296 56241 55874.1069328704 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061226 We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 6 AO6 THE SLOWEST ROTATING PULSAR 4U 1954+31 XIS Y 4U1538-522 235.59708 -52.38611 327.41949089 2.163702 -99 NULL NULL 406047010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061232 Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star magnetic poles. In this proposal we request a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of changes of the broad band (0.1 -- 100 keV) spectrum with respect to both binary and pulse phases. GALACTIC POINT SOURCES 4 C ROTHSCHILD RICHARD NULL NULL USA 6 AO6 THE FIRST SUZAKU OBSERVATION OF 4U 1538-522 XIS Y 4U 0115+63 19.6209 63.7559 125.91670035 1.04099954 84.7167 55747.0027430556 55748.0529976852 406048010 24279 50000 24280 24279 0 24283.9 2 2 0 2 1 0 0 45127.2 45127.2 90727.9 1 PROCESSED 55777.2688657407 56163 55778.4298611111 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS Y 4U 0115+63 19.6139 63.7554 125.91367385 1.04017806 82.1235 55750.053587963 55751.0210763889 406049010 42274.8 45000 42274.8 42354.8 0 42354.8 2 2 0 2 1 0 0 42143.2 42143.2 83577.9 1 PROCESSED 55777.3219791667 56163 55778.4311226852 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS Y CEP X-4 324.878 56.98611 99.01219478 3.31239245 -99 NULL NULL 406050010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N CEP X-4 324.878 56.98611 99.01219478 3.31239245 -99 NULL NULL 406051010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N XTE J1946+274 296.41371 27.36539 63.20701539 1.39576569 -99 NULL NULL 406052010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N XTE J1946+274 296.41371 27.36539 63.20701539 1.39576569 -99 NULL NULL 406053010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N V 0332+53 53.7495 53.17319 146.05199466 -2.19402959 -99 NULL NULL 406054010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N V 0332+53 53.7495 53.17319 146.05199466 -2.19402959 -99 NULL NULL 406055010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N MXB 0656-072 104.57 -7.2105 220.12826569 -1.76940259 -99 NULL NULL 406056010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N MXB 0656-072 104.57 -7.2105 220.12826569 -1.76940259 -99 NULL NULL 406057010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061234 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N 2S 1417-62 215.30333 -62.69833 313.02106782 -1.59841182 -99 NULL NULL 406058010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061235 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N GS 1843-02 282.07375 -2.42028 30.41972107 -0.40463814 -99 NULL NULL 406059010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061235 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N GX 304-1 195.3153 -61.5986 304.10001953 1.25086712 115.9338 55957.437037037 55959.1669444444 406060010 16524.3 65000 16691.2 16524.3 0 16691.2 2 2 0 2 1 0 0 58712.4 58712.4 149432.1 3 PROCESSED 56033.2457407407 88068 56033.2695023148 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061235 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS Y SAX J2103.5+4545 315.89879 45.75153 87.13025662 -0.68481282 -99 NULL NULL 406061010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061235 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N LSV +44 17 70.24717 44.53036 159.84706366 -1.27003263 -99 NULL NULL 406062010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061235 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 6 AO6-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 406063010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061241 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 6 AO6-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N 4U 1543-47 236.78583 -47.66944 330.91865964 5.42579106 -99 NULL NULL 406064010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061241 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 6 AO6-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N XTE J1118+480 169.54542 48.03694 157.66026546 62.32060029 -99 NULL NULL 406065010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061241 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 6 AO6-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N V404 CYG 306.01596 33.86728 73.11883543 -2.09143677 -99 NULL NULL 406066010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061241 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 6 AO6-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N A 0620-00 95.68542 -0.34583 209.95635423 -6.53992625 -99 NULL NULL 406067010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061241 Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 6 AO6-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N GRS 1915+105 288.79833 10.94556 45.36563993 -0.21936861 -99 NULL NULL 406068010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061242 We propose a 100 ks ToO to observe a soft state of GRS 1915+105 at L<30% L Edd. This ToO will address several important science goals: (1) a measurement of the black hole spin via two independent methods (X-ray continuum fitting and broad iron line analysis), (2) the determination of the accretion disk-corona geometry via studies of fluorescence lines and Compton reflection components, and (3) investigation of the broad-band spectrum for input into photoionization models. GALACTIC POINT SOURCES 4 A LEE JULIA NULL NULL USA 6 AO6-TOO MEASURING THE GRS 1915+105 BLACK HOLE SPIN AND BROADBAND CONTINUUM PROPERTIES XIS Y SGR 1806-20 272.1607 -20.4008 10.00344249 -0.23433657 89.0334 56010.449837963 56012.5314814815 406069010 70596.4 70000 70596.4 70596.4 0 70596.4 2 2 0 2 1 0 0 63957.1 63957.1 179827.9 2 PROCESSED 56023.2183101852 88068 56023.2387384259 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061301 Recent Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic ages. The hard X-rays of magnetars become weaker but harder for older objects. In order to accomplish this picture, we have to verify that this correlation is rather free from selection effects, and holds even when the sources vary on long time scales. Here we propose a 70 ks observation of SGR 1806-20. If we detect the hard X-rays from this source at a rather intensity, the above correlation will be much reinforced. GALACTIC POINT SOURCES 4 C ENOTO TERUAKI NULL NULL USA 6 AO6 VARIABILITY OF HARD X-RAYS FROM MAGNETARS XIS Y GX 17+2 274.0108 -14.0482 16.42401351 1.2676957 264.7715 55853.116099537 55855.5287037037 406070010 6506.9 100000 6757.2 6506.9 0 6757.2 3 2 0 2 1 0 0 87359.9 87359.9 208429.7 3 PROCESSED 55873.2590509259 56241 55873.2944444445 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062003 The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique. GALACTIC POINT SOURCES 4 A CACKETT EDWARD NULL NULL EUR 6 AO6 EXPLORING THE IRON LINE - KHZ QPO CONNECTION XIS Y 4U 1543-624 236.9719 -62.5774 321.74901084 -6.34183385 299.1939 55826.4056828704 55827.6217592593 406072010 49185.1 50000 49193.1 49185.1 0 49201.1 2 2 0 2 1 0 0 45309.4 45309.4 105059.9 1 PROCESSED 55848.3822916667 56222 55851.4556134259 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062010 We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results. GALACTIC POINT SOURCES 4 A MADEJ OLIWIA NULL NULL EUR 6 AO6 INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624 XIS Y AX J1818.8-1559 274.7184 -16.0002 15.02984997 -0.2600064 265.8517 55849.5538888889 55852.1474537037 406074010 95191.2 100000 99385.9 99385.9 0 95191.2 2 2 0 2 1 0 0 83874.6 83874.6 224069.9 1 PROCESSED 55873.9578819445 56241 55873.993599537 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062016 The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidates GALACTIC POINT SOURCES 4 B MEREGHETTI SANDRO NULL NULL EUR 6 AO6 A NEW GALACTIC MAGNETAR CANDIDATE XIS Y IGR J07193-1233 109.83 -12.556 227.26135569 0.36077082 -99 NULL NULL 406075010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 062017 The soft gamma repeaters (SGRs) and the Anomalous X-ray pulsars (AXPs) constitute a small class of X-ray sources which are currently believed to host an ultra-magnetized neutron star, or magnetar. Catching new candidates and enlarge the sample of these peculiar objects is vital in two main respects: i) it allows to test further current models for their activity and ii) it will shed light on the (evolutionary) links among magnetars and other classes of isolated neutron stars. The aim of this proposal is to observe with Suzaku the most promising magnetar candidate, IGR J07193-1233, selected among a large number of still unidentified INTEGRAL sources. GALACTIC POINT SOURCES 4 C PAVAN LUCIA NULL NULL EUR 6 AO6 CATCHING MAGNETAR CANDIDATES AMONG UNIDENTIFIED INTEGRAL SOURCES WITH SUZAKU XIS N 4U 1705-44 257.2257 -44.096 343.32512852 -2.33758895 104.9955 56013.5320486111 56016.4231134259 406076010 100811.2 100000 100811.2 100819.2 0 100820.9 2 2 0 2 1 0 0 90075.9 90075.9 249767.7 2 PROCESSED 56027.1700462963 88068 56027.2013657407 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062019 We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system. GALACTIC POINT SOURCES 4 A DI SALVO TIZIANA NULL NULL EUR 6 AO6-TOO SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE XIS Y 4U 0614+091 94.28042 9.13694 200.87736381 -3.36351731 -99 NULL NULL 406077010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 067090 We propose an investigation of the jet from the ultracompact X-ray binary (UCXB) 4U 0614+091 with Suzaku. 4U 0614+091 is one of the 13 UCXBs whose orbital periods (< 1 hour) are determined. By analogy with microquasars, the spectral state of UCXBs would be low/hard, and there is a possibility that UCXBs have jets. Signs of the existence of the jet in 4U 0614+091 from radio and infrared observations are already reported. Existence of the jet can be recognized by a high-sensitivity spectroscopy of the hard X-ray tailing component. If this component is thermal radiation, the origin would be corona with a high temperature. If this is non-thermal radiation, the origin would be the jet. The wide-band observation with Suzaku will clarify what actually happens in the UCXB. GALACTIC POINT SOURCES 4 C SATO TAMOTSU MADEJ OLIWIA JAP 6 AO6 SUZAKU OBSERVATION OF THE JET FROM THE ULTRACOMPACT X-RAY BINARY 4U 0614+091 XIS N IGRJ16479-4514 252.0242 -45.1934 340.16807688 -0.11668459 91.5317 55980.9438194444 55983.5363541667 406078010 149778.5 150000 149786.5 149778.5 0 149786.5 2 2 0 2 1 0 0 154729.5 154729.5 223981.9 0 PROCESSED 56062.2569675926 88068 56062.2788425926 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 068014 We propose a 100 ks observation of the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period, the eclipsing IGRJ16479-4514 (3.3 d), with the main aim of probing its X-ray properties along one entire orbital phase with unprecedented sensitivity. The requested net exposure time indeed translates into an observation almost continuously spanning the whole binary system orbit, allowing for the first time an orbital phase resolved investigation of the X-ray emission properties, which will allow us to study the structure of the supergiant companion (its density and ionization state) and to cast light on the outburst mechanism at work in this new class of transients. GALACTIC POINT SOURCES 4 A SIDOLI LARA BODAGHEE ARASH EUS 6 AO6 UNVEILING THE MYSTERY OF THE SUPERGIANT FAST X-RAY TRANSIENT WITH THE SHORTEST ORBITAL PERIOD XIS Y CYG X-1 299.59033 35.20161 71.33499876 3.06682766 -99 NULL NULL 407001010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N CYG X-1 299.59033 35.20161 71.33499876 3.06682766 -99 NULL NULL 407001020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N CYG X-1 299.59033 35.20161 71.33499876 3.06682766 -99 NULL NULL 407001030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 407002010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 407002020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO REIS RUBENS JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N XTE J1550-564 237.74458 -56.47667 325.88223339 -1.82706287 -99 NULL NULL 407002030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 407003010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 407003020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N GRO J1655-40 253.5 -39.84581 344.98161118 2.45630442 -99 NULL NULL 407003030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 407004010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 407004020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N X1630-472 248.50458 -47.39289 336.91037296 0.25136454 -99 NULL NULL 407004030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 407005010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 407005020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N H1743-322 266.25833 -32.22667 357.12592965 -1.60785557 -99 NULL NULL 407005030 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070002 Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. GALACTIC POINT SOURCES 4 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7-TOO MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST XIS N NQ GEM 112.97717 24.50306 194.63349275 19.35254552 -99 NULL NULL 407006010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 070021 Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects. GALACTIC POINT SOURCES 4 C EZE ROMANUS NULL NULL JAP 7 AO7 SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS XIS N HEN 3-461 159.78625 -51.40347 282.90464688 6.25005811 -99 NULL NULL 407007010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 070021 Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects. GALACTIC POINT SOURCES 4 C EZE ROMANUS NULL NULL JAP 7 AO7 SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS XIS N MRK 520 330.17242 10.55219 69.39248442 -34.0304333 -99 NULL NULL 407014010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070028 Compton-thick AGNs contribute to the hard X-ray background and are key objects for investigating the cosmological evolution of AGNs. But heavy obscuration under 10 keV, and source misidentification mean that very few sources have been studied in detail. We have developed new infrared and hard X-ray diagnostics of AGN identification, based on which we select one candidate, Mrk 520, which must be very highly obscured and likely Compton-thick. With Suzaku, we will characterize all emission components, not only thermal and scattering components under 10 keV, but also the heavily obscured continuum over 10 keV, and reflection components. GALACTIC POINT SOURCES 4 C MATSUTA KEIKO NULL NULL JAP 7 AO7 MRK 520 : A NEW COMPTON-THICK AGN? XIS N CYG X-1 299.59071 35.18919 71.32454476 3.06009128 -99 NULL NULL 407015010 -99 85000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070030 We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes. GALACTIC POINT SOURCES 4 A YAMADA SHINYA NULL NULL JAP 7 AO7 INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 XIS N Z CAM 126.305 73.11089 141.38213775 32.62862284 -99 NULL NULL 407016010 -99 35000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070038 Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases. GALACTIC POINT SOURCES 4 C SAITOU KEI NULL NULL JAP 7 AO7 COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE XIS N V4641 SGR 274.84013 -25.40717 6.77395378 -4.7890572 -99 NULL NULL 407017010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070041 We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics: 1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, MAXI/GSC, Swift/XRT and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planned simultaneously with Swift, many radio and optical/NIR observatories. GALACTIC POINT SOURCES 4 A YAMAOKA KAZUTAKA NULL NULL JAP 7 AO7-TOO THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR XIS N AX J1622.1-5005 245.53333 -50.095 333.60475648 -0.20613936 -99 NULL NULL 407018010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070043 Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 7 AO7 ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? XIS N AX J1846.8-0240 281.7182 -2.6613 30.04319345 -0.19850989 89.4057 56018.0125115741 56019.1146990741 407019010 37620.9 40000 37620.9 41612.7 0 39220.7 2 2 0 2 1 0 0 37250 37250 95219.9 0 PROCESSED 56033.2221412037 88068 56033.2323032407 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070043 Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 7 AO7 ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? XIS Y AX J1620.7-4942 245.19583 -49.71278 333.72073134 0.21799808 -99 NULL NULL 407020010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070043 Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 7 AO7 ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? XIS N AX J1445.7-5931 221.44583 -59.53167 316.97324327 0.186216 -99 NULL NULL 407021010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070043 Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. GALACTIC POINT SOURCES 4 A MAKISHIMA KAZUO NULL NULL JAP 7 AO7 ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? XIS N 1FGL J0747.4-3303 116.88879 -33.092 248.37397684 -3.91098782 -99 NULL NULL 407022010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070051 We propose to observe two of Fermi/LAT unassociated sourced from 2-year catalog which are located on the Galactic Plane. These two sources are bright in gamma-ray energies and well localized but no counterpart in other wavelength is known so far. We expect to determine which gamma-ray source category the proposed targets belong to, from X-ray morphological and spectral characteristics to be obtained. It will be more interesting that the objects look like known categories since it might mean a discovery of a new class of gamma-ray sources. We hope to promote systematic understandings for the gamma-ray objects in the Galactic Plane. GALACTIC POINT SOURCES 4 C NAKAMORI TAKESHI NULL NULL JAP 7 AO7 SEARCH FOR X-RAY COUNTERPARTS FOR FERMI/LAT UNASSOCIATED SOURCES ON THE GALACTIC PLANE XIS N 1RXSJ171405.2-202747 258.52167 -20.46306 3.21688369 10.61566491 -99 NULL NULL 407024010 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ171757.8-332837 259.49083 -33.47694 352.96308376 2.46029803 -99 NULL NULL 407025010 -99 12000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ175219.2-190727 268.08 -19.12417 9.20798372 3.73361636 -99 NULL NULL 407026010 -99 12000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ170047.8-314442 255.19917 -31.745 352.21410507 6.39819107 -99 NULL NULL 407027010 -99 12000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ182853.8-241746 277.22417 -24.29611 8.76534346 -6.19787712 -99 NULL NULL 407028010 -99 12000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ173905.2-392615 264.77167 -39.4375 350.34867934 -4.37314858 -99 NULL NULL 407029010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N 1RXSJ171542.3-243131 258.92625 -24.52528 0.04342141 8.00113057 -99 NULL NULL 407030010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070052 We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. GALACTIC POINT SOURCES 4 C MORI HIDEYUKI NULL NULL JAP 7 AO7 SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE XIS N LS 5039 276.56275 -14.84842 16.88157018 -1.28923077 -99 NULL NULL 407033010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070062 We propose a 200 ks observation of the gamma-ray binary LS 5039 with Suzaku. Our main aim is to search for pulsation from its compact object. Our analysis of past X-ray data suggests pulsation with parameters typical of magnetars. Addition of new Suzaku data will allow us to confirm the suggested pulsation. If confirmed, the discovery is important both for gamma-ray binary science and for magnetar science. Another aim of the proposed observation is to investigate stability of the X-ray flux and spectral property at each orbital phase. We are particularly interested in testing stability of hour-scale lightcurve structures. New Suzaku data, in combination with the previous data, should provide important clues to understand the emission mechanism. GALACTIC POINT SOURCES 4 C TAKAHASHI TADAYUKI NULL NULL JAP 7 AO7 REVEALING THE NATURE OF THE COMPACT OBJECT IN LS 5039 XIS N U GEM IN QUIECSECNCE 118.77183 22.00142 199.22315443 23.3945234 -99 NULL NULL 407034010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070065 It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. GALACTIC POINT SOURCES 4 B HAYASHI TAKAYUKI NULL NULL JAP 7 AO7-TOO OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST XIS Y U GEM IN OUTBURST 118.7732 21.9928 199.23241259 23.39259554 281.117 56029.4105324074 56030.750162037 407035010 50254.7 50000 50254.7 50254.7 0 50254.7 2 2 0 2 1 0 0 47296.7 47296.7 115707.9 1 PROCESSED 56044.3683101852 88068 56044.3887731482 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070065 It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. GALACTIC POINT SOURCES 4 B HAYASHI TAKAYUKI NULL NULL JAP 7 AO7-TOO OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST XIS Y SWIFT J1922.7-1716 290.692 -17.283 20.69989276 -14.55317706 -99 NULL NULL 407036010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070077 This proposal aims at a 60 ksec pointing (non time critical) onto the LMXB, Swift J1922.7-1716, which is considered to reside in the hard state. The purpose is to obtain a wide-band spectrum of this object with the XIS, HXD-PIN, and HXD-GSO. The XIS data will allow us to estimate the blackbody radius which underlies the expected Compton hard continuum, while the HXD data can be used to study an enigmatic spectral feature at ~40 keV often seen in this type of sources. Although the source is considered to be relatively bright, the XIS data are expected to be free from pile-up effects. GALACTIC POINT SOURCES 4 C SAKURAI SOKI NULL NULL JAP 7 AO7 SUZAKU STUDY OF LOW-MAGNETIC-FIELD NEUTRON STARS VIA THE HARD STATE OF LMXBS XIS N IGR J17091-3624 257.28333 -36.40667 349.52594917 2.21189442 -99 NULL NULL 407037010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070097 We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate. GALACTIC POINT SOURCES 4 B YAMAOKA KAZUTAKA NULL NULL JAP 7 AO7 SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 XIS N II PEG 358.76667 28.63367 108.23244051 -32.62392433 -99 NULL NULL 407038010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070102 We propose a Suzaku observation of the powerful flare star II Peg with the high sensitivity of HXD. MAXI/GSC results from 2009 to 2011 show that this source exhibits the highest flaring activity with the largest luminosities and the largest fluxes. Then detection of the non-thermal emission is the most expected from this source at the on-set of a flare. We are to observe this target simultaneously with radio, infrared, optical, and X-ray bands for the first time. Our goal is (1) to detect impulsive non-thermal emission at the powerful II Peg flare (2) to obtain wide-band SED variability from radio to hard X-ray band, and (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. GALACTIC POINT SOURCES 4 C TSUBOI YOHKO NULL NULL JAP 7 AO7 NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEG XIS N EUVE J1439 +75.0 220.02163 75.09272 114.09811948 40.11634493 -99 NULL NULL 407039010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070112 The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. GALACTIC POINT SOURCES 4 B HARAYAMA ATSUSHI NULL NULL JAP 7 AO7 SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS XIS Y PG 1658 +440 254.95183 44.01775 69.12302307 38.05451186 -99 NULL NULL 407040010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070112 The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. GALACTIC POINT SOURCES 4 B HARAYAMA ATSUSHI NULL NULL JAP 7 AO7 SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS XIS N WR140 305.11667 43.85444 80.930231 4.1770017 -99 NULL NULL 407041010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071203 In the campaign observations of the prototypical colliding wind binary system WR 140 at its last periastron passage in 2009, Suzaku discovered an extremely hard and variable X-ray component. The current best explanation of its origin is inverse-Compton cooling of particles accelerated in the wind-wind collision shock, and if so this would be the first detection of non-thermal X-ray emission from any Wolf-Rayet system. However, other mechanisms cannot be excluded because the observed intensity was stronger than expected from the observed radio luminosity. We propose to re-observe WR 140 near apastron in 2012 with Suzaku to identify the emission mechanism which produces the hard component. GALACTIC POINT SOURCES 4 C HAMAGUCHI KENJI NULL NULL USA 7 AO7 MEASURING EXTREMELY HARD X-RAY EMISSION FROM WR140 AT APASTRON XIS N HEN 3-1591 271.88342 -25.89536 5.07306413 -2.67684889 -99 NULL NULL 407042010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071211 The number of symbiotic stars known to be medium energy (2-10 keV) X-ray emitters has increased markedly in the last several years. These are white dwarfs accreting from a giant mass donor, unlike the less common class of symbiotic X-ray binaries in which the accretor is a neutron star. The X-ray spectra of the white dwarf symbiotics can be used to constrain the white dwarf mass and accretion rate. Here we focus on one object, Hen 3-1591, which belongs to a rare subclass of d'-type yellow symbiotic, commonly thought to harbor a young white dwarf. Hen 3-1591 is the first of this subclass to show medium energy X-ray emission, and hence we propose a moderately deep Suzaku observation to characterize its white dwarf and the circum-binary environment. GALACTIC POINT SOURCES 4 B MUKAI KOJI NULL NULL USA 7 AO7 THE X-RAY EMISSION OF THE YELLOW SYMBIOTIC STAR, HEN 3-1591 XIS N CH UMA 151.75287 67.54647 142.89508741 42.65158931 -99 NULL NULL 407043010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071212 The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? GALACTIC POINT SOURCES 4 A MUKAI KOJI NULL NULL USA 7 AO7 DWARF NOVAE WITH EXTREME WHITE DWARF MASSES XIS Y EK TRA 228.50375 -65.09306 317.22568595 -6.25656218 -99 NULL NULL 407044010 -99 70000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071212 The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? GALACTIC POINT SOURCES 4 A MUKAI KOJI NULL NULL USA 7 AO7 DWARF NOVAE WITH EXTREME WHITE DWARF MASSES XIS N BF ERI 69.87475 -4.59961 201.03990907 -31.30067574 -99 NULL NULL 407045010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071212 The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 7 AO7 DWARF NOVAE WITH EXTREME WHITE DWARF MASSES XIS N AT ARA 262.64079 -46.09947 343.85518736 -6.61951744 -99 NULL NULL 407046010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071212 The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 7 AO7 DWARF NOVAE WITH EXTREME WHITE DWARF MASSES XIS N BV CEN 202.83117 -54.97597 308.68415273 7.44968026 -99 NULL NULL 407047010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071212 The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? GALACTIC POINT SOURCES 4 C MUKAI KOJI NULL NULL USA 7 AO7 DWARF NOVAE WITH EXTREME WHITE DWARF MASSES XIS N T PYXIDIS 136.17292 -32.37986 257.20715673 9.70672304 -99 NULL NULL 407048010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071213 We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins. GALACTIC POINT SOURCES 4 C TAKEI DAI NULL NULL USA 7 AO7 COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTS XIS N AQL X-1 287.81687 0.58494 35.71842844 -4.14317601 -99 NULL NULL 407049010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071221 Long term optical/X-ray monitoring of X-ray binaries has revealed that the accretion flow pattern can be remarkably different during different outbursts of the same source, challenging standard disk-instability models. Of particular interest is the Low-Intensity State (LIS) in Aql X-1, where the optical-to-X-ray flux ratio is about a factor of 8 higher than that during normal outbursts explainable using the disk-instability model. Suzaku data, along with contemporaneous optical/IR and radio observations, will allow probing the nature of accretion flow in the LIS of Aql X-1. We request a 100 ksec ToO observation of Aql X-1 during a LIS to achieve our science goals. The observation will test the predictions of ADIOS models and constrain disk--jet coupling. GALACTIC POINT SOURCES 4 A MAITRA DIPANKAR NULL NULL USA 7 AO7-TOO SUZAKU OBSERVATION OF AQUILA X-1 DURING ITS LOW-INTENSITY STATE XIS N SERPENS X-1 279.98983 5.036 36.1182193 4.84217349 -99 NULL NULL 407050010 -99 250000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071222 Much recent work has been focused on Fe Kalpha emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the neutron star LMXB, Serpens X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe Kalpha line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe Kalpha GALACTIC POINT SOURCES 4 C CACKETT EDWARD NULL NULL USA 7 AO7 THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES XIS N HERCULES X-1 254.45763 35.34239 58.14908153 37.52297277 -99 NULL NULL 407051010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071224 This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. GALACTIC POINT SOURCES 4 B GREFENSTETTE BRIAN NULL NULL USA 7 AO7 STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY XIS N HERCULES X-1 254.45763 35.34239 58.14908153 37.52297277 -99 NULL NULL 407051020 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071224 This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. GALACTIC POINT SOURCES 4 B GREFENSTETTE BRIAN NULL NULL USA 7 AO7 STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY XIS N HERCULES X-1 254.45763 35.34239 58.14908153 37.52297277 -99 NULL NULL 407051030 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071224 This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. GALACTIC POINT SOURCES 4 B GREFENSTETTE BRIAN NULL NULL USA 7 AO7 STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY XIS N GX 1+4 263.009 -24.74561 1.93703286 4.79492907 -99 NULL NULL 407052010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071225 We propose to observe GX 1+4 during/after a torque reversal with SUZAKU, as a Target Of Opportunity. The pulse period shows the largest known change in time, with an energy spectrum unusually hard and strong suggestions of having the highest magnetic field of any accreting pulsar. Fermi/GBM monitoring will notify of GX 1+4 changing its current spin-down state. SUZAKU will then measure, for the first time, a detailed wide-band energy spectrum of the source during spin-up. This measurement will provide a unique insight into an event in which the physical mechanism(s) is(are) still poorly understood, in part due to the lack of wide-band spectral studies with sufficient energy resolution during torque reversals. Optical/IR ToO observations from the REM telescope (Chile) will be also triggered. GALACTIC POINT SOURCES 4 A CAMERO-ARRANZ ASCENSION NULL NULL USA 7 AO7-TOO TOO OBSERVATIONS OF THE NEUTRON STAR / RED GIANT BINARY SYSTEM GX 1+4 / V2116 OPHIUCHI XIS N 4U 0115+63 19.63292 63.74 125.92365665 1.02574493 -99 NULL NULL 407053010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N 4U 0115+63 19.63292 63.74 125.92365665 1.02574493 -99 NULL NULL 407054010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N CEP X-4 324.878 56.98611 99.01219478 3.31239245 -99 NULL NULL 407055010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N CEP X-4 324.878 56.98611 99.01219478 3.31239245 -99 NULL NULL 407056010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N XTE J1946+274 296.41371 27.36539 63.20701539 1.39576569 -99 NULL NULL 407057010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N XTE J1946+274 296.41371 27.36539 63.20701539 1.39576569 -99 NULL NULL 407058010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N V 0332+53 53.7495 53.17319 146.05199466 -2.19402959 -99 NULL NULL 407059010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N V 0332+53 53.7495 53.17319 146.05199466 -2.19402959 -99 NULL NULL 407060010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N MXB 0656-072 104.57 -7.2105 220.12826569 -1.76940259 -99 NULL NULL 407061010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N MXB 0656-072 104.57 -7.2105 220.12826569 -1.76940259 -99 NULL NULL 407062010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071231 We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD XIS N 2S 1417-62 215.30333 -62.69833 313.02106782 -1.59841182 -99 NULL NULL 407063010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071232 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N KS 1947+300 297.39787 30.20883 66.09899527 2.08357456 -99 NULL NULL 407064010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071232 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N SWIFT J1626.6-5156 246.651 -51.94264 332.7799243 -2.00275201 -99 NULL NULL 407065010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071232 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N SAX J2103.5+4545 315.89879 45.75153 87.13025662 -0.68481282 -99 NULL NULL 407066010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071232 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N LSV +44 17 70.24717 44.53036 159.84706366 -1.27003263 -99 NULL NULL 407067010 -99 65000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071232 We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. GALACTIC POINT SOURCES 4 A POTTSCHMIDT KATJA NULL NULL USA 7 AO7-TOO CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES XIS N 4U1538-522 235.59708 -52.38611 327.41949089 2.163702 -99 NULL NULL 407068010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071233 Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit. GALACTIC POINT SOURCES 4 A ROTHSCHILD RICHARD NULL NULL USA 7 AO7 THE FIRST SUZAKU OBSERVATION OF 4U1538-522 XIS N 1FGL J1018.6-5856 154.73175 -58.94614 284.35188181 -1.6900659 -99 NULL NULL 407069010 -99 70000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071234 We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. GALACTIC POINT SOURCES 4 B TANAKA TAKAAKI NULL NULL USA 7 AO7 SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 XIS N 1FGL J1018.6-5856 154.73175 -58.94614 284.35188181 -1.6900659 -99 NULL NULL 407070010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071234 We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. GALACTIC POINT SOURCES 4 B TANAKA TAKAAKI NULL NULL USA 7 AO7 SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 XIS N 1FGL J1018.6-5856 154.73175 -58.94614 284.35188181 -1.6900659 -99 NULL NULL 407071010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071234 We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. GALACTIC POINT SOURCES 4 B TANAKA TAKAAKI NULL NULL USA 7 AO7 SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 XIS N CYGNUS X-1 299.59042 35.20167 71.33508842 3.06679615 -99 NULL NULL 407072010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071241 We propose for a single 30 ks observation of the accreting black hole Cygnus X-1. NuSTAR is an upcoming (to be launched in Spring 2012) hard X-ray (5-80 keV) mission that will plan its schedule to obtain simultaneous coverage of Cyg X-1 with Suzaku. The observations will be used for both science and cross-calibration. The combination of Suzaku and NuSTAR will provide the best measurement of the reflection component, including a relativistically broadened iron line and a hard X-ray excess, and the information will be used to test emission models and constrain the Cyg X-1 accretion geometry. The XIS capabilities to measure the iron line are essential for the science, and the HXD coverage is essential for the cross-calibration. GALACTIC POINT SOURCES 4 A TOMSICK JOHN NULL NULL USA 7 AO7 CYGNUS X-1 WITH SUZAKU AND NUSTAR XIS N XTE J1118+48 169.54542 48.03694 157.66026546 62.32060029 -99 NULL NULL 407073010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071243 It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. GALACTIC POINT SOURCES 4 A REIS RUBENS NULL NULL USA 7 AO7-TOO UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS XIS N XTE J1550-564 237.74458 -56.47669 325.88222081 -1.82707843 -99 NULL NULL 407074010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071243 It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. GALACTIC POINT SOURCES 4 A REIS RUBENS NULL NULL USA 7 AO7-TOO UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS XIS N XTE J1650-500 252.504 -49.96211 336.71823399 -3.42702607 -99 NULL NULL 407075010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071243 It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. GALACTIC POINT SOURCES 4 A REIS RUBENS NULL NULL USA 7 AO7-TOO UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS XIS N XTE J1817-330 274.43142 -33.01881 359.81724224 -7.99556497 -99 NULL NULL 407076010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071243 It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. GALACTIC POINT SOURCES 4 A REIS RUBENS NULL NULL USA 7 AO7-TOO UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS XIS N 4U 1755-33 269.666 -33.8075 357.21517442 -4.87185587 -99 NULL NULL 407077010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071243 It has long been known that black hole binaries display distinct spectral states. However, the driving mechanism behind the state transition is still a matter of much debate. The importance of Suzaku in the study of black hole binaries cannot be overemphasised; with a single 40ks Suzaku observation of XTE J1752 223, we found that state transition is not a manifestation of a change in the inner extent of the accretion disk; we confirmed the black hole nature of the central source; and constrained its spin parameter. Here, we propose to build on this success through a single 40ks ToO observation of a black hole transient in outburst during a either the high/soft, intermediate or brighter phases of the low/hard state. GALACTIC POINT SOURCES 4 A REIS RUBENS NULL NULL USA 7 AO7-TOO UNDERSTANDING BLACK HOLES: SPIN, DISK PHYSICS AND STATE TRANSITIONS XIS N GX 339-4 255.70625 -48.78972 338.9393589 -4.32669914 -99 NULL NULL 407078010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071244 Due to the presence of a steady jet, constraining the properties of black hole systems in their canonical hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, the upcoming NuSTAR mission, and radio observations to answer these questions. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 7 AO7-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N 4U 1543-47 236.78583 -47.66944 330.91865964 5.42579106 -99 NULL NULL 407079010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071244 Due to the presence of a steady jet, constraining the properties of black hole systems in their canonical hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, the upcoming NuSTAR mission, and radio observations to answer these questions. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 7 AO7-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N V404 CYG 306.01596 33.86728 73.11883543 -2.09143677 -99 NULL NULL 407080010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071244 Due to the presence of a steady jet, constraining the properties of black hole systems in their canonical hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, the upcoming NuSTAR mission, and radio observations to answer these questions. GALACTIC POINT SOURCES 4 B TOMSICK JOHN NULL NULL USA 7 AO7-TOO CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES XIS N 1E 1547.0-5408 237.72546 -54.30658 327.23698364 -0.1315599 -99 NULL NULL 407081010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N 1E 1547.0-5408 237.72546 -54.30658 327.23698364 -0.1315599 -99 NULL NULL 407081020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SGR 0501+4516 75.28333 45.27528 161.54955797 1.95129634 -99 NULL NULL 407082010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SGR 0501+4516 75.28333 45.27528 161.54955797 1.95129634 -99 NULL NULL 407082020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SGR 1806-20 272.16383 -20.41097 9.99597117 -0.24183424 -99 NULL NULL 407083010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SGR 1806-20 272.16383 -20.41097 9.99597117 -0.24183424 -99 NULL NULL 407083020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SWIFT J1822-1606 275.575 -16.07411 15.35266129 -1.02094777 -99 NULL NULL 407084010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SWIFT J1822-1606 275.575 -16.07411 15.35266129 -1.02094777 -99 NULL NULL 407084020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SWIFT J1834.9-0846 278.71717 -8.76556 23.24974475 -0.34100673 -99 NULL NULL 407085010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N SWIFT J1834.9-0846 278.71717 -8.76556 23.24974475 -0.34100673 -99 NULL NULL 407085020 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071301 Recently discovered hard X-rays in ~10-300 keV is an unique spectral property of strongly magnetized neutron stars: soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs). Combining the XIS and HXD spectra, our Suzaku study derived an empirical relation between this hard X-rays and the well-known soft thermal X-rays (<10 keV) as a function of their pulsar ages and magnetic fields. Such a correlation implies an unification of SGRs and AXPs into one evolutional path. Our next step is to investigate the broadband spectra of transient magnetars in their outbursts. Here we propose a reserved ToO towards transient sources to detect the hard X-rays during early phases of outburst, and to perform detailed spectral investigations. GALACTIC POINT SOURCES 4 B ENOTO TERUAKI NULL NULL USA 7 AO7-TOO DO THE HARD X-RAYS ALWAYS APPEAR IN TRANSIENT MAGNETARS? XIS N LMC X-3 84.73596 -64.08425 273.57643041 -32.08143715 -99 NULL NULL 407086010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072002 We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state. GALACTIC POINT SOURCES 4 A KOLEHMAINEN MARI NULL NULL EUR 7 AO7-TOO A TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES? XIS N MWC 560 111.46371 -7.73558 223.75985215 4.04625645 -99 NULL NULL 407087010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072003 Although jets are ubiquitous and important components in many different astrophysical systems, their formation remains very poorly understood. The pole-on jet in the symbiotic system MWC 560 serves as a Rosetta Stone for understanding pulsed, highly collimated, jets. We propose to use Suzaku for X-ray observations of the symbiotic star MWC 560. It provides us with a unique opportunity to observe the launch site of the jet, the shock-induced propagation of the jet, and its end point, where the ejecta merge into the jet head. We detected with XMM a hard component from the accretion site and a soft component associated with the jet. Further observations are required for solving questions concerning the accretion process and for characterizing the soft component. GALACTIC POINT SOURCES 4 C STUTE MATTHIAS NULL NULL EUR 7 AO7 CATCHING A SYMBIOTIC STAR'S PULSED JET IN THE ACT: X-RAY OBSERVATIONS OF MWC560 XIS N 4U 0352+30 58.06325 30.9 162.65863605 -17.69224618 -99 NULL NULL 407088010 -99 150000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072011 After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys. GALACTIC POINT SOURCES 4 B DOROSHENKO VICTOR NULL NULL EUR 7 AO7 CRACKING THE X PER XIS N EXO 2030+375 308.06367 37.63747 77.15188826 -1.24180491 -99 NULL NULL 407089010 -99 75000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072013 We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties. GALACTIC POINT SOURCES 4 A FERRIGNO CARLO NULL NULL EUR 7 AO7 UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375 XIS Y 4U 1705-44 257.22696 17.14847 37.83631459 30.1547389 -99 NULL NULL 407090010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072015 We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system. GALACTIC POINT SOURCES 4 A DI SALVO TIZIANA NULL NULL EUR 7 AO7-TOO SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE XIS N J1620-4927 245.17275 -49.46006 333.8881362 0.4079132 -99 NULL NULL 407091010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARELLI MARTINO NULL NULL EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS N J1803-2149 270.78992 -21.81519 8.14453694 0.19016071 -99 NULL NULL 407092010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARELLI MARTINO NULL NULL EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS N J1746-3239 266.72867 -32.66517 356.95743439 -2.1748349 -99 NULL NULL 407093010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARELLI MARTINO NULL NULL EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS N J1522-5734 230.52229 -57.58311 322.05253936 -0.41511189 -99 NULL NULL 407094010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072019 The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. GALACTIC POINT SOURCES 4 A MARELLI MARTINO NULL NULL EUR 7 AO7 SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS XIS N 4U 1735-44 264.74292 -44.45 346.05430491 -6.99387213 -99 NULL NULL 407095010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072024 We propose to observe the bursting low-mass X-ray binary 4U~1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum, performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to study the iron line at 6.4-7 keV simultaneously with the expected iron edge, to detect other emission lines at lower energy, and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source) thanks to the broad-band capabilities of Suzaku. This will allow us to increase the sample of broad iron lines in neutron star X-ray binaries, and above all, to infer and probe the origin of these components, which is still debated. GALACTIC POINT SOURCES 4 C EGRON ELISE NULL NULL EUR 7 AO7 BROAD BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU XIS N 1FGL J1018.6-5856 154.73208 -58.94356 284.35060516 -1.68781714 -99 NULL NULL 407096010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 073113 Recently, a modulated signal has been detected with the Fermi from the source 1FGL J1018.6-5856. The presence of a O-type star in this source, and the variable character of the signal suggested that the source is a new gamma-ray binary system. Since it is expected that X-rays in these sources has the synchrotron origin, detailed X-ray observations are very important for understanding of the processes occurring in the system. However, sensitive observations of source in the X-ray energy bands are still missing. Therefore, we propose to observe the source with Suzaku. Since a long observational campaign is planned for 2012 by the HESS collaboration, the obtained X-ray, together with TeV, data will allow a proper modeling of the physical processes behind the non-thermal emission in system. GALACTIC POINT SOURCES 4 B ODAKA HIROKAZU TANAKA TAKAAKI JUS 7 AO7 X-RAY OBSERVATION OF GAMMA-RAY BINARY 1FGL J1018.6-5856 XIS N BULGE 3 274.7046 -31.4846 1.3002625 -7.49777303 80.4025 53800.3437962963 53801.7474421296 500001010 51846.8 50000 51854.8 51854.8 51854.8 51846.8 2 2 2 2 1 0 0 45078.3 45078.3 121245.9 0 PROCESSED 54325.1603935185 54247 54041.7128703704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001014 Leading . GALACTIC DIFFUSE EMISSION 5 A MCCAMMON DAN NULL NULL JAP 0 SWG THE SOFT GALACTIC BULGE XIS N BULGE 2 270.6176 -29.5847 1.30042786 -3.49803376 83.2679 53801.7493981482 53802.0689699074 500002010 13028 10000 13052 13044 13036 13028 1 1 1 1 1 0 0 10674.1 10674.1 27599.9 1 PROCESSED 54320.5751273148 54247 54041.664525463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001014 Leading . GALACTIC DIFFUSE EMISSION 5 A MCCAMMON DAN NULL NULL JAP 0 SWG THE SOFT GALACTIC BULGE XIS N BULGE 6 282.6839 -33.8925 1.99857856 -14.59644221 88.3467 53802.7373032407 53803.0466087963 500003010 14261.7 10000 14261.7 14261.7 14261.7 14261.7 2 2 2 2 1 0 0 11414 11414 26715.9 1 PROCESSED 54320.5876041667 54247 54041.7424305556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001014 Leading . GALACTIC DIFFUSE EMISSION 5 A MCCAMMON DAN NULL NULL JAP 0 SWG THE SOFT GALACTIC BULGE XIS N RCW86 SW 220.2761 -62.6782 315.14426109 -2.43598628 109.6929 53778.0961689815 53780.2814699074 500004010 100765.9 100000 100781.9 100765.9 100781.9 100781.9 2 2 2 2 1 0 0 90681.9 90681.9 188791.8 2 PROCESSED 54330.3924537037 54247 54041.2835648148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001019 The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 0 SWG THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86 XIS N GC CENTER #2 266.7693 -28.6295 0.42794484 -0.11339991 74.7707 53821.958587963 53823.7585069444 500005010 88424.7 100000 88432.7 88424.7 88432.7 88432.7 2 2 2 2 1 0 0 64591.1 64591.1 155501.9 2 PROCESSED 54328.6633796296 54247 54133.0079861111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001020 We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 0 SWG SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1 NULL N SN 1987A 83.8361 -69.2786 279.71542477 -31.94667609 132.5904 53677.835775463 53678.3475 500006010 36786.3 40000 36786.3 36786.3 36786.3 36786.3 2 2 2 2 1 0 0 32919.8 32919.8 44166.1 1 PROCESSED 54326.9673726852 54247 54037.1281481482 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001028 SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies. GALACTIC DIFFUSE EMISSION 5 A HASINGER GUENTHER NULL NULL JAP 0 SWG SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR NULL N HESS J1804-216 271.1693 -21.6722 8.44223916 -0.04647489 89.0483 53831.6120138889 53832.4919328704 500007010 37522.2 50000 37522.2 37522.2 37522.2 37522.2 2 2 2 2 1 0 0 28933.6 28933.6 75990.1 0 PROCESSED 54322.9283217593 54247 54042.288900463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001029 HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 0 SWG SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' XIS N HESS J1804-216 BGD 270.9564 -22.0176 8.04431311 -0.04388906 89.2004 53832.4925462963 53833.454375 500008010 40717.1 50000 40717.1 40717.1 40717.1 40717.1 2 2 2 2 1 0 0 30642.9 30642.9 83087.9 1 PROCESSED 54327.1449652778 54247 54056.4266666667 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001029 HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 0 SWG SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' XIS N GALACTIC RIDGE 281.0049 -4.0776 28.45801897 -0.21166151 265.5297 53671.1112037037 53673.8960069445 500009010 93327.6 100000 93343.6 93359.6 93343.6 93327.6 2 2 2 2 1 0 0 77536.4 77536.4 240575.9 0 PROCESSED 54331.0101967593 54247 54037.6929513889 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001042 We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. GALACTIC DIFFUSE EMISSION 5 A EBISAWA KEN NULL NULL JAP 0 SWG ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION NULL N GALACTIC RIDGE 281.0036 -4.078 28.45707071 -0.21069081 265.5303 54023.0938888889 54025.8141087963 500009020 98858.3 100000 98874.3 98866.3 98858.3 98874.3 2 2 2 2 1 0 0 81951.9 81951.9 235013.9 1 PROCESSED 54330.1000115741 54697 54055.6082407407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001042 We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. GALACTIC DIFFUSE EMISSION 5 A EBISAWA KEN NULL NULL JAP 0 SWG ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION XIS Y RXJ_0852-4622_NW 132.2926 -45.6157 265.39238743 -1.14402175 137.763 53723.4478240741 53727.3016666667 500010010 175453 150000 175453 175525 175460.8 175461 2 2 2 2 1 0 0 230002.5 230002.5 332943.7 7 PROCESSED 54331.9048263889 54247 54059.902662037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001048 We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL JAP 0 SWG HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 HXD N RXJ_0852-4622_NW_offset 135.1284 -47.9102 268.39892579 -1.13950817 140.267 53727.3040393518 53728.368912037 500010020 59178.4 50000 59178.4 59192.5 59202.6 59192.5 2 2 2 2 1 0 0 63482.1 63482.1 91995.9 0 PROCESSED 54327.312962963 54247 54039.2486226852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001048 We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL JAP 0 SWG HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 HXD N SMC DIFFUSE 1 13.0188 -72.8206 302.86615918 -44.30756989 221.6864 53687.4452893518 53688.2231944445 500011010 46778.9 50000 46778.9 46786.9 46786.9 46786.9 1 1 1 1 1 0 0 47868.4 47868.4 67199.9 0 PROCESSED 54322.7758449074 54247 54038.3531712963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001049 We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL JAP 0 SWG DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS XIS N 73P/SW3 279.2884 33.5067 62.26395264 17.33399104 47.3721 53862.3946875 53862.4794444444 500012010 3250 5000 3250 3250 3250 3250 1 1 1 1 1 0 0 2313.9 2313.9 7304 0 PROCESSED 54320.6031944444 54256 54042.1755671296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 279.6627 33.4734 62.35168426 17.03145652 46.5564 53862.4804282407 53862.5419444444 500012020 3248 5000 3248 3248 3248 3248 1 1 1 1 1 0 0 2111.9 2111.9 5279.9 0 PROCESSED 54320.4688078704 54256 54042.2282175926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 316.717 24.6807 71.53645371 -15.07849931 72.7087 53868.1752314815 53868.2085532407 500013010 2353 20000 2353 2353 2353 2353 1 1 1 1 1 0 0 2595 2595 2871.9 0 PROCESSED 54320.6021064815 54256 54042.2312268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 317.1042 24.5187 71.64340536 -15.45205291 72.7099 53868.2091666667 53868.2752199074 500013020 3225 20000 3225 3225 3225 3225 1 1 1 1 1 0 0 3467 3467 5703.9 0 PROCESSED 54320.4892361111 54256 54042.2634027778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 317.5094 24.3437 71.75290875 -15.84652301 72.7094 53868.2758333333 53868.3418865741 500013030 3225 20000 3225 3225 3225 3225 1 1 1 1 1 0 0 2915 2915 5703.9 0 PROCESSED 54320.6158796296 54256 54042.2712731482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 317.9167 24.1666 71.86402338 -16.24383714 72.7109 53868.3425 53868.4085532407 500013040 3225 20000 3225 3225 3225 3225 1 1 1 1 1 0 0 2677 2677 5703.9 0 PROCESSED 54320.4917708333 54256 54042.2977430556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 318.3252 23.9905 71.97868305 -16.64134569 72.7093 53868.4091666667 53868.4752199074 500013050 3225 20000 3225 3225 3225 3225 1 1 1 1 1 0 0 2584 2584 5703.9 0 PROCESSED 54320.6176851852 54256 54089.4348611111 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 318.7382 23.8104 72.09504522 -17.04458663 72.7096 53868.4758333333 53868.5418865741 500013060 3218 20000 3218 3218 3218 3218 1 1 1 1 1 0 0 2539 2539 5695.9 0 PROCESSED 54320.492349537 54256 54042.3000462963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 319.1503 23.6322 72.21442919 -17.44595626 72.7095 53868.5425 53868.6085532407 500013070 3062.4 20000 3062.4 3062.4 3062.4 3062.4 1 1 1 1 1 0 0 2088 2088 5688 1 PROCESSED 54320.614375 54256 54042.3037268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 319.575 23.4516 72.3420597 -17.8575616 72.7092 53868.609212963 53868.6738310185 500013080 3164.4 20000 3164.4 3164.4 3164.4 3164.4 1 1 1 1 1 0 0 2986 2986 5551.9 0 PROCESSED 54320.4853472222 54256 54042.3213657407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.4857 -9.3839 140.65827116 -71.47693301 59.4008 53893.6903703704 53893.7356365741 500014010 3228 35000 3228 3228 3228 3228 1 1 1 1 1 0 0 3312 3312 3903.9 0 PROCESSED 54320.6211689815 54267 54052.5070949074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 17.8447 -9.1515 138.54867442 -71.41609802 59.3994 53893.7363888889 53893.8023032407 500014020 3236.9 35000 3236.9 3236.9 3236.9 3236.9 1 1 1 1 1 0 0 2478 2478 5687.9 0 PROCESSED 54320.6365740741 54267 54052.5079861111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 17.8996 -9.1693 138.7272506 -71.42013328 59.3998 53893.8025 53893.8689699074 500014030 3236.1 35000 3236.1 3236.1 3236.1 3236.1 1 1 1 1 1 0 0 2433.1 2433.1 5735.9 0 PROCESSED 54320.6368634259 54267 54052.5088310185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 17.9545 -9.1915 138.90931762 -71.42827213 59.4015 53893.8691666667 53893.9356365741 500014040 3236 35000 3236 3236 3236 3236 1 1 1 1 1 0 0 2490.9 2490.9 5735.9 0 PROCESSED 54320.5128356482 54267 54052.5308912037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.0085 -9.2093 139.0853548 -71.43220951 59.4015 53893.9358333333 53894.0023032407 500014050 3235 35000 3235 3235 3235 3235 1 1 1 1 1 0 0 2504.1 2504.1 5735.9 0 PROCESSED 54320.5147106482 54267 54052.5317361111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.0599 -9.2267 139.25333623 -71.43625621 59.4006 53894.0025 53894.0689699074 500014060 3235 35000 3235 3235 3235 3235 1 1 1 1 1 0 0 2490 2490 5735.9 0 PROCESSED 54320.6379398148 54267 54052.5346759259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.1094 -9.2436 139.41528011 -71.44015907 59.3996 53894.0691666667 53894.1356365741 500014070 2220.9 35000 2220.9 2220.9 2220.9 2220.9 1 1 1 1 1 0 0 1939 1939 5735.9 1 PROCESSED 54320.6268634259 54267 54052.5472800926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.1606 -9.2654 139.58635244 -71.44823165 59.3999 53894.1358333333 53894.2085416667 500014080 1863.7 35000 1863.7 1863.7 1863.7 1863.7 2 2 2 2 1 0 0 1921.2 1921.2 6277.9 0 PROCESSED 54320.6348263889 54267 54052.5243171296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.2084 -9.2837 139.744498 -71.45365551 59.3985 53894.2087384259 53894.2689467593 500014090 1508.9 35000 1508.9 1508.9 1508.9 1508.9 1 1 1 1 1 0 0 1655.2 1655.2 5202 0 PROCESSED 54320.4982523148 54267 54052.5382986111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.2503 -9.299 139.88257526 -71.45759255 59.3985 53894.2691435185 53894.3356134259 500014100 1312.1 35000 1312.1 1312.1 1312.1 1312.1 1 1 1 1 1 0 0 1322 1322 5742 0 PROCESSED 54320.6302893518 54267 54052.5405324074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.2949 -9.3163 140.03044964 -71.46265703 59.3979 53894.3358101852 53894.4022800926 500014110 1424.9 35000 1424.9 1424.9 1424.9 1424.9 1 1 1 1 1 0 0 1433 1433 5742 0 PROCESSED 54320.5114236111 54267 54052.5225694444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.338 -9.3332 140.17356876 -71.46762322 59.3974 53894.4024768518 53894.4682986111 500014120 1555.1 35000 1555.1 1555.1 1555.1 1555.1 1 1 1 1 1 0 0 1566 1566 5682 0 PROCESSED 54320.5052199074 54267 54052.5441782407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.3869 -9.3535 140.33698221 -71.47421859 59.3991 53894.4684490741 53894.5356365741 500014130 1693.9 35000 1693.9 1693.9 1693.9 1693.9 1 1 1 1 1 0 0 1694 1694 5804 0 PROCESSED 54320.6286689815 54267 54052.5234722222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.435 -9.3697 140.49459076 -71.47695116 59.4003 53894.5358333333 53894.6016087963 500014140 1977 35000 1977 1977 1977 1977 1 1 1 1 1 0 0 1951 1951 5671.9 0 PROCESSED 54320.4993171296 54267 54052.5450231482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N 73P/SW3 18.4874 -9.3902 140.66879726 -71.4825298 59.4036 53894.6018055556 53894.680775463 500014150 3232 35000 3232 3232 3232 3232 1 1 1 1 1 0 0 3293 3293 6815.9 0 PROCESSED 54320.6442361111 54267 54052.5265509259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001050 Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. GALACTIC DIFFUSE EMISSION 5 A PORTER FREDERICK NULL NULL JAP 0 SWG AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 XIS N MBM12 44.0042 19.487 159.18888296 -34.46916863 253.4644 53769.9600578704 53772.6460416667 500015010 102937.1 100000 102937.1 102937.1 102937.1 102937.1 2 2 2 2 1 0 0 93670.9 93670.9 232049.9 1 PROCESSED 54330.2671412037 54247 54041.1327662037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001059 Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB. GALACTIC DIFFUSE EMISSION 5 A SMITH RANDALL NULL NULL JAP 0 SWG DATING THE LOCAL HOT BUBBLE WITH SUZAKU XIS N SN1006 SE 225.8656 -42.0517 327.61589547 14.40537 115.0022 53765.3759259259 53766.487662037 500016010 51607.6 50000 51613.2 51621.2 51621.2 51607.6 2 2 2 2 1 0 0 55670.4 55670.4 96039.9 2 PROCESSED 54324.9845138889 54247 54040.6484259259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001062 We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. GALACTIC DIFFUSE EMISSION 5 A HUGHES JOHN NULL NULL JAP 0 SWG THE EJECTA IN SN1006 XIS N SN1006 NW 225.6364 -41.8003 327.59294648 14.70833496 115.0008 53766.4881365741 53767.55375 500017010 53019.4 50000 53019.4 53027.7 53027.3 53027.3 2 2 2 2 1 0 0 60412.3 60412.3 92067.9 0 PROCESSED 54324.6815625 54247 54040.7669675926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001062 We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. GALACTIC DIFFUSE EMISSION 5 A HUGHES JOHN NULL NULL JAP 0 SWG THE EJECTA IN SN1006 XIS N SGR C 266.1523 -29.4673 359.43182832 -0.08906822 82.0001 53786.5315393518 53789.4515509259 500018010 106921.9 100000 106921.9 106921.9 106921.9 106921.9 2 2 2 2 1 0 0 46606.9 46606.9 252277.8 2 PROCESSED 54328.8217013889 54247 54041.6109375 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001079 We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. GALACTIC DIFFUSE EMISSION 5 A MURAKAMI HIROSHI NULL NULL JAP 0 SWG FOSSILS OF THE GALACTIC CENTER ACTIVITY XIS N SGR C BGD 265.7856 -29.8854 358.90876565 -0.03691694 81.9998 53789.4522106482 53789.8349421296 500019010 13307.3 10000 13315.3 13315.3 13315.3 13307.3 2 2 2 2 1 0 0 12240.4 12240.4 33063.9 0 PROCESSED 54320.7962847222 54247 54041.3629166667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001079 We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. GALACTIC DIFFUSE EMISSION 5 A MURAKAMI HIROSHI NULL NULL JAP 0 SWG FOSSILS OF THE GALACTIC CENTER ACTIVITY XIS N CYGNUS LOOP NE1 314.1885 31.738 75.60815027 -8.84073861 223.0005 53697.7354282407 53698.2051388889 500020010 20343.7 20000 20351.7 20351.7 20351.7 20343.7 1 1 1 1 1 0 0 17992 17992 40575.9 0 PROCESSED 54324.2030092593 54247 54037.9167476852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001093 We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 0 SWG CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT NULL N CYGNUS LOOP NE2 313.9681 31.9542 75.65570239 -8.55863001 223.0005 53698.2056134259 53698.6766666667 500021010 21413.5 20000 21445.5 21437.5 21429.5 21413.5 2 2 2 2 1 0 0 21654.1 21654.1 40693.9 0 PROCESSED 54324.5717013889 54247 54038.4014351852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001093 We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 0 SWG CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT NULL N CYGNUS LOOP NE3 313.7583 32.1826 75.71932756 -8.27611719 222.9011 53703.7415162037 53704.2355208333 500022010 21133.8 20000 21191.6 21719.9 21133.8 21359.9 2 2 2 2 1 0 0 20244.5 20244.5 42679.9 1 PROCESSED 54324.6667013889 54247 54038.7522106482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001093 We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 0 SWG CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT XIS N CYGNUS LOOP NE4 313.5005 32.369 75.72495347 -7.98937114 221.2023 53704.2368287037 53704.7661342593 500023010 25004.9 20000 25004.9 25268.9 25006.7 25068.9 2 2 2 2 1 0 0 25124.9 25124.9 45726 1 PROCESSED 54324.6202430556 54247 54038.67625 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001093 We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 0 SWG CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT XIS N TYCHO SNR 6.3244 64.1507 120.08671326 1.42345384 81.1044 53913.439224537 53915.6530555556 500024010 101127.4 100000 101143.4 101127.4 101143.4 101143.4 2 2 2 2 1 0 0 94512.3 94512.3 191206.8 3 PROCESSED 54332.1766203704 54289 54052.7199884259 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001099 We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. GALACTIC DIFFUSE EMISSION 5 A HUGHES JOHN NULL NULL JAP 0 SWG SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT XIS N TYCHO SNR HXD BKGD 9.2173 64.3076 121.35322514 1.48051733 84.2005 53915.6541782407 53916.7606944444 500025010 51008.8 50000 51008.8 51008.8 51008.8 51008.8 2 2 2 2 1 0 0 48722.4 48722.4 95593.9 2 PROCESSED 54324.0584375 54302 54052.5940509259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001099 We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. GALACTIC DIFFUSE EMISSION 5 A HUGHES JOHN NULL NULL JAP 0 SWG SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT HXD N NEP 272.8227 66.0165 95.79277142 28.663354 126.3033 53776.2556944445 53778.0836111111 500026010 88508.2 80000 88532.2 88508.2 88524.2 88532.2 2 2 2 2 1 0 0 83672.8 83672.8 157902 0 PROCESSED 54327.7111342593 54247 54041.1403703704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000042 We propose a second Suzaku observation of the NEP region in order to constrain the long-term and short-term valiability of OVII and OIVVV emission line intensities.Short-term variability detected in the first Suzaku observation implies existence of a charge-exchange component in oVIII linem suggesting solar wind and geo corona interaction. First purpose is to confirm this with the second observtaion.Secondly, to search a long-term variability. If it is observed, it will place a further constraints on the solar wind and interplanetary medium near the Earth. GALACTIC DIFFUSE EMISSION 5 A SWG NULL NULL NULL JAP 0 SWG NEP XIS N HIGH LAT. DIFFUSE A 246.1745 43.4846 68.4171583 44.39202319 129.9994 53780.2926388889 53781.9640509259 500027010 73578.7 70000 73586.7 73586.7 73578.7 73586.7 2 2 2 2 1 0 0 67399.3 67399.3 144397.9 3 PROCESSED 54328.5553472222 54247 54041.3110416667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000044 We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. GALACTIC DIFFUSE EMISSION 5 A SWG NULL NULL NULL JAP 0 SWG HIGH LATTITUDE DIFFUSE A & B XIS N HIGH LAT. DIFFUSE B 38.7468 -52.2774 272.40280946 -58.27300774 280.6379 53783.933900463 53786.5211111111 500027020 103553 100000 103553 103561 103561 103561 2 2 2 2 1 0 0 68609.4 68609.4 223523.8 3 PROCESSED 54329.4329513889 54247 54041.5670717593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000044 We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. GALACTIC DIFFUSE EMISSION 5 A SWG NULL NULL NULL JAP 0 SWG HIGH LATTITUDE DIFFUSE A & B XIS N VICINITY OF LMC X-3 83.4844 -63.8863 273.3865557 -32.64248934 284.6189 53811.6008333333 53813.9168055556 500031010 82018.5 80000 82026.5 82018.5 82026.5 82026.5 2 2 2 2 1 0 0 74614.8 74614.8 200063.9 2 PROCESSED 54329.0668402778 54247 54056.4806828704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 000043 We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ? GALACTIC DIFFUSE EMISSION 5 A SWG NULL NULL NULL JAP 0 SWG VICINITY OF LMC X-3 XIS N SKY_50.0_-62.4 50.0507 -62.4328 278.67600391 -47.08169247 281.591 53795.7055671296 53796.9369675926 501001010 80145 80000 80153 80145 80153 80145 2 2 2 2 1 0 0 74012.2 74012.2 106376 0 PROCESSED 54324.2393518518 54401 53905.6164930556 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011252 We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. GALACTIC DIFFUSE EMISSION 5 A SHELTON ROBIN NULL NULL USA 1 AO1 SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE XIS N SKY_53.3_-63.4 53.24 -63.4549 278.62179386 -45.30780651 286.1724 53797.8694444444 53800.3342476852 501002010 101475.2 100000 101475.2 101475.2 101475.2 101475.2 2 2 2 2 1 0 0 145431.8 145431.8 212853.9 4 PROCESSED 54329.5976736111 54401 53906.7729282407 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011252 We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. GALACTIC DIFFUSE EMISSION 5 A SHELTON ROBIN NULL NULL USA 1 AO1 SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE XIS N M17 275.2076 -16.1829 15.0906551 -0.7606192 110.1996 53805.8263425926 53808.5349421296 501003010 102702.1 100000 102710.1 102710.1 102702.1 102710.1 2 2 2 2 1 0 0 92566.1 92566.1 233967.8 4 PROCESSED 54330.0440625 54394 53905.822662037 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010066 Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution. GALACTIC DIFFUSE EMISSION 5 A TSUJIMOTO MASAHIRO NULL NULL JAP 1 AO1 XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS XIS N DRACO HVC REGION A 243.9602 60.0594 91.20688798 42.38144862 79.8192 53814.6161111111 53816.0050578704 501004010 61179.8 60000 61179.8 61179.8 61179.8 61179.8 2 2 2 2 1 0 0 61230.1 61230.1 119987.9 2 PROCESSED 54405.7030902778 54394 53906.0459722222 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010069 High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 1 AO1 SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - XIS N DRACO HVC REGION B 243.9603 59.1738 90.07720195 42.68363475 80.282 53816.0059953704 53817.4148611111 501005010 61632 60000 61644.7 61644 61632 61636 2 2 2 2 1 0 0 60686.5 60686.5 121709.9 2 PROCESSED 54405.7328819444 54400 53906.4964583333 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010069 High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 1 AO1 SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - XIS N IC 443 94.2975 22.7757 188.8694635 3.11574616 274.0004 54165.4446643518 54166.5154398148 501006010 42011.3 40000 42011.3 42012.9 0 42020.9 2 2 0 2 1 0 0 34693.4 34693.4 92509.9 2 PROCESSED 54324.7636574074 54736 54174.6613541667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010040 IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. GALACTIC DIFFUSE EMISSION 5 B OZAKI MASANOBU NULL NULL JAP 1 AO1 UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION XIS Y IC 443 94.2972 22.4797 189.13057055 2.97563306 274.0001 54166.5158680556 54167.612025463 501006020 44013.5 40000 44013.5 44037.5 0 44021.5 2 2 0 2 1 0 0 36320.9 36320.9 94699.9 1 PROCESSED 54324.2986805556 54736 54172.2247800926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010040 IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. GALACTIC DIFFUSE EMISSION 5 B OZAKI MASANOBU NULL NULL JAP 1 AO1 UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION XIS Y CTB 37B 258.4918 -38.2006 348.64561092 0.37683278 270.1267 53974.0604976852 53976.2398032407 501007010 82815.1 80000 82871.1 82815.1 82879.1 82863.1 2 2 2 2 1 0 0 68860.3 68860.3 188277.9 2 PROCESSED 54328.2313541667 54526 54053.4840162037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010042 The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the extended sample with radio SNR counterpart, CTB 37B, which is marginally detected on the edge of ASCA GIS. ASCA spectrum shows rather soft power-law feature, indicating that there are both thermal and non-thermal X-ray emission. With the low background of XISs and HXD, parameters of both components are determined with 80 ks exposure. The non-thermal component suggests the new sample of accelerators, and the thermal compopent reveals the condition of the proton acceleration site, for the first time. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 1 AO1 UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS XIS N GC SOUTH 266.5016 -29.1694 359.84485124 -0.1935349 265.0006 54004.5960185185 54007.8925231482 501008010 129577.3 130000 129577.3 129577.3 129577.3 129577.3 2 2 2 2 1 0 0 111259.1 111259.1 284803.8 5 PROCESSED 54331.2681018518 54744 54021.0929050926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010044 Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 1 AO1 SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER XIS Y GC SOUTH BGD 266.1893 -28.9082 359.92534776 0.17564926 265.0003 54007.8931365741 54009.2884143518 501009010 51190 50000 51198 51206 51190 51198 2 2 2 2 1 0 0 47715.7 47715.7 120547.9 0 PROCESSED 54324.1121643518 54735 54020.9371064815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010044 Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 1 AO1 SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER XIS Y HESS J1745-303 266.2629 -30.3722 358.71029443 -0.64354718 263.6011 54015.0950462963 54016.4300810185 501010010 50670.7 50000 50670.7 50670.7 50670.7 50670.7 1 1 1 1 1 0 0 45689.7 45689.7 115311.9 1 PROCESSED 54327.2596643518 54526 54021.698587963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010046 So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons. GALACTIC DIFFUSE EMISSION 5 A YAMAZAKI RYO NULL NULL JAP 1 AO1 X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303 XIS N G344.7-0.1 255.9588 -41.7032 344.67682908 -0.15577285 89.2821 54152.1890393518 54153.2919097222 501011010 42133.6 40000 42133.6 42133.6 0 42133.6 2 2 0 2 1 0 0 34201.6 34201.6 95280 1 PROCESSED 54405.8961342593 54777 54158.2352662037 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010050 We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR. GALACTIC DIFFUSE EMISSION 5 C YAMAUCHI SHIGEO NULL NULL JAP 1 AO1 SUZAKU OBSERVATION OF G344.7-0.1 XIS Y CYGNUS_LOOP_P1 313.519 31.9657 75.41990185 -8.25713566 240 54417.6059259259 54418.0904976852 501012010 16738.5 10000 16738.5 16748.9 0 16742.5 2 2 0 2 1 0 0 15775.8 15775.8 41860 1 PROCESSED 54430.2016087963 54798 54430.2159375 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P2 313.2729 31.7708 75.13379207 -8.21853117 240.0005 54418.0909722222 54418.4168865741 501013010 16379.9 10000 16387.9 16387.9 0 16379.9 1 1 0 1 1 0 0 10978.6 10978.6 28151.9 0 PROCESSED 54430.180150463 54798 54430.1915972222 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P3 313.0409 31.565 74.84662265 -8.19493741 240.0003 54418.4174074074 54418.9377083333 501014010 16764.8 12000 16781.2 16780.8 0 16764.8 2 2 0 2 1 0 0 14696.2 14696.2 44943.9 0 PROCESSED 54430.2504861111 54798 54430.2624884259 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P4 312.8083 31.361 74.56035476 -8.16867105 239.9997 54418.9382291667 54419.3196643518 501015010 18279 15000 18287 18279 0 18287 1 1 0 1 1 0 0 14286 14286 32943.9 0 PROCESSED 54430.2299074074 54798 54430.2398726852 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P5 312.5567 31.1701 74.2739834 -8.12038976 239.9995 54419.3201388889 54420.0627777778 501016010 28406.2 22000 28406.2 28406.2 0 28406.2 2 2 0 2 1 0 0 25370 25370 64155.9 1 PROCESSED 54430.3177893518 54798 54430.4318865741 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P6 312.3057 30.9823 73.99029438 -8.06939848 240.0003 54415.3923032407 54416.1668287037 501017010 28704.9 22000 28704.9 28704.9 0 28704.9 1 1 0 1 1 0 0 26887.8 26887.8 66911.9 0 PROCESSED 54430.1751041667 54798 54430.18875 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P7 312.0838 30.7678 73.70103145 -8.0534172 239.9966 54416.1673032407 54416.7223263889 501018010 24154.5 22000 24154.5 24154.5 0 24154.5 2 2 0 2 1 0 0 18861 18861 47920 0 PROCESSED 54430.1240972222 54798 54430.1343287037 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P9 311.8173 30.594 73.41991066 -7.98099126 239.9998 54416.7228935185 54417.2502199074 501019010 19565.6 15000 19565.6 19565.6 0 19565.6 2 2 0 2 1 0 0 17344.6 17344.6 45537.9 0 PROCESSED 54430.2193865741 54798 54430.2327546296 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P10 311.5744 30.3992 73.13474548 -7.93635975 240.0007 54417.2506944444 54417.6043402778 501020010 16795.8 10000 16795.8 16819.8 0 16803.8 2 2 0 2 1 0 0 12672.9 12672.9 30549.9 0 PROCESSED 54430.1487731482 54798 54430.1578472222 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P8 313.9965 31.4722 75.29540263 -8.88432445 62.5181 53868.0059837963 53868.1717476852 501028010 4870.6 6000 4870.6 4870.6 4870.6 4870.6 2 2 2 2 1 0 0 2328 2328 14316 0 PROCESSED 54320.6489236111 54394 53914.3326157407 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P12 313.7421 31.2725 74.99964096 -8.84356964 62.1405 53864.7943055556 53865.1391087963 501029010 13542.6 10000 13542.6 13542.6 13542.6 13542.6 2 2 2 2 1 0 0 2156.7 2156.7 29780 1 PROCESSED 54320.8458333333 54394 53914.0447916667 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P13 313.4901 31.0708 74.70349314 -8.80441033 68.2467 53865.1416666667 53865.5321643518 501030010 17073 17000 17073 17081 17089 17089 1 1 1 1 1 0 0 14269 14269 33727.9 0 PROCESSED 54320.8883333333 54394 53914.0847569444 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P14 313.2365 30.8681 74.40554659 -8.76356285 62.362 53867.6311111111 53868.0050462963 501031010 18580.9 18000 18580.9 18580.9 18580.9 18580.9 2 2 2 2 1 0 0 12737.8 12737.8 32297.9 0 PROCESSED 54323.0484837963 54394 53914.3142476852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P15 312.9857 30.6621 74.106397 -8.72540127 61.9987 53880.177974537 53880.6716898148 501032010 20728.9 21000 20728.9 20728.9 20728.9 20728.9 2 2 2 2 1 0 0 17476 17476 42634.9 0 PROCESSED 54323.2058796296 54394 53926.2440046296 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P16 312.737 30.4592 73.81069789 -8.68546284 61.9998 53877.1905439815 53877.7605671296 501033010 23337.5 22000 23369.5 23337.5 23369.5 23369.5 2 2 2 2 1 0 0 20118.4 20118.4 49243.9 2 PROCESSED 54326.8950462963 54398 53926.8416319445 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P17 312.199 30.014 73.16561663 -8.59879153 61.9999 53877.7613657407 53878.0446064815 501034010 14195.3 14000 14199.3 14203.3 14199.3 14195.3 2 2 2 2 1 0 0 14823.1 14823.1 24464 0 PROCESSED 54320.6985069444 54394 53926.1395833333 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS N CYGNUS_LOOP_P18 312.0547 29.7111 72.84665082 -8.68804998 237.4994 54087.0528819444 54087.3405208333 501035010 12011 13000 12915 12011 0 12907 2 2 0 2 1 0 0 11439.4 11439.4 24835.9 3 PROCESSED 54320.5629513889 54750 54096.4390972222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y CYGNUS_LOOP_P19 311.8094 30.0818 73.00862935 -8.2918477 237.4997 54087.3411805556 54087.8245833333 501036010 18595 17000 18595 18595 0 18595 2 2 0 2 1 0 0 18355 18355 41755.9 0 PROCESSED 54322.5466782407 54744 54096.1443171296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010052 We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 1 AO1 OBSERVATION OF THE CYGNUS LOOP XIS Y RCW 86 221.2555 -62.3618 315.68741681 -2.33681001 278.3377 53959.4574652778 53961.1294907407 501037010 59805.4 60000 59829.4 59805.4 59829.4 59821.4 2 2 2 2 1 0 0 54405 54405 144420 1 PROCESSED 54324.8825810185 54394 54021.0740972222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010054 We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs. GALACTIC DIFFUSE EMISSION 5 B YAMAGUCHI HIROYA NULL NULL JAP 1 AO1 RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE XIS N GC_SGR_B_EAST 267.0203 -28.3518 0.77973231 -0.1584432 71.8708 54162.5141203704 54164.5273726852 501039010 96401.8 100000 96401.8 96401.8 0 96401.8 2 2 0 2 1 0 0 91082.9 91082.9 173931.8 3 PROCESSED 54327.8467592593 54736 54171.4429050926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010060 We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. GALACTIC DIFFUSE EMISSION 5 B KOYAMA KATSUJI NULL NULL JAP 1 AO1 OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION XIS Y GC_SGR_B_NORTH 266.6958 -28.383 0.60519276 0.06967717 271.4415 53999.7284837963 54001.2863425926 501040010 61375.3 62000 61391.3 61375.3 61383.3 61391.3 2 2 2 2 1 0 0 53867 53867 134581.8 2 PROCESSED 54327.8705324074 54735 54021.2828472222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010060 We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. GALACTIC DIFFUSE EMISSION 5 B KOYAMA KATSUJI NULL NULL JAP 1 AO1 OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION XIS Y GC_SGR_B_NORTH 266.6955 -28.3829 0.60514127 0.06995468 271.4417 54002.2105555556 54003.2919444444 501040020 44829.5 38000 44845.5 44829.5 44837.5 44853.5 2 2 2 2 1 0 0 39970.5 39970.5 93431.9 1 PROCESSED 54327.2088194445 54744 54021.2868055556 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010060 We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. GALACTIC DIFFUSE EMISSION 5 B KOYAMA KATSUJI NULL NULL JAP 1 AO1 OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION XIS Y SNR 0509-67.5 77.3855 -67.5341 278.15788525 -34.58671131 68.6442 53965.2623032407 53966.1640509259 501041010 51276.2 50000 51276.2 51276.2 51276.2 51276.2 2 2 2 2 1 0 0 50829.4 50829.4 77890 1 PROCESSED 54322.9097222222 54526 54020.7617592593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010072 Hot plasma in young supernova remnants (SNRs) are generally in the state of non-equilibrium ionization (NEI), hence strong L-shell lines of Si, Fe and other elements appear in soft energy band (<1keV). With the observations with Chandra and XMM, quite large ambiguity of ionization age for each element remains because of the limited energy resolution in the soft energy band. Utilizing the supreme energy resolution and background property of Suzaku/XIS, we propose the observation of the youngest type Ia SNR in the LMC, 0509-67.5. We correctly diagnose the NEI plasma of this SNR by determining the ionization age and electron temperature for each element component and constrain the ejecta structure of Type Ia SNR. GALACTIC DIFFUSE EMISSION 5 C NAKAJIMA HIROSHI NULL NULL JAP 1 AO1 NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5 XIS N HESS J1614-518 243.5851 -51.743 331.574855 -0.5276897 283.402 53993.6672222222 53994.4571064815 501042010 40177.7 50000 40185.7 40177.7 40185.7 40185.7 2 2 2 2 1 0 0 43560.7 43560.7 68227.9 0 PROCESSED 54323.3265509259 54526 54020.8545833333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010073 We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES XIS N HESS J1614-518 BG 242.0174 -52.4329 330.3996927 -0.37656553 291.2192 53994.4597569444 53995.3015509259 501043010 43555.4 50000 43563.4 43563.4 43555.4 43563.4 1 1 1 1 1 0 0 50592.2 50592.2 72703.9 1 PROCESSED 54323.3811458333 54526 54020.8662268518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010073 We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES XIS N HESS J1825-137 276.5031 -13.6997 17.87105596 -0.70261201 269.3213 54025.8175462963 54027.1682291667 501044010 50293 50000 50293 50293 50293 50293 2 2 2 2 1 0 0 42955.7 42955.7 116694 1 PROCESSED 54325.0219328704 54526 54055.4418634259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010073 We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES XIS N HESS J1825-137 BG 276.9022 -13.2649 18.4366217 -0.84356166 269.33 54027.1689351852 54028.5072337963 501045010 52144.4 50000 52152.4 52144.4 52152.4 52144.4 2 2 2 2 1 0 0 42197.4 42197.4 115607.9 2 PROCESSED 54325.0172453704 54526 54055.6591550926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010073 We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES XIS N GALACTIC CENTER 265.9791 -28.902 359.8343278 0.33569605 108.8002 54169.6271990741 54170.1633564815 501046010 25211 25000 25227 25211 0 25243 2 2 0 2 1 0 0 25008.7 25008.7 46291.9 0 PROCESSED 54322.4241319444 54736 54179.4773842593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER GC2 265.779 -29.1853 359.50136289 0.33591697 108.7998 54170.1638773148 54170.7946064815 501047010 25599 25000 25607 25599 0 25623 1 1 0 1 1 0 0 19088.6 19088.6 54479.9 0 PROCESSED 54323.1010069444 54736 54182.2693865741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER GC3 265.5781 -29.4684 359.1684549 0.33584661 108.8001 54170.7951273148 54171.3397453704 501048010 27454.6 25000 27478.6 27454.6 0 27478.6 1 1 0 1 1 0 0 24054.8 24054.8 47047.9 1 PROCESSED 54320.8735069444 54736 54182.2788425926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER 265.3803 -29.7558 358.83357751 0.33021849 269 54016.4324074074 54017.0968055556 501049010 19562.7 20000 19562.7 19562.7 19562.7 19562.7 2 2 2 2 1 0 0 17633.6 17633.6 57395.9 1 PROCESSED 54323.3270833333 54735 54053.4403356482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER 265.9089 -29.649 359.16615355 -0.00387238 269 54017.0975115741 54017.5690277778 501050010 22047.7 20000 22047.7 22047.7 22047.7 22047.7 1 1 1 1 1 0 0 18625.6 18625.6 40735.9 0 PROCESSED 54323.2511805556 54735 54053.4127777778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER 265.7083 -29.9322 358.83372455 -0.00453222 269.0002 54017.5695486111 54018.2808333333 501051010 21869 20000 21877 21877 21869 21877 2 2 2 2 1 0 0 21132.2 21132.2 61445.9 0 PROCESSED 54326.9430439815 54735 54053.5109953704 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER 265.5037 -30.2156 358.49956421 -0.00336241 269.0005 54018.2813541667 54018.887662037 501052010 19245.1 20000 19261.1 19261.1 19253.1 19245.1 2 2 2 2 1 0 0 16046.2 16046.2 52379.9 1 PROCESSED 54322.6539583333 54735 54053.5074537037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER 265.2994 -30.4982 358.16648703 -0.00302139 269.0003 54018.8881828704 54019.4209953704 501053010 21908.6 20000 21908.6 21932.1 21916.6 21916.6 1 1 1 1 1 0 0 19948 19948 46031.9 0 PROCESSED 54322.5734143518 54735 54053.5019675926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER GC9 266.6299 -29.2499 359.83430056 -0.33104727 109.8001 54171.3410532407 54171.9988888889 501054010 26104.4 25000 26104.4 26104.4 0 26104.4 2 2 0 2 1 0 0 23542.4 23542.4 56829.9 0 PROCESSED 54322.5788310185 54736 54182.2954166667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER GC10 266.4308 -29.5343 359.50116476 -0.33080245 109.7996 54171.9994097222 54172.6529976852 501055010 27225.7 25000 27225.7 27249.7 0 27233.7 2 2 0 2 1 0 0 21181.9 21181.9 56453.9 0 PROCESSED 54326.9427777778 54736 54182.3161342593 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER GC11 266.231 -29.8182 359.16839231 -0.33075371 109.7993 54172.6536111111 54173.2086111111 501056010 26537.4 25000 26545.4 26545.4 0 26537.4 2 2 0 2 1 0 0 25278.9 25278.9 47946 0 PROCESSED 54323.2388310185 54736 54182.3328125 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GALACTIC CENTER 266.0341 -30.1068 358.83318764 -0.33628911 269.0002 54019.4218402778 54020.1446064815 501057010 20488.4 20000 20488.4 20496.4 20496.4 20496.4 2 2 2 2 1 0 0 19086 19086 62437.9 0 PROCESSED 54326.9540972222 54735 54053.6059837963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC SGR D NORTH 266.9758 -27.7178 1.30220378 0.20283685 108.7992 54173.2100578704 54174.7883564815 501058010 63242.2 63000 63250.2 63242.2 0 63258.2 2 2 0 2 1 0 0 51147.9 51147.9 136351.9 0 PROCESSED 54327.5074189815 54735 54182.440462963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC SGR D 267.0913 -27.9356 1.16847417 0.00287016 108.7996 54174.7887847222 54176.2127199074 501059010 62237.2 63000 62237.2 62245.2 0 62245.2 2 2 0 2 1 0 0 54369.7 54369.7 123028 0 PROCESSED 54326.7557523148 54736 54185.4865740741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC SGR D EAST 267.2856 -27.6502 1.50163715 0.00269695 108.7997 54176.2132407407 54177.8737731482 501060010 64795.3 63000 64795.3 64826.7 0 64811.3 2 2 0 2 1 0 0 54629.7 54629.7 143465.9 1 PROCESSED 54324.9423263889 54736 54185.4429050926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010074 We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI KOKUBUN MOTOHIDE JAP 1 AO1 MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y RXJ1713-3946 257.9704 -39.5791 347.29183097 -0.10508063 267.9995 53989.172025463 53989.5306365741 501063010 18422 20000 18422 18422 18422 18422 2 2 2 2 1 0 0 17759.7 17759.7 30971.9 1 PROCESSED 54320.5825462963 54526 54021.1086458333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.1633 -39.7281 347.25895477 -0.31287235 268.0002 53989.5311574074 53989.9216898148 501064010 21322 20000 21322 21322 21322 21322 2 2 2 2 1 0 0 23030.6 23030.6 33727.9 0 PROCESSED 54320.8300115741 54526 54020.8109027778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.1672 -39.4231 347.50735004 -0.13585591 267.9988 53989.9221643518 53990.3106712963 501065010 22011 20000 22011 22011 22011 22011 2 2 2 2 1 0 0 20797.3 20797.3 33557.9 0 PROCESSED 54323.0392361111 54526 54020.8390162037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 257.7744 -39.7271 347.08325974 -0.07081205 268.0001 53990.3113310185 53990.7106944444 501066010 20920.7 20000 20940.7 20920.7 20926 20944.7 2 2 2 2 1 0 0 20699 20699 34504 1 PROCESSED 54320.8296643518 54526 54020.8077546296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 257.7765 -39.428 347.32530765 0.10490445 268.0003 53990.7111689815 53991.0488888889 501067010 21179.6 20000 21187.6 21179.6 21193.1 21195.6 1 1 1 1 1 0 0 21986.1 21986.1 29167.9 0 PROCESSED 54320.7777662037 54526 54020.8250925926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.5534 -39.7289 347.43430559 -0.55631777 267.9997 53991.0497337963 53991.4460300926 501068010 21001.5 20000 21017.5 21009.5 21001.5 21025.5 2 2 2 2 1 0 0 21209.3 21209.3 34233.9 1 PROCESSED 54323.0678356482 54526 54021.2424537037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.5524 -39.4291 347.6770378 -0.38034705 267.9999 53997.5713773148 53997.9140509259 501069010 18375 20000 18375 18375 18375 18375 1 1 1 1 1 0 0 14276.7 14276.7 29599.9 0 PROCESSED 54323.0316550926 54526 54021.1502546296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.5527 -40.0289 347.19063141 -0.73133412 268.0015 53997.9147569444 53998.4425925926 501070010 20744.2 20000 20744.2 20752.2 20752.2 20752.2 2 2 2 2 1 0 0 22026.6 22026.6 45595.9 1 PROCESSED 54322.5989467593 54526 54021.1763541667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.942 -39.4278 347.8535904 -0.62405701 268.0013 53998.4433912037 53998.8467476852 501071010 21174.1 20000 21174.1 21198.1 21190.1 21182.1 1 1 1 1 1 0 0 18338.7 18338.7 34839.9 0 PROCESSED 54323.1323148148 54526 54020.8878009259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N RXJ1713-3946 258.9408 -39.7267 347.60984156 -0.7970823 268.0009 54013.3138541667 54013.877974537 501072010 19981.7 20000 19981.7 19981.7 19981.7 19981.7 2 2 2 2 1 0 0 16299.7 16299.7 48718 1 PROCESSED 54322.580474537 54526 54021.6599652778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010158 We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. GALACTIC DIFFUSE EMISSION 5 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 HXD N G156.2+5.7E 75.8128 51.6405 156.70319129 6.10796494 274.6638 54149.9177893518 54151.1750231482 501074010 53333.1 50000 53349.4 53349.1 0 53333.1 2 2 0 2 1 0 0 50821.8 50821.8 108619.9 2 PROCESSED 54405.89 54773 54158.2839583333 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011235 G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. GALACTIC DIFFUSE EMISSION 5 C PETRE ROBERT NULL NULL USA 1 AO1 A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 XIS Y G156.2+5.7NW 74.223 52.4174 155.48379099 5.80912082 273.883 54147.6530902778 54148.7558333333 501075010 50546.8 50000 50546.8 50546.8 0 50546.8 2 2 0 2 1 0 0 46195.8 46195.8 95259.9 0 PROCESSED 54323.998275463 54695 54153.2775 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011235 G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. GALACTIC DIFFUSE EMISSION 5 C PETRE ROBERT NULL NULL USA 1 AO1 A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 XIS Y SNR 0103-72.6 16.2944 -72.389 301.47055063 -44.70024477 13.8765 53848.0156018518 53849.3773032407 501077010 49271.5 50000 49279.5 49287.5 49287.5 49271.5 2 2 2 2 1 0 0 37190.5 37190.5 117629.9 3 PROCESSED 54323.9669212963 54401 53907.4220023148 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011241 We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 1 AO1 BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD XIS N SNR G93.3+6.9 CENTER 312.9805 55.373 93.25121789 6.97467523 40.9208 53905.2215509259 53905.6480787037 501079010 20537.2 20000 20545.2 20545.2 20545.2 20537.2 2 2 2 2 1 0 0 20008 20008 36815.9 0 PROCESSED 54320.8424537037 54401 53926.792962963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B WANG Q. DANIEL NULL NULL USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N SNR G93.3+6.9 S1 313.1088 55.5284 93.41888838 7.01647125 40.6424 53905.6486458333 53905.9696064815 501080010 15875 15000 15875 15890.2 15891 15883 1 1 1 1 1 0 0 12758.8 12758.8 27727.9 1 PROCESSED 54389.5268287037 54401 53926.199212963 2.1.6.14 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B WANG Q. DANIEL NULL NULL USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N SNR G93.3+6.9 S2 312.6887 55.4958 93.24230604 7.18061007 40.0056 53905.9701736111 53906.4293865741 501081010 16009.2 15000 16035.2 16027.2 16009.2 16035.2 2 2 2 2 1 0 0 18375.7 18375.7 39667.9 1 PROCESSED 54389.5320601852 54401 53927.314537037 2.1.6.14 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B WANG Q. DANIEL NULL NULL USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N SNR G93.3+6.9 S3 313.171 55.2801 93.24775568 6.83197363 40.0152 53906.4300462963 53906.7266087963 501082010 16334.7 15000 16334.7 16358.7 16350.7 16342.7 1 1 1 1 1 0 0 13918.6 13918.6 25615.9 0 PROCESSED 54320.7147800926 54401 53926.2481365741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B WANG Q. DANIEL NULL NULL USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N SNR G93.3+6.9 S4 312.7524 55.2472 93.07038921 6.99620044 39.4008 53906.7271296296 53907.0550347222 501083010 15366.2 15000 15366.2 15366.2 15366.2 15366.2 2 2 2 2 1 0 0 14469.4 14469.4 28327.9 1 PROCESSED 54320.7038773148 54401 53926.117662037 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B WANG Q. DANIEL NULL NULL USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N MONOGEM RING WEST 118.3557 8.2507 212.50229712 17.5030797 287.8334 53865.545462963 53867.1127199074 501084010 54268.5 50000 54268.5 54268.5 54268.5 54268.5 2 2 2 2 1 0 0 43231.2 43231.2 135389.9 2 PROCESSED 54327.5581365741 54401 53914.2479282407 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011243 We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium. GALACTIC DIFFUSE EMISSION 5 B PLUCINSKY PAUL NULL NULL USA 1 AO1 THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU XIS N VELA FRAGMENT B 135.5139 -43.4767 265.2464603 1.98991007 89.0012 54044.6051388889 54046.4341898148 501085010 57880.4 60000 57896.4 57880.4 57896.4 57896.4 2 2 2 2 1 0 0 56965.2 56965.2 158021.9 2 PROCESSED 54327.9224652778 54695 54091.4107175926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011245 Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM. GALACTIC DIFFUSE EMISSION 5 C GAETZ TERRANCE NULL NULL USA 1 AO1 SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B XIS Y PUP A : BEK 125.942 -42.9405 260.51799115 -3.16426215 276.3687 53842.2933449074 53842.5807407407 501086010 16091.3 15000 16091.3 16099.3 16091.3 16091.3 1 1 1 1 1 0 0 9698.5 9698.5 24797 0 PROCESSED 54327.0470138889 54401 53906.8467708333 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011246 We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL USA 1 AO1 MAPPING OXYGEN IN PUPPIS A XIS N PUP A : NE 125.7583 -42.7117 260.25284038 -3.14403225 277.1213 53842.913287037 53843.3091319445 501087010 20710.9 20000 20733.6 20734.9 20718.9 20710.9 1 1 1 1 1 0 0 19744.3 19744.3 34189.9 1 PROCESSED 54327.2677662037 54401 53906.9450231482 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011246 We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL USA 1 AO1 MAPPING OXYGEN IN PUPPIS A XIS N PUP A : INTERIOR 125.5916 -42.8951 260.333956 -3.34905821 276.8883 53842.5813541667 53842.9127199074 501088010 20270.9 20000 20292.4 20294.9 20278.9 20270.9 1 1 1 1 1 0 0 19951.9 19951.9 28623.9 0 PROCESSED 54326.9224652778 54401 53906.8948611111 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011246 We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL USA 1 AO1 MAPPING OXYGEN IN PUPPIS A XIS N PUP A : SE 126.0128 -43.1802 260.74447692 -3.25911558 277.1832 53843.3098842593 53843.8328009259 501089010 29749.3 30000 29749.3 29817.2 29765.2 29761.2 4 2 4 4 1 0 0 22886.7 22886.7 45174 0 PROCESSED 54405.7210532407 54401 53907.001412037 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011246 We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL USA 1 AO1 MAPPING OXYGEN IN PUPPIS A XIS N PUP A : S 125.6829 -43.1445 260.57740663 -3.43620983 277.8865 53843.8334606482 53844.4397569444 501090010 31144.5 30000 31160.5 31152.5 31144.5 31168.5 2 2 2 2 1 0 0 26585.6 26585.6 52371.9 1 PROCESSED 54405.7329166667 54401 53907.0902199074 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011246 We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. GALACTIC DIFFUSE EMISSION 5 A HWANG UNA NULL NULL USA 1 AO1 MAPPING OXYGEN IN PUPPIS A XIS N N11 SB 74.1823 -66.412 277.1886014 -36.07081942 146.432 54046.4407291667 54047.232037037 501091010 30452 30000 30452 30452 30452 30452 2 2 2 2 1 0 0 26405 26405 68365.9 0 PROCESSED 54322.8478935185 54455 54088.5643287037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011251 Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. GALACTIC DIFFUSE EMISSION 5 C WILLIAMS ROSA NULL NULL USA 1 AO1 A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES XIS N LMC X-3 OFF FIELD 1 85.5783 -64.5441 274.09377866 -31.6918405 324.0002 53847.1442361111 53848.0099421296 501097010 43606.7 50000 43606.7 43606.7 43606.7 43606.7 2 2 2 2 1 0 0 42026.1 42026.1 74745.9 0 PROCESSED 54327.0138888889 54526 53907.3335763889 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011256 The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. GALACTIC DIFFUSE EMISSION 5 A WANG Q. DANIEL NULL NULL USA 1 AO1 A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA XIS N LMC X-3 OFF FIELD 1 85.5246 -64.555 274.10794908 -31.71433471 145.4977 54039.3159722222 54039.7509722222 501097020 15374.9 10000 15374.9 15382.9 15382.9 15382.9 2 2 2 2 1 0 0 14926.3 14926.3 37580 0 PROCESSED 54320.8499537037 54526 54088.8072222222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011256 The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. GALACTIC DIFFUSE EMISSION 5 A WANG Q. DANIEL NULL NULL USA 1 AO1 A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA XIS N CAR-D1 162.0244 -59.5887 287.89332648 -0.36746291 282.973 53891.5567361111 53892.6343055556 501099010 76907.4 75000 76924 76932 76931.4 76907.4 2 2 2 2 1 0 0 64257.6 64257.6 93089.9 0 PROCESSED 54323.974224537 54401 53926.947974537 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011257 Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip. GALACTIC DIFFUSE EMISSION 5 B HAMAGUCHI KENJI NULL NULL USA 1 AO1 ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION XIS N GALACTIC PLANE 111 347.9369 61.9538 111.50111702 1.31488521 81.8498 53892.6499652778 53893.680775463 501100010 72140.9 75000 72164.9 72164.9 72164.9 72140.9 2 2 2 2 1 0 0 61025 61025 89034.9 1 PROCESSED 54327.2307407407 54401 53927.3325115741 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011258 We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component. GALACTIC DIFFUSE EMISSION 5 B KUNTZ K. NULL NULL USA 1 AO1 BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111 XIS N DRACO ENHANCEMENT 239.3128 61.2868 93.98685674 43.98646489 194.9053 54048.1213888889 54049.8515509259 501101010 43862.8 75000 79427.4 79427.4 43862.8 79419.4 2 2 2 2 1 0 0 75874.1 75874.1 149474 1 PROCESSED 54328.9772106482 54455 54088.7470486111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011259 We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature. GALACTIC DIFFUSE EMISSION 5 C KUNTZ K. NULL NULL USA 1 AO1 THE SOFT COMPONENT OF THE GALACTIC HALO XIS N MBM12 OFF-CLOUD 41.3205 18.3346 157.33933963 -36.81758445 247.4802 53772.648599537 53774.618275463 501104010 75329.2 70000 75337.2 75329.2 75337.2 75337.2 2 2 2 2 1 0 0 67769 67769 170115.9 1 PROCESSED 54329.8071296296 54401 53905.9757523148 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011262 Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission. GALACTIC DIFFUSE EMISSION 5 B SMITH RANDALL NULL NULL USA 1 AO1 THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND XIS N HESS J1718-385 259.5512 -38.6075 348.79652534 -0.53531102 91.2393 54154.3587731482 54154.7773611111 501105010 20744 19000 20744 20744 0 20744 1 1 0 1 1 0 0 15836.5 15836.5 36151.9 0 PROCESSED 54323.1104976852 54527 54158.2865740741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012044 HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons. GALACTIC DIFFUSE EMISSION 5 A HINTON JAMES NULL NULL EUR 1 AO1 PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE XIS N G156.2+5.7 CENTER 74.723 51.7342 156.21466687 5.62934315 273.4473 54148.7568171296 54149.9169444444 501106010 51214.2 50000 51222.2 51230.2 0 51214.2 1 1 0 1 1 0 0 46482 46482 100199.9 0 PROCESSED 54322.8893634259 54695 54158.4264351852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013079 Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR. GALACTIC DIFFUSE EMISSION 5 B UENO MASARU PETRE ROBERT JUS 1 AO1 REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7 XIS Y VELA X (REGION A) 128.7666 -45.458 263.74862198 -2.99483781 337.7597 53927.7846990741 53929.4703819444 501107010 60773.5 60000 60773.5 60773.5 60773.5 60773.5 2 2 2 2 1 0 0 54161.1 54161.1 145605.8 3 PROCESSED 54329.2805671296 54401 53942.4562037037 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B KARGALTSEV OLEG MORI KOJI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N VELA X (REGION C) 127.7806 -46.2716 263.99736145 -4.03006469 349.189 53933.9133796296 53934.7730787037 501108010 29202.8 30000 29202.8 29202.8 29202.8 29202.8 2 2 2 2 1 0 0 25592.9 25592.9 74248 1 PROCESSED 54327.0649652778 54404 53943.4988773148 2.0.6.13 6 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B KARGALTSEV OLEG MORI KOJI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N VELA PULSAR/PWN 1 128.7701 -45.1981 263.5414959 -2.83747227 337.9628 53926.0492592593 53927.7841782407 501109010 60291.3 60000 60344.6 60291.3 60331.3 60323.3 2 2 2 2 1 0 0 52689.9 52689.9 149865.9 1 PROCESSED 54327.9542824074 54401 53942.4588078704 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B KARGALTSEV OLEG MORI KOJI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR HXD N VELA PULSAR/PWN 3 128.6368 -45.8007 263.96966687 -3.27226783 344.1164 53925.347974537 53926.0467476852 501110010 17588.6 20000 17604.6 17588.6 17588.6 17604.6 1 1 1 1 1 0 0 17225.2 17225.2 60351.9 0 PROCESSED 54323.0630902778 54401 53930.634224537 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B KARGALTSEV OLEG MORI KOJI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N G12.0-0.1 273.0232 -18.6277 11.94868379 -0.09019508 259.2908 54375.5953819444 54376.9863310185 502001010 53752.1 53000 53752.1 53752.1 0 53752.1 2 2 0 2 1 0 0 47183 47183 120172 1 PROCESSED 54403.1000694444 54751 54403.1207986111 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020010 We propose an observation of a supernova remnant (SNR) G12.0-0.1 with Suzaku. ASCA discovered X-ray emission from this SNR. The X-ray spectrum exhibit a power-law shape, and the radius and X-ray luminosity estimated from the ASCA results are similar to those of SN 1006, which suggests that it is a SN 1006-like SNR. However, due to the poor statistics, we could not conclude that G12.0-0.1 is SN 1006-like SNR. Precise measurements of the X-ray spectrum with the XIS will provide us with understanding the physical process in the SNR. GALACTIC DIFFUSE EMISSION 5 B YAMAUCHI SHIGEO NULL NULL JAP 2 AO2 SUZAKU OBSERVATION OF G12.0-0.1 XIS Y GC14 267.1584 -29.141 0.16624555 -0.66947426 260.5381 54382.6950694444 54383.1530555556 502002010 23190.3 20000 23206.3 23190.3 0 23206.3 1 1 0 1 1 0 0 20932.9 20932.9 39559.9 0 PROCESSED 54402.7161111111 54771 54402.7240740741 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC15 266.9617 -29.4257 359.83382525 -0.66952641 260.7835 54383.1536226852 54383.6391666667 502003010 21467.1 20000 21475.1 21467.1 0 21475.1 2 2 0 2 1 0 0 18922.5 18922.5 41943.9 0 PROCESSED 54402.7409490741 54771 54402.7485532407 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC16 267.4868 -29.3131 0.16607902 -1.00376926 260.5335 54383.6397800926 54384.0419444444 502004010 19873 20000 19873 19890.3 0 19874.3 1 1 0 1 1 0 0 18832.1 18832.1 34736 0 PROCESSED 54402.537337963 54771 54402.5680208333 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC17 267.2896 -29.5968 359.83441438 -1.00224826 260.2809 54384.0425578704 54384.480787037 502005010 20603.5 20000 20603.5 20603.5 0 20603.5 2 2 0 2 1 0 0 18174.3 18174.3 37854 1 PROCESSED 54402.5452430556 54777 54402.5689583333 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC18 266.183 -28.6222 0.16630142 0.32982124 260.5302 54384.4819560185 54384.9633564815 502006010 22631.1 20000 22631.1 22641.3 0 22635.1 2 2 0 2 1 0 0 21670.2 21670.2 41584.1 1 PROCESSED 54402.6549537037 54771 54402.6632291667 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC19 265.8593 -28.4466 0.1669402 0.66404713 262.6738 54384.9647569444 54385.4112731482 502007010 22017.4 20000 22017.4 22041.4 0 22025.4 2 2 0 2 1 0 0 19524.8 19524.8 38572 0 PROCESSED 54402.4310763889 54771 54402.4381365741 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC20 265.6604 -28.73 359.83402449 0.66365416 262.9349 54385.4117939815 54385.9099421296 502008010 23778.6 20000 23790.6 23786.6 0 23778.6 2 2 0 2 1 0 0 22923.4 22923.4 43032 0 PROCESSED 54403.0139699074 54771 54403.0227314815 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC21 267.484 -27.3686 1.83363899 -0.00346152 261.5433 54385.9113888889 54386.3127199074 502009010 20861.5 20000 20861.5 20861.5 0 20861.5 2 2 0 2 1 0 0 19648.3 19648.3 34663.9 1 PROCESSED 54402.5691319444 54771 54402.5769444444 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC22 266.3806 -28.337 0.50023196 0.3305092 262.5049 54386.3138888889 54386.785 502010010 21621.4 20000 21621.4 21621.4 0 21621.4 2 2 0 2 1 0 0 21194.4 21194.4 40662 1 PROCESSED 54402.6825347222 54771 54402.6900231482 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y GC23 266.578 -28.0524 0.83380185 0.3300796 262.2345 54386.7855208333 54387.2294444444 502011010 23013 20000 23013 23021 0 23029 1 1 0 1 1 0 0 22071.2 22071.2 38319.9 2 PROCESSED 54402.5213657407 54777 54402.5316898148 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020013 We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. GALACTIC DIFFUSE EMISSION 5 B KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU XIS Y HESS J1745-303 1 266.2249 -30.1096 358.91712668 -0.478438 70.5005 54527.7555555556 54529.7363310185 502016010 70529.1 67000 70537.1 70529.1 0 70545.1 2 2 0 2 1 0 0 61793.2 61793.2 171095.9 3 PROCESSED 54539.3010532407 54908 54539.3190509259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020023 A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. GALACTIC DIFFUSE EMISSION 5 B YAMAZAKI RYO NULL NULL JAP 2 AO2 SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 XIS Y HESS J1745-303 2 266.4705 -30.0867 359.0474588 -0.64781783 70.5003 54531.5601388889 54533.6669444444 502017010 72544.3 67000 72552.3 72552.3 0 72544.3 2 2 0 2 1 0 0 63972.3 63972.3 182014.9 2 PROCESSED 54550.3784027778 54919 54550.4057986111 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020023 A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. GALACTIC DIFFUSE EMISSION 5 B YAMAZAKI RYO NULL NULL JAP 2 AO2 SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 XIS Y HESS J1745-303 3 266.0567 -30.2413 358.72882707 -0.42335991 69.0003 54533.6682523148 54535.8752199074 502018010 79016.2 67000 79016.2 79040.2 0 79024.2 2 2 0 2 1 0 0 70201 70201 190658 2 PROCESSED 54550.3213773148 54919 54550.3420601852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020023 A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. GALACTIC DIFFUSE EMISSION 5 B YAMAZAKI RYO NULL NULL JAP 2 AO2 SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 XIS Y SGR D SNR 267.1922 -28.1274 1.05009547 -0.17236121 267.8977 54349.018599537 54352.6738310185 502020010 139080.8 133000 139080.8 139080.8 0 139080.8 2 2 0 2 1 0 0 124502.5 124502.5 315779.8 1 PROCESSED 54404.7849074074 54776 54371.5203472222 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020031 We propose a 100 ksec observation of the Sgr D region. This region contains a supernova remnant (SNR), a massive molecular cloud, an HII region and diffuse TeV gamma-ray emission. The objectives are to detect Sgr D SNR and diffuse X-rays from the TeV source, to discover new SNRs and X-ray Reflection Nebulae (XRNe), and to investigate the spatial distribution of high temperature plasma connecting the Galactic center and the Galactic ridge regions. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 2 AO2 OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS XIS Y ANTICENTER 113.3357 -19.5305 234.9976882 0.00424804 280.7829 54212.8606481482 54215.4197222222 502021010 89542.9 80000 89550.9 89558.9 0 89542.9 2 2 0 2 1 0 0 78988.7 78988.7 221050.8 3 PROCESSED 54330.0300578704 54744 54223.2040046296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020032 We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. Absolute measurement of the O VII and O VIII line fluxes will help establish the origin of this mysterious component of the diffuse background. This will allow a search for spectral signatures of non-thermal emission, i.e. charge- exchange emission, in the 3/4 keV band and the determination of abundances in hot gas thermal emission without risk of confusion by emission from hot gas in the Galactic Bulge. GALACTIC DIFFUSE EMISSION 5 B MASUI KENSUKE NULL NULL JAP 2 AO2 SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK XIS Y (L,B)=(0.25,-0.27) 266.8068 -28.8823 0.22878525 -0.27253682 265.3343 54343.5232986111 54346.7919560185 502022010 134790.4 133000 134798.4 134806.4 0 134790.4 2 2 0 2 1 0 0 116842.5 116842.5 282375.9 1 PROCESSED 54404.7619212963 54724 54356.5238657407 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020044 The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma with kT=6-7keV (GCDX). The comparison of Suzaku and VLA 90cm images show a hit for special correlation, suggest a magnetic confinement of GCDX. Thus, in order to search for new SNRs and investigate the galactic latitude dependency of the GCDX, we make a GC observation with the aiming point of (l,b)=(0.25, -0.27). We also see the correlation of GCDX with the radio. GALACTIC DIFFUSE EMISSION 5 B TSURU TAKESHI NULL NULL JAP 2 AO2 GLOBAL STRUCTURES OF THE GALACTIC CENTER DIFFUSE X-RAY PLASMA (GCDX) XIS Y VELA JR P1 131.9787 -45.8064 265.40235777 -1.43438498 347.0031 54285.3151273148 54285.6904398148 502023010 10649.6 10000 10649.6 10657.6 0 10657.6 2 2 0 2 1 0 0 9044.6 9044.6 32419.9 0 PROCESSED 54328.4144675926 54696 54328.4268402778 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P2 132.1691 -45.7748 265.4613949 -1.31133586 347.0033 54285.6908217593 54285.9036342593 502024010 10850.2 10000 10874.2 10866.2 0 10850.2 1 1 0 1 1 0 0 9603.7 9603.7 18375.9 0 PROCESSED 54328.4112037037 54696 54328.4167361111 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P3 132.1192 -45.6039 265.30669647 -1.23070071 347.0044 54285.9040162037 54286.1057175926 502025010 10298 10000 10298 10298 0 10298 1 1 0 1 1 0 0 6726 6726 17423.9 0 PROCESSED 54328.4405208333 54696 54328.4516782407 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P4 132.5157 -45.5453 265.43667302 -0.97855833 347.0031 54286.1062847222 54286.4480787037 502026010 10972.4 10000 10972.4 10972.4 0 10972.4 2 2 0 2 1 0 0 11295.9 11295.9 29511.9 1 PROCESSED 54328.4266435185 54759 54328.4405787037 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P5 132.9105 -45.488 265.56829981 -0.72857938 347.002 54286.4486458333 54286.7502777778 502027010 10977 10000 10977 10977 0 10977 1 1 0 1 1 0 0 10785.8 10785.8 26053.9 0 PROCESSED 54328.4557986111 54696 54328.4697800926 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P6 133.325 -45.4847 265.75161327 -0.50306307 347.0024 54286.7508449074 54286.9863888889 502028010 11507.2 10000 11531.2 11523.2 0 11507.2 1 1 0 1 1 0 0 8257.9 8257.9 20343.9 0 PROCESSED 54328.3799537037 54696 54328.3854166667 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P7 133.7759 -45.5828 266.02998701 -0.32446592 347.0033 54286.9870023148 54287.3023032407 502029010 14583.8 10000 14583.8 14583.8 0 14583.8 2 2 0 2 1 0 0 12605 12605 27239.9 0 PROCESSED 54328.4528125 54696 54328.4686111111 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P8 133.862 -45.8612 266.28131071 -0.45847751 347.0005 54287.3028240741 54287.7009722222 502030010 13219.6 10000 13219.6 13219.6 0 13219.6 2 2 0 2 1 0 0 14441 14441 34391.9 0 PROCESSED 54333.4437384259 54703 54333.4507175926 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P9 133.4161 -45.7633 266.00615013 -0.63304204 347.0009 54287.7015856482 54287.9516666667 502031010 13252.4 10000 13268.4 13252.4 0 13268.4 1 1 0 1 1 0 0 9887.7 9887.7 21599.9 0 PROCESSED 54333.4355671296 54703 54333.4413657407 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P10 132.9993 -45.7656 265.8217159 -0.85784968 347.0018 54287.9522337963 54288.2308564815 502032010 13040 10000 13048 13040 0 13056 2 2 0 2 1 0 0 10698.8 10698.8 24067.9 0 PROCESSED 54333.4252083333 54703 54333.4328240741 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P11 132.5986 -45.8258 265.69032827 -1.11165473 347.0024 54288.2314236111 54288.6112731482 502033010 11283.3 10000 11283.3 11283.3 0 11283.3 2 2 0 2 1 0 0 12207.9 12207.9 32790.1 1 PROCESSED 54328.396712963 54696 54328.4031944445 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P12 132.2515 -46.051 265.71195175 -1.4410688 347.0011 54289.0722106482 54289.4078009259 502034010 9947.9 10000 9947.9 9947.9 0 9947.9 1 1 0 1 1 0 0 10494 10494 28983.9 0 PROCESSED 54328.4737384259 54696 54328.4792939815 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P13 131.851 -46.106 265.57984888 -1.69160478 347.0011 54290.1290162037 54290.4411342593 502035010 9408.9 10000 9408.9 9408.9 0 9408.9 2 2 0 2 1 0 0 8953.1 8953.1 26963.9 0 PROCESSED 54328.4845949074 54696 54328.4906134259 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P14 131.9312 -46.3861 265.83284327 -1.824218 347.0017 54290.4416087963 54290.675150463 502036010 11034 10000 11034 11042 0 11042 1 1 0 1 1 0 0 11139.1 11139.1 20167.9 0 PROCESSED 54328.4693055556 54696 54328.4740277778 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P15 132.3334 -46.3288 265.96324441 -1.57253381 347.0016 54291.1946064815 54291.46 502037010 8876 10000 8876 8876 0 8876 2 2 0 2 1 0 0 7341.1 7341.1 22912.1 1 PROCESSED 54328.4606134259 54696 54328.472962963 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P16 132.6844 -46.1051 265.94403391 -1.24290223 347.0001 54291.4605671296 54291.7363773148 502038010 16442 10000 16450 16450 0 16442 1 1 0 1 1 0 0 16277 16277 23823.9 1 PROCESSED 54328.4918518518 54696 54328.4979398148 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P17 133.087 -46.0455 266.0760896 -0.98967894 347.0002 54291.7369444444 54291.9238773148 502039010 13032.6 10000 13064.5 13064.6 0 13032.6 1 1 0 1 1 0 0 8827.2 8827.2 16143.9 0 PROCESSED 54333.3993518518 54707 54333.4040277778 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y VELA JR P18 133.5064 -46.0415 266.25968404 -0.76370949 347.0006 54291.9244444444 54292.1668634259 502040010 15012.3 10000 15012.3 15036.2 0 15020.3 2 2 0 2 1 0 0 12895.2 12895.2 20943.9 1 PROCESSED 54328.4602199074 54696 54328.4716666667 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020049 We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 2 AO2 HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR XIS Y SN1006 225.7268 -41.9424 327.58003425 14.55159393 117.0193 54521.6264351852 54526.8613310185 502046010 211737.3 200000 211745.3 211737.3 0 211745.3 2 2 0 2 1 0 0 184362.2 184362.2 417275.9 6 PROCESSED 54535.6674884259 54904 54535.729375 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020052 Thermal plasma incident SN1006 has very interesting characteristic. Suzaku PV spectrum revealed ionization parameter of the plasma is significantly low. We investigated the spatial variation of the ionization parameter, and found the outer region of SN1006 has lower ionization parameter than the inner region. However, since the center region of SN1006 is placed on the edge of FOV in the PV observation, the spectra have poor statistics, and the ionization state and the metal abundance cannot be decided with good precision. We propose to observe the center region of SN1006 deeply to decide the physical condition of the plasma of young SNR. Necessary exposure time is 150ksec. GALACTIC DIFFUSE EMISSION 5 A YAMAGUCHI HIROYA NULL NULL JAP 2 AO2 THE CENTER REGION OF SN1006 XIS Y LOW_LATITUDE_86-21 332.3169 30.2173 86.0039952 -20.78963339 82.7457 54229.0809259259 54230.9966898148 502047010 81548.6 80000 81548.6 81548.6 0 81548.6 2 2 0 2 1 0 0 72293.1 72293.1 165509.9 2 PROCESSED 54328.7660069444 54744 54244.7948032407 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020061 High galactic-latitude Suzaku observations of soft X-ray diffuse emission so far made show general tendency that the OVII emission line becomes stronger with decreasing abs(b). This suggests that the major part of the emission is originating from the halo of our galaxy. However, we cannot rule out the possibility that the data is contaminated by solar wind charge exchange emission from the entire heliosphere. In oder to confirm the abs(b) dependency and to constrain the spatial distribution of the halo emission, we propose to observe diffuse radiation at a low galactic latitude of abs(b) ~ 20 deg, where the galactic absorption still does not affect the line intensity significantly. GALACTIC DIFFUSE EMISSION 5 B YOSHINO TOMOTAKA NULL NULL JAP 2 AO2 SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE XIS Y 47 TUCANAE 6.2112 -71.9961 305.8317488 -44.9821189 65.5967 54261.1765162037 54263.5404976852 502048010 132105.2 133000 132145.2 132105.2 0 132137.2 2 2 0 2 1 0 0 132904.2 132904.2 204231.9 1 PROCESSED 54329.1934375 54745 54271.5258796296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020066 We propose a 100 ks observation of the globular cluster 47 Tuc. An extended (~2') hard x-ray emission, presumably of non-thermal origin, was detected with Chandra from a position ~6' toward north east of its center. However, the Chandra ACIS spectrum does not allow us to determine with confidence whether it is a non-thermal emission or a high temperature thermal source. Utilizing the high sensitivity of the XIS, we try to distinguish between these two cases. If confirmed, the result may provide valuable information on particle acceleration in non-relativistic shocks, with potential relations the galactic-ridge x-ray emission. We perform a single pointing observation placing the center of the diffuse emission onto XIS nominal position. GALACTIC DIFFUSE EMISSION 5 B YUASA TAKAYUKI NULL NULL JAP 2 AO2 OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK XIS Y HESS J1702-420 255.6874 -42.0709 344.26217794 -0.21974248 106.4451 54550.458599537 54555.625162037 502049010 215693.2 200000 215705.3 215693.2 0 215705.3 2 2 0 2 1 0 0 140637.5 140637.5 395721.5 6 PROCESSED 54566.8834490741 54933 54566.9486458333 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020067 The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the most mysterious sample, HESS J1702-420, which has the brightest HESS compact source without clear counterparts. ASCA Galactic plane survey shows no evidence of X-ray emission although the exposure was too short. With the large effective area and the low background of XISs, we will be able to detect quite dim counterpart or make strong upper-limit in the hard X-ray band. This result will lead us to distinguish that HESS J1702-420 is the true "dark" protonic accelerator, or a hypothetical PWN powered by PSR J1702-4128. GALACTIC DIFFUSE EMISSION 5 B BAMBA AYA NULL NULL JAP 2 AO2 RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR XIS Y GC_G0.9+0.1 266.9332 -28.1474 0.91503767 0.01290063 105.8953 54536.2637152778 54540.229375 502051010 138761.4 133000 138761.4 138761.4 0 138761.4 2 2 0 2 1 0 0 122221.4 122221.4 342576.8 1 PROCESSED 54550.651087963 54919 54550.6988078704 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020071 The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 2 AO2 SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D XIS Y M17 EAST 275.3895 -16.2062 15.15230897 -0.92571433 271.9996 54377.3569907407 54380.0940277778 502052010 114569.5 107000 114577.5 114569.5 0 114577.5 2 2 0 2 1 0 0 100887.3 100887.3 236449.8 3 PROCESSED 54403.5124884259 54771 54403.5436111111 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020085 We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. GALACTIC DIFFUSE EMISSION 5 A TSUJIMOTO MASAHIRO NULL NULL JAP 2 AO2 FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - XIS Y M17 EAST BKG 275.6441 -15.5803 15.81995827 -0.84785909 271.9998 54380.0947800926 54381.7571064815 502053010 71494 67000 71494 71508.5 0 71502 2 2 0 2 1 0 0 62554.9 62554.9 143610 1 PROCESSED 54403.219212963 54771 54403.2344791667 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020085 We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. GALACTIC DIFFUSE EMISSION 5 A TSUJIMOTO MASAHIRO NULL NULL JAP 2 AO2 FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - XIS Y GALACTIC BULGE 268.3774 -29.9651 359.99980668 -2.0020922 279.4328 54372.0700347222 54375.590462963 502059010 136824 133000 136824 136824 0 136824 2 2 0 2 1 0 0 110515.6 110515.6 304130.6 2 PROCESSED 54402.6143981482 54770 54402.653275463 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020118 We propose a 100 ks observation on the Galactic Bulge (b=-2.0) with Suzaku. The origin of thermal diffuse X-ray emission will be for the first time clarified with a fine spectroscopy with Suzaku XIS, especially from the Fe-K line analysis. The non-thermal emission from the Galactic Bulge will be also investigated with HXD-PIN. GALACTIC DIFFUSE EMISSION 5 A KOKUBUN MOTOHIDE NULL NULL JAP 2 AO2 INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU XIS Y COMET_8P_TUTTLE-P1_BGD-1 28.5142 5.254 150.31676982 -54.25438929 248.4996 54471.3338888889 54471.5001273148 502061010 8390 6000 8390 8390 0 8390 1 1 0 1 1 0 0 7441.9 7441.9 14343.9 0 PROCESSED 54542.2523263889 54908 54542.2616319444 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1_BGD-2 28.5654 5.0072 150.57128999 -54.45813442 248.5002 54471.5006018518 54471.6876273148 502061020 5682.1 4000 5690.1 5682.1 0 5696.7 1 1 0 1 1 0 0 5598 5598 16151.9 0 PROCESSED 54542.2566666667 54908 54542.2619097222 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-1 27.7163 7.989 147.31647839 -52.04673223 248.4436 54470.5233333333 54470.5821759259 502062010 680.3 2000 680.3 680.3 0 680.3 1 1 0 1 1 0 0 632 632 5080 0 PROCESSED 54542.1940625 54908 54542.4502083333 2.2.7.18 4 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-2 27.9946 7.7582 147.87340904 -52.1573456 248.4994 54470.5826041667 54470.6488310185 502062020 2219.3 2000 2219.3 2219.3 0 2219.3 1 1 0 1 1 0 0 2164 2164 5718 0 PROCESSED 54542.2083912037 54908 54542.2129166667 2.2.7.18 4 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-3 28.0473 7.5049 148.10975305 -52.37174422 248.4997 54470.6493055556 54470.7154861111 502062030 1963.3 2000 1963.3 1963.3 0 1963.3 1 1 0 1 1 0 0 1905 1905 5718 0 PROCESSED 54542.2244212963 54908 54542.2294791667 2.2.7.18 4 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-4 28.0997 7.2516 148.34803657 -52.5857522 248.4989 54470.7159143518 54470.7821527778 502062040 1723.3 2000 1723.3 1723.3 0 1723.3 1 1 0 1 1 0 0 1456.7 1456.7 5722 0 PROCESSED 54542.2130787037 54908 54542.2187847222 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-5 28.1493 7.0036 148.58110255 -52.79544349 248.5006 54470.7825810185 54470.8487384259 502062050 1674.6 2000 1674.6 1674.6 0 1674.6 1 1 0 1 1 0 0 1703 1703 5686.1 0 PROCESSED 54542.198587963 54908 54542.2043055556 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-6 28.2017 6.7525 148.82276905 -53.00641332 248.5018 54470.8491666667 54470.9154050926 502062060 2026.6 2000 2026.6 2026.6 0 2026.6 1 1 0 1 1 0 0 2044 2044 5664 0 PROCESSED 54542.2264699074 54908 54542.2318634259 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-7 28.2572 6.4878 149.08057764 -53.2281425 248.4991 54470.9158333333 54470.9820717593 502062070 3219 2000 3219 3219 0 3219 1 1 0 1 1 0 0 3459 3459 5664 0 PROCESSED 54542.2344444444 54908 54542.2385532407 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-8 28.3076 6.2429 149.32011202 -53.43313536 248.4984 54470.9825 54471.0487384259 502062080 3219 3200 3219 3219 0 3219 1 1 0 1 1 0 0 3374 3374 5664 0 PROCESSED 54542.2187268518 54908 54542.2264583333 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-9 28.3593 5.9969 149.56477648 -53.63811023 248.4989 54471.0491666667 54471.1154050926 502062090 3218.6 3200 3218.6 3218.6 0 3218.6 1 1 0 1 1 0 0 2439 2439 5664 0 PROCESSED 54542.2309606482 54908 54542.2348611111 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-10 28.408 5.7525 149.8061723 -53.84230192 248.5015 54471.1158333333 54471.1820717593 502062100 3219.6 3200 3219.6 3219.6 0 3219.6 1 1 0 1 1 0 0 2166 2166 5679.9 0 PROCESSED 54542.2383912037 54908 54542.2429513889 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-11 28.4619 5.5053 150.05998726 -54.04643055 248.5015 54471.1825 54471.2487384259 502062110 3219 3200 3219 3219 0 3219 1 1 0 1 1 0 0 2035.6 2035.6 5688 0 PROCESSED 54542.2827314815 54908 54542.2871990741 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-12 28.5143 5.2526 150.31791041 -54.25562458 248.4993 54471.2491666667 54471.3154050926 502062120 3219.6 3200 3219.6 3219.6 0 3219.6 1 1 0 1 1 0 0 2162 2162 5696 0 PROCESSED 54542.2453703704 54908 54542.261400463 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P1-13 28.5683 5.0085 150.57488577 -54.45575395 248.5007 54471.3158333333 54471.3334606482 502062130 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1503.9 0 PROCESSED 54542.2384490741 54910 54544.4202893518 2.2.7.18 3 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_01 39.6412 -35.6843 240.18300744 -65.68930545 257.5577 54490.0082291667 54490.1627083333 502063010 4346.8 5000 4346.8 4346.8 0 4346.8 2 2 0 2 1 0 0 4402.9 4402.9 13327.9 1 PROCESSED 54546.0913194445 54912 54546.0974189815 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_02 39.704 -35.8295 240.49763907 -65.60654763 257.6692 54490.1630902778 54490.2960069444 502063020 5204.9 5000 5204.9 5204.9 0 5204.9 1 1 0 1 1 0 0 5591.9 5591.9 11449.9 0 PROCESSED 54546.1033101852 54912 54546.1091666667 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_03 39.7649 -35.9737 240.80897167 -65.5250468 257.7596 54490.2964351852 54490.4293287037 502063030 6038.9 6000 6054.9 6038.9 0 6054.9 2 2 0 2 1 0 0 6601.1 6601.1 11463.9 0 PROCESSED 54546.0981597222 54912 54546.1040046296 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_04 39.8249 -36.1145 241.11100541 -65.44459708 257.8515 54490.4297106482 54490.562662037 502063040 6687.6 6700 6687.6 6719.1 0 6687.6 1 1 0 1 1 0 0 7388.7 7388.7 11479.9 0 PROCESSED 54546.1084606482 54912 54546.1129513889 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_05 39.8852 -36.2545 241.40935004 -65.36366996 257.9439 54490.5630439815 54490.6959953704 502063050 6697.4 6700 6697.6 6697.6 0 6697.4 1 1 0 1 1 0 0 6161.9 6161.9 11479.9 0 PROCESSED 54546.1210648148 54912 54546.126712963 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_06 39.9457 -36.3936 241.70384829 -65.28238509 258.0349 54490.6963773148 54490.8293287037 502063060 6690.4 6700 6690.6 6690.6 0 6690.4 1 1 0 1 1 0 0 4338 4338 11479.9 0 PROCESSED 54546.1146527778 54912 54546.1201736111 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_07 40.0041 -36.5319 241.99586619 -65.20252382 258.1285 54490.8297106482 54490.962662037 502063070 5267.6 5000 5291.6 5267.6 0 5299.4 1 1 0 1 1 0 0 2753 2753 11479.9 0 PROCESSED 54546.1262268518 54912 54546.130462963 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_08 40.0642 -36.6693 242.2833952 -65.12116443 253.2206 54490.9649421296 54491.0959953704 502063080 3541.6 4000 3549.6 3541.6 0 3557.6 2 2 0 2 1 0 0 3564 3564 11311.9 0 PROCESSED 54546.1353472222 54912 54546.1411689815 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_09 40.126 -36.804 242.56232387 -65.03879756 253.3121 54491.0963773148 54491.2292824074 502063090 4397.9 4000 4397.9 4397.9 0 4397.9 1 1 0 1 1 0 0 4752 4752 11443.9 0 PROCESSED 54546.208912037 54912 54546.2142592593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_10 40.1849 -36.9375 242.83840601 -64.95862507 253.4045 54491.2297106482 54491.362662037 502063100 5730.4 5000 5738.4 5738.4 0 5730.4 2 2 0 2 1 0 0 6209.1 6209.1 11473.9 0 PROCESSED 54546.1898148148 54912 54546.1949884259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_11 40.2448 -37.071 243.11250517 -64.87732742 253.5002 54491.3630439815 54491.4959953704 502063110 6382.2 6700 6390.2 6382.2 0 6390.2 1 1 0 1 1 0 0 6838.5 6838.5 11479.9 0 PROCESSED 54546.1949884259 54912 54546.1994097222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_12 40.3045 -37.2045 243.38522043 -64.79583615 253.5926 54491.4963773148 54491.6293287037 502063120 6608.2 6700 6608.2 6608.2 0 6624.2 1 1 0 1 1 0 0 6469.8 6469.8 11479.9 0 PROCESSED 54546.2570949074 54912 54546.2619675926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_13 40.3641 -37.3366 243.65335896 -64.71445889 253.6857 54491.6297106482 54491.762662037 502063130 6590.7 6700 6614.7 6598.7 0 6590.7 1 1 0 1 1 0 0 5022.1 5022.1 11479.9 0 PROCESSED 54546.2157291667 54912 54546.2204861111 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_14 40.423 -37.4668 243.91615364 -64.63380941 253.7796 54491.7630439815 54491.8959953704 502063140 6562.7 6700 6562.7 6586.7 0 6562.7 1 1 0 1 1 0 0 3833 3833 11479.9 0 PROCESSED 54546.2526736111 54912 54546.2568518518 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_15 40.4836 -37.5961 244.17467378 -64.55180166 253.8725 54491.8963773148 54492.0293287037 502063150 3471.7 4000 3479.7 3471.7 0 3487.7 1 1 0 1 1 0 0 2346.1 2346.1 11479.9 1 PROCESSED 54546.2096527778 54912 54546.2153587963 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_16 40.5411 -37.7213 244.42429467 -64.47300408 253.9693 54492.0297106482 54492.162662037 502063160 3770.5 4000 3770.5 3770.5 0 3770.5 1 1 0 1 1 0 0 3988.1 3988.1 11479.9 0 PROCESSED 54546.2263541667 54912 54546.2311574074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_17 40.6015 -37.8518 244.68288405 -64.39021906 254.0645 54492.1630439815 54492.2959953704 502063170 5149.5 5000 5149.5 5149.5 0 5149.5 1 1 0 1 1 0 0 5414.2 5414.2 11432 0 PROCESSED 54546.2419560185 54912 54546.2465509259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_18 40.6547 -37.9803 244.9394556 -64.31314542 254.1595 54492.2963773148 54492.4293287037 502063180 6150.5 6000 6150.5 6150.5 0 6150.5 1 1 0 1 1 0 0 6613.3 6613.3 11479.9 0 PROCESSED 54546.232037037 54912 54546.2369675926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_BGD-1 40.599 -37.8517 244.68396515 -64.39213957 254.2787 54492.4296643518 54492.562662037 502064010 6570.7 5000 6570.7 6602.4 0 6586.7 1 1 0 1 1 0 0 6629.3 6629.3 11487.9 0 PROCESSED 54546.2370717593 54912 54546.2413888889 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y COMET_8P_TUTTLE-P2_BGD-2 40.4817 -37.5941 244.17118034 -64.55380496 254.4101 54492.5631365741 54492.7293287037 502064020 6979.7 5000 6979.7 7003.7 0 6987.7 1 1 0 1 1 0 0 5547.1 5547.1 14351.9 0 PROCESSED 54546.2484722222 54912 54546.2537847222 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021001 We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. GALACTIC DIFFUSE EMISSION 5 A BROWN GREGORY NULL NULL USA 2 AO2 SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE XIS Y G21.5-0.9 278.4035 -10.5067 21.56184596 -0.8687642 103.5554 54188.7945023148 54189.6252199074 502065010 25141.6 100000 25156 25141.6 0 25156 1 2 0 1 1 0 0 22889 22889 71769.9 1 PROCESSED 54324.3367592593 54695 54209.5181018518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021211 We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. GALACTIC DIFFUSE EMISSION 5 B HARRUS ILANA NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 HXD Y G21.5-0.9 278.4038 -10.5066 21.56207071 -0.86897985 103.5553 54190.0674074074 54191.7405671296 502065020 53526.1 100000 53526.1 53551 0 53566.1 1 2 0 1 1 0 0 48618 48618 144541.8 0 PROCESSED 54328.3614930556 54695 54200.5054861111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021211 We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. GALACTIC DIFFUSE EMISSION 5 B HARRUS ILANA NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 HXD Y G332.5-5.6 CENTER 250.7335 -54.5135 332.53119736 -5.54004522 262.5079 54330.694224537 54331.8731944444 502066010 70148.8 80000 70148.8 70148.8 0 70156.8 1 1 0 1 1 0 0 71490.7 71490.7 101839.9 0 PROCESSED 54404.7105324074 54721 54354.4910300926 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021216 We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. GALACTIC DIFFUSE EMISSION 5 B REYNOLDS STEPHEN NULL NULL USA 2 AO2 G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION XIS Y G332.5-5.6 NE 251.0925 -54.3783 332.77088512 -5.61037777 77.916 54504.4521296296 54505.6669444444 502067010 71192.6 80000 71200.6 71208.6 0 71192.6 2 2 0 2 1 0 0 65250.8 65250.8 104941.8 0 PROCESSED 54515.6833912037 54883 54515.6965509259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021216 We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. GALACTIC DIFFUSE EMISSION 5 B REYNOLDS STEPHEN NULL NULL USA 2 AO2 G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION XIS Y G296.1-0.5N 177.8287 -62.3875 296.02814016 -0.3243747 322.3815 54321.2538541667 54323.4522453704 502068010 77175.9 67000 77175.9 77175.9 0 77175.9 2 2 0 2 1 0 0 68484.6 68484.6 189923.7 1 PROCESSED 54404.8102777778 54716 54347.5137268518 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021218 Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. GALACTIC DIFFUSE EMISSION 5 B BORKOWSKI KAZIMIERZ NULL NULL USA 2 AO2 G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE XIS Y G296.1-0.5S 177.6962 -62.7172 296.04515802 -0.65925146 111.5869 54482.7727662037 54484.6668402778 502069010 69213 67000 69213 69213 0 69213 2 2 0 2 1 0 0 61009.6 61009.6 163623.7 2 PROCESSED 54515.097962963 54929 54563.4417824074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021218 Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. GALACTIC DIFFUSE EMISSION 5 C BORKOWSKI KAZIMIERZ NULL NULL USA 2 AO2 G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE XIS Y ARC1 40.8605 -42.0069 253.28744097 -62.75503946 235.1247 54480.7980787037 54482.7640509259 502070010 104369.4 100000 104377.4 104385.4 0 104369.4 2 2 0 2 1 0 0 115420.2 115420.2 169837.7 3 PROCESSED 54490.6791550926 54860 54490.7270717593 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021222 Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. GALACTIC DIFFUSE EMISSION 5 C SHELTON ROBIN NULL NULL USA 2 AO2 A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC XIS Y ARC2 39.9365 -39.101 247.81076012 -64.49485898 35.5401 54256.3120486111 54258.149525463 502071010 105727.1 100000 105735.1 105735.1 0 105727.1 2 2 0 2 1 0 0 82923.6 82923.6 158741.8 1 PROCESSED 54328.645775463 54702 54264.533275463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021222 Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. GALACTIC DIFFUSE EMISSION 5 B SHELTON ROBIN NULL NULL USA 2 AO2 A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC XIS Y ARC_BACKGROUND 39.8321 -35.8483 240.48423372 -65.50115915 257.6627 54496.6274537037 54499.812662037 502072010 0 100000 0 0 0 0 0 0 0 0 1 0 0 105161 105161 275153.7 4 PROCESSED 54515.3963888889 54883 54515.6371875 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021222 Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. GALACTIC DIFFUSE EMISSION 5 C SHELTON ROBIN NULL NULL USA 2 AO2 A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC XIS Y MBM20 68.9409 -14.6227 211.39642208 -36.55928879 252.4258 54507.612025463 54510.6980439815 502075010 107066.8 100000 107066.8 107066.8 0 107066.8 2 2 0 2 1 0 0 92803.6 92803.6 266603.6 2 PROCESSED 54522.4101851852 54889 54522.4496527778 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021224 We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. GALACTIC DIFFUSE EMISSION 5 B GALEAZZI MASSIMILIANO NULL NULL USA 2 AO2 STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 XIS Y ERIDANUS HOLE 67.1401 -17.0746 213.43674881 -39.09232011 64.2755 54311.0359606482 54313.2161921296 502076010 103752.3 100000 103752.3 103752.3 0 103752.3 2 2 0 2 1 0 0 92209.1 92209.1 188351.8 2 PROCESSED 54404.8421412037 54710 54340.7341898148 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021224 We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. GALACTIC DIFFUSE EMISSION 5 B GALEAZZI MASSIMILIANO NULL NULL USA 2 AO2 STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 XIS Y G54.1+0.3 292.6593 18.8091 54.05763723 0.20765467 245.096 54403.6644560185 54406.3335532407 502077010 101641.1 100000 101641.1 101649.1 0 101649.1 2 2 0 2 1 0 0 92923.5 92923.5 230585.7 3 PROCESSED 54417.7049074074 54786 54417.8870833333 2.1.6.16 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022032 A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae. GALACTIC DIFFUSE EMISSION 5 C BOCCHINO FABRIZIO NULL NULL EUR 2 AO2 THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3 HXD Y KEPLER 262.6698 -21.4886 4.51918955 6.82146946 98.2145 54514.1665393518 54516.9793287037 502078010 116963.6 100000 116963.6 116963.6 0 116963.6 2 2 0 2 1 0 0 98955.1 98955.1 242995.6 3 PROCESSED 54525.581412037 54894 54525.6176851852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 023074 We propose to observe the Kepler's SNR in which evidence of particle acceleration will be found. Aim of the observation is to determine power-law contribution in the hard-tail spectrum above 10 keV with HXD-PIN. If we also find the Fe-Kb and Ni-K emission lines with XIS which have not observed in any previous missions, temperature and nt parameter of a NEI model will be fixed. The determination will help to distinguish the power-law component from the thermal one. We also memtioned that the amount of Fe and Ni will be a good estimator to determine the type of Kepler's SNR. GALACTIC DIFFUSE EMISSION 5 B TAMAGAWA TORU Park Sangwook JUS 2 AO2 SEARCH FOR EVIDENCE OF COSMIC-RAY ACCELERATION IN THE KEPLER'S SNR XIS Y RCW86_WEST 220.2753 -62.427 315.24703456 -2.20673417 96.1553 54864.7563194444 54866.0134259259 503001010 53551.9 50000 53551.9 53551.9 0 53551.9 2 2 0 2 1 0 0 48908.1 48908.1 108602 1 PROCESSED 54962.1812268518 55329 54880.570462963 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030011 Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. GALACTIC DIFFUSE EMISSION 5 B YAMAGUCHI HIROYA NULL NULL JAP 3 AO3 RCW86 MAPPING OBSERVATION XIS Y RCW86_NORTH 220.4956 -62.2074 315.43082177 -2.04872285 96.1584 54860.901099537 54862.1175231482 503002010 55376 50000 55384 55384 0 55376 2 2 0 2 1 0 0 50273.1 50273.1 105081.8 2 PROCESSED 54962.1317361111 55329 54880.5551041667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030011 Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. GALACTIC DIFFUSE EMISSION 5 B YAMAGUCHI HIROYA NULL NULL JAP 3 AO3 RCW86 MAPPING OBSERVATION XIS Y RCW86_SOUTH 220.8315 -62.6734 315.37853465 -2.53716675 96.1597 54862.1182291667 54863.3647569445 503003010 54818.1 50000 54818.1 54818.1 0 54834.1 2 2 0 2 1 0 0 47348.3 47348.3 107684.8 1 PROCESSED 54962.3811805556 55329 54880.5892361111 2.3.12.25 3 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030011 Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. GALACTIC DIFFUSE EMISSION 5 B YAMAGUCHI HIROYA NULL NULL JAP 3 AO3 RCW86 MAPPING OBSERVATION XIS Y RCW86_SE 221.3859 -62.671 315.61056381 -2.64231092 96.79 54863.365787037 54864.7550115741 503004010 53327.4 50000 53359.4 53327.4 0 53359.4 2 2 0 2 1 0 0 47813.6 47813.6 119987.9 0 PROCESSED 54962.145 55329 54880.5420138889 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030011 Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. GALACTIC DIFFUSE EMISSION 5 B YAMAGUCHI HIROYA NULL NULL JAP 3 AO3 RCW86 MAPPING OBSERVATION XIS Y ANTICENTER2 12.9862 62.9112 122.98962226 0.03950805 69.9598 54679.0120717593 54680.8411921296 503006010 86110.1 80000 86123 86123 0 86110.1 2 2 0 2 1 0 0 106785 106785 158019.8 1 PROCESSED 54693.3033796296 55070 54693.3237847222 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030020 We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. The ROSAT 3/4 keV band all sky map does not show significant dip in intensity at galactic plane, where the CXB component is totally absorbed by galactic absorption. Thus unknown emission must be compensating the CXB component in this energy band. Our AO-2 observation of a general direction of the anticenter direction gives a clear clue to understand the origin of the mysterious emission. We propose to make additional observation in order to confirm the emission component detected in the AO-2 observation generally exist in the galactic plane. GALACTIC DIFFUSE EMISSION 5 B MASUI KENSUKE NULL NULL JAP 3 AO3 SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK XIS Y GC_LARGEPROJECT1 266.4387 -28.5683 0.32941305 0.16640393 260.8767 54711.4273958333 54712.9530555556 503007010 52152.3 50000 52152.3 52152.3 0 52152.3 2 2 0 2 1 0 0 44183.8 44183.8 131793.8 2 PROCESSED 54777.8369444444 54557 54780.6858796296 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT2 266.7785 -29.1292 0.00479668 -0.37932142 260.8763 54712.9538078704 54714.2891087963 503008010 53638.8 50000 53654.8 53638.8 0 53654.8 2 2 0 2 1 0 0 42811.1 42811.1 115333.8 0 PROCESSED 54777.7471759259 54557 54780.4880092593 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT3 266.4525 -29.3384 359.67825031 -0.24492188 260.8779 54714.2896759259 54715.6634722222 503009010 52397.5 50000 52405.5 52397.5 0 52411.4 2 2 0 2 1 0 0 40269.1 40269.1 118677.8 2 PROCESSED 54777.8299421296 54557 54780.6767476852 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT4 266.0398 -29.5556 359.30535174 -0.05184233 261.05 54715.6640393518 54717.0690277778 503010010 53105.6 50000 53121.6 53105.6 0 53113.6 2 2 0 2 1 0 0 37064.6 37064.6 121366 1 PROCESSED 54777.5397337963 54557 54780.6585648148 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT5 265.9469 -29.8331 359.02671432 -0.12852462 265.43 54717.3806597222 54718.8981365741 503011010 57633.4 50000 57633.4 57633.4 0 57633.4 2 2 0 2 1 0 0 40155.5 40155.5 131099.8 1 PROCESSED 54777.6566203704 54557 54780.6683912037 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT6 266.2992 -29.9408 359.09468885 -0.44519015 265.9621 54723.8160532407 54725.0348842593 503012010 57685.5 50000 57693.5 57685.5 0 57698.1 2 2 0 2 1 0 0 51903.2 51903.2 105287.8 1 PROCESSED 54777.4563657407 54557 54780.6521643518 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT7 265.6744 -30.0704 358.7007591 -0.05229538 265.9998 54725.0356365741 54727.1975 503013010 104769 100000 104777 104777 0 104769 2 2 0 2 1 0 0 93901.3 93901.3 186709.8 3 PROCESSED 54777.6505787037 54557 54780.5885532407 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT8 265.1842 -30.7499 357.90048261 -0.05223369 268.8911 54727.1991782407 54728.3141203704 503014010 55365.1 50000 55365.1 55389.1 0 55365.1 2 2 0 2 1 0 0 51206.9 51206.9 96311.8 1 PROCESSED 54777.8241550926 54557 54783.7018055556 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT9 265.0297 -30.9626 357.64981902 -0.05267713 269.1132 54728.3146412037 54729.4140393518 503015010 56771.6 50000 56779.6 56771.6 0 56787.6 2 2 0 2 1 0 0 52845.4 52845.4 94975.9 0 PROCESSED 54777.8057523148 54557 54780.4933564815 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT10 264.8736 -31.1751 357.39875369 -0.05245192 268.5898 54731.2832060185 54732.3383912037 503016010 52171.2 50000 52171.2 52179.2 0 52179.2 2 2 0 2 1 0 0 49291.3 49291.3 91163.9 1 PROCESSED 54777.7188888889 54557 54780.6078935185 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT11 264.7183 -31.3859 357.14965021 -0.05250387 268.3335 54732.3390046296 54733.3897337963 503017010 51286.5 50000 51294.5 51286.5 0 51302.5 2 2 0 2 1 0 0 48583.4 48583.4 90775.9 2 PROCESSED 54777.870625 54557 54780.6941550926 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT12 264.5602 -31.5978 356.8985011 -0.05173107 288.0843 54733.394375 54733.9377777778 503018010 29401.2 50000 29412.5 29412.5 0 29401.2 2 2 0 2 1 0 0 26671.6 26671.6 46942 0 PROCESSED 54777.7444444444 54557 54780.4814583333 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT12 264.5606 -31.5967 356.89961278 -0.05143068 268.4538 54742.7536226852 54743.154375 503018020 12246.6 10000 12246.6 12246.6 0 12246.6 2 2 0 2 1 0 0 10232 10232 34617.9 1 PROCESSED 54777.5525578704 54557 54780.5624652778 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT12 264.5561 -31.5945 356.89942182 -0.04701536 96.416 54881.313900463 54881.6919444445 503018030 11914 10000 11922 11922 0 11914 2 2 0 2 1 0 0 10090.9 10090.9 32657.9 1 PROCESSED 54962.381412037 54557 54895.5872106482 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT13 264.4001 -31.8052 356.65040302 -0.04773216 95.4712 54881.6929282407 54883.0522453704 503019010 52776.4 50000 52776.4 52797.2 0 52784.4 2 2 0 2 1 0 0 42439.5 42439.5 117433.8 0 PROCESSED 54963.067974537 54557 54902.1118171296 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT14 264.2413 -32.0163 356.39993487 -0.04727305 95.7088 54883.0527199074 54884.7911342593 503020010 61044.1 50000 61068.1 61044.1 0 61060.1 2 2 0 2 1 0 0 51718.5 51718.5 150131.9 1 PROCESSED 54962.4140972222 54557 54895.6029166667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y GC_LARGEPROJECT15 265.2338 -30.2129 358.37855715 0.19604348 267.777 54743.1555902778 54744.4565277778 503021010 53826 50000 53834 53834 0 53826 2 2 0 2 1 0 0 49640.5 49640.5 112378.1 0 PROCESSED 54777.4686921296 54557 54780.430150463 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030022 We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 3 AO3 ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE XIS Y LOOP 1 L=356.00 263.2426 -31.9466 356.00010804 0.70279756 93.3363 54908.96625 54909.8933333333 503022010 41319.3 40000 41319.3 41319.3 0 41319.3 2 2 0 2 1 0 0 34318.7 34318.7 80069.9 0 PROCESSED 54963.3456365741 55330 54923.2640162037 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030023 NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. GALACTIC DIFFUSE EMISSION 5 C YAMAUCHI SHIGEO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER XIS Y LOOP 2 L=356.33 263.4562 -31.667 356.33349006 0.70266893 94.2779 54916.2757060185 54917.0786921296 503023010 31152.7 40000 31152.7 31152.7 0 31152.7 2 2 0 2 1 0 0 28234.6 28234.6 69369.9 0 PROCESSED 54963.1729513889 55330 54930.234849537 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030023 NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. GALACTIC DIFFUSE EMISSION 5 C YAMAUCHI SHIGEO NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER XIS Y HESS J1800-240A 270.4845 -23.9659 6.13495239 -0.62617494 86.9255 54558.6209606482 54559.3266087963 503025010 34782.2 30000 34782.2 34790.2 0 34790.2 2 2 0 2 1 0 0 25703.3 25703.3 60967.9 0 PROCESSED 54574.0403587963 54953 54574.0504861111 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030043 H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. GALACTIC DIFFUSE EMISSION 5 A TANAKA TAKAAKI NULL NULL JAP 3 AO3 OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION XIS Y HESS J1800-240B 270.1124 -24.0578 5.8867537 -0.376417 87.1402 54562.3157523148 54563.0141666667 503026010 31672.8 30000 31672.8 31672.8 0 31672.8 1 1 0 1 1 0 0 26769.8 26769.8 60320 1 PROCESSED 54580.1709490741 54953 54580.1793402778 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030043 H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. GALACTIC DIFFUSE EMISSION 5 A TANAKA TAKAAKI NULL NULL JAP 3 AO3 OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION XIS Y HESS J1800-240C 269.7173 -24.0469 5.71665641 -0.05804766 87.3071 54563.0147337963 54563.6877662037 503027010 30975.5 30000 30975.5 30975.5 0 30975.5 2 2 0 2 1 0 0 27815.5 27815.5 58123.9 1 PROCESSED 54580.1815277778 54953 54580.1897453704 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030043 H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. GALACTIC DIFFUSE EMISSION 5 A TANAKA TAKAAKI NULL NULL JAP 3 AO3 OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION XIS Y HESS J1825-137 276.5024 -13.9965 17.60816681 -0.84042551 271.0002 54754.9096064815 54756.458599537 503028010 57210.4 50000 57210.4 57210.4 0 57210.4 2 2 0 2 1 0 0 51548.5 51548.5 133793.8 1 PROCESSED 54777.9353125 55148 54780.7053703704 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030044 The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. GALACTIC DIFFUSE EMISSION 5 B TANAKA TAKAAKI NULL NULL JAP 3 AO3 MAPPING OBSERVATIONS OF HESS J1825-137 XIS Y HESS_J1825-137_2 276.1969 -13.7002 17.73170044 -0.43977824 271.0001 54756.4591666667 54758.1953009259 503029010 57199.3 50000 57199.3 57199.3 0 57199.3 2 2 0 2 1 0 0 51185 51185 149985.8 0 PROCESSED 54777.9703819444 55148 54780.5081365741 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030044 The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. GALACTIC DIFFUSE EMISSION 5 B TANAKA TAKAAKI NULL NULL JAP 3 AO3 MAPPING OBSERVATIONS OF HESS J1825-137 XIS Y HESS_J1825-137_3 276.1966 -13.9971 17.46909054 -0.57831059 271.0001 54758.195775463 54759.7917476852 503030010 55499.6 50000 55499.6 55499.6 0 55499.6 2 2 0 2 1 0 0 47325.2 47325.2 137837.9 1 PROCESSED 54778.0046064815 55148 54780.7804050926 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030044 The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. GALACTIC DIFFUSE EMISSION 5 B TANAKA TAKAAKI NULL NULL JAP 3 AO3 MAPPING OBSERVATIONS OF HESS J1825-137 XIS Y VELA JR P19 133.9797 -46.1476 266.55257885 -0.58147519 346.9993 54650.629849537 54651.2362731482 503031010 19817.4 10000 19817.4 19817.4 0 19817.4 2 2 0 2 1 0 0 17156.4 17156.4 52383.9 1 PROCESSED 54665.2314699074 55036 54665.3240393518 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P20 133.6175 -46.3272 266.52787238 -0.88873335 346.9997 54651.2368402778 54651.5828009259 503032010 16823.7 10000 16823.7 16831.7 0 16831.7 1 1 0 1 1 0 0 14798.2 14798.2 29887.9 0 PROCESSED 54665.19875 55036 54665.3228125 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P21 133.1972 -46.3295 266.34323773 -1.11269222 347.0005 54651.5833680556 54652.0557175926 503033010 14287.2 10000 14295.2 14287.2 0 14303.2 2 2 0 2 1 0 0 12066.5 12066.5 40801.9 1 PROCESSED 54665.2108796296 55036 54665.3234375 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P22 132.4428 -46.6127 266.23093455 -1.69368029 346.9992 54652.0565625 54652.3891087963 503034010 15264.3 10000 15264.3 15270.9 0 15270.9 2 2 0 2 1 0 0 14971.7 14971.7 28728 0 PROCESSED 54670.1272685185 55036 54670.1353125 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P23 132.7881 -46.3947 266.21323714 -1.3716571 347.0013 54652.3896759259 54652.7710416667 503035010 15690.1 10000 15698.1 15690.1 0 15706.1 1 1 0 1 1 0 0 11039 11039 32943.9 1 PROCESSED 54664.2194907407 55031 54664.7904513889 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P24 132.0303 -46.6729 266.0989339 -1.95139979 347.001 54652.7719328704 54653.1668865741 503036010 12373.5 10000 12373.5 12373.5 0 12373.5 2 2 0 2 1 0 0 12254.8 12254.8 34120 1 PROCESSED 54679.3105671296 55048 54679.3185763889 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P25 132.5224 -46.8921 266.48184745 -1.82836861 347.0024 54653.1675462963 54653.4335532407 503037010 13160 10000 13160 13160 0 13160 1 1 0 1 1 0 0 12432.5 12432.5 22975.9 0 PROCESSED 54679.3099884259 55048 54679.3166203704 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P26 132.8787 -46.6693 266.46476457 -1.49839932 347.0019 54653.4341203704 54653.837025463 503038010 14553 10000 14553 14553 0 14553 1 1 0 1 1 0 0 10953.6 10953.6 34783.9 0 PROCESSED 54679.3635300926 55048 54679.3709606482 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P27 133.2844 -46.6061 266.59417196 -1.24373956 347.0008 54653.8375925926 54654.1668865741 503039010 11033.7 10000 11041.7 11041.7 0 11033.7 1 1 0 1 1 0 0 11337.2 11337.2 28447.9 0 PROCESSED 54679.3267824074 55048 54679.3497222222 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P28 133.7109 -46.6037 266.78076878 -1.01777641 347.0004 54654.1674537037 54654.4259143518 503040010 13093 10000 13101 13093 0 13101 1 1 0 1 1 0 0 12054 12054 22296 0 PROCESSED 54679.3607291667 55048 54679.3674421296 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P29 134.0711 -46.43 266.80859879 -0.71638658 347 54654.4264814815 54654.7203703704 503041010 11368.5 10000 11380.2 11368.5 0 11380.2 1 1 0 1 1 0 0 8222.5 8222.5 25367.9 0 PROCESSED 54679.388599537 55048 54679.3958217593 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P30 134.1665 -46.7036 267.059354 -0.84402772 347.0006 54654.7208449074 54655.0844328704 503042010 10115.9 10000 10115.9 10115.9 0 10115.9 2 2 0 2 1 0 0 10053.6 10053.6 31383.9 0 PROCESSED 54679.3883912037 55048 54679.397962963 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P31 133.8003 -46.8845 267.03483855 -1.15221367 347.0003 54655.085 54655.3273032407 503043010 11209.5 10000 11217.5 11225.5 0 11209.5 1 1 0 1 1 0 0 11542 11542 20927.9 0 PROCESSED 54679.3658217593 55048 54679.372974537 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P32 133.3695 -46.8865 266.8467839 -1.37881435 347.0018 54655.3279166667 54655.5648032407 503044010 11264.9 10000 11272.9 11264.9 0 11280.9 1 1 0 1 1 0 0 8337.5 8337.5 20455.9 0 PROCESSED 54679.3747569444 55048 54679.381087963 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P33 133.4681 -47.1616 267.10091899 -1.50393046 347.0007 54655.5652777778 54656.0084837963 503045010 12015.5 10000 12015.5 12015.5 0 12015.5 2 2 0 2 1 0 0 11011.6 11011.6 38289.9 0 PROCESSED 54679.4111342593 55048 54679.4195601852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P34 132.1138 -46.9499 266.35035002 -2.0812575 347.0005 54656.0096990741 54656.2634143518 503046010 11042.1 10000 11058.1 11042.1 0 11058.1 2 2 0 2 1 0 0 11130.6 11130.6 21916 0 PROCESSED 54670.2165740741 55037 54670.2236342593 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P35 132.966 -46.9473 266.71715615 -1.62954887 347.0008 54656.2642592593 54656.5141087963 503047010 11562.1 10000 11586.1 11562.1 0 11594.1 1 1 0 1 1 0 0 9619.8 9619.8 21583.9 0 PROCESSED 54670.2250694444 55037 54670.2319212963 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P36 133.0606 -47.2239 266.97132611 -1.75647675 346.9998 54656.5145833333 54656.9168634259 503048010 11122.6 10000 11130.6 11122.6 0 11138.6 2 2 0 2 1 0 0 9383.8 9383.8 34749.9 1 PROCESSED 54670.2613194444 55037 54670.2692361111 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P37 132.6136 -47.1701 266.73640279 -1.95651055 346.9993 54656.9174768518 54657.2418287037 503049010 12529.4 10000 12541.4 12529.4 0 12545.4 2 2 0 2 1 0 0 12852.7 12852.7 28020 0 PROCESSED 54670.2703240741 55037 54670.278900463 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y VELA JR P38 132.2003 -47.2308 266.60579829 -2.21244802 347.0003 54657.2423958333 54657.5209953704 503050010 14043.6 10000 14043.6 14043.6 0 14059.6 1 1 0 1 1 0 0 11426 11426 24063.9 0 PROCESSED 54670.249849537 55037 54670.2561111111 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030048 We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. GALACTIC DIFFUSE EMISSION 5 A UCHIYAMA YASUNOBU NULL NULL JAP 3 AO3 COMPLETING SUZAKU MAPPING OF VELA JR SNR XIS Y WESTERLUND 2 156.0088 -57.7448 284.2643696 -0.3172737 343.7602 54687.6527199074 54689.327962963 503053010 73670 100000 73670 73670 0 73670 2 2 0 2 1 0 0 86577.6 86577.6 144729.8 0 PROCESSED 54706.4623263889 55252 54706.476412037 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030059 Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. GALACTIC DIFFUSE EMISSION 5 A FUJITA YUTAKA NULL NULL JAP 3 AO3 NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 XIS Y WESTERLUND 2 155.9878 -57.7462 284.25564056 -0.32444098 166.5036 54866.5949189815 54867.1669444444 503053020 33492.4 30000 33500.4 33492.4 0 33500.4 2 2 0 2 1 0 0 32073 32073 49415.9 1 PROCESSED 54963.3371180556 55329 54880.5574189815 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030059 Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. GALACTIC DIFFUSE EMISSION 5 A FUJITA YUTAKA NULL NULL JAP 3 AO3 NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 XIS Y RCW 38 134.7638 -47.5154 267.93999829 -1.06526988 109.8553 54788.5064351852 54790.699525463 503054010 81537.7 80000 81549.5 81537.7 0 81541.5 2 2 0 2 1 0 0 60928.1 60928.1 189459.7 1 PROCESSED 54802.3985416667 55171 54811.741099537 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030069 We propose to make Suzaku observation of HII region RCW 38 for 80 ksec in order to study non-thermal phenomena in a massive star-forming region. The region is thought to be a site of high energy particle acceleration by interaction of strong stellar wind from high-mass stars. The main purpose is to observe extended emission from RCW 38. The high resolution spectroscopy by XIS enables us to distinguish non-thermal emission from thermal component and to obtain properties of non-thermal component. In addition, HXD will detect non-thermal radiation from RCW 38. GALACTIC DIFFUSE EMISSION 5 C ODAKA HIROKAZU NULL NULL JAP 3 AO3 SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38 XIS Y CYGNUS LOOP (P11) 312.4425 31.5127 74.4826992 -7.83027866 49.9999 54595.9014814815 54596.7391087963 503055010 31894.7 25000 31902.7 31894.7 0 31910.7 2 2 0 2 1 0 0 25073.8 25073.8 72359.9 0 PROCESSED 54606.1312731482 54972 54606.1436342593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P20) 311.9894 31.1824 73.97872298 -7.73281487 50.0002 54596.7397685185 54597.51 503056010 30112.9 25000 30112.9 30134.3 0 30120.9 2 2 0 2 1 0 0 27205.7 27205.7 66533.9 0 PROCESSED 54606.1028819444 54972 54606.1121759259 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P21) 313.196 32.4197 75.60030214 -7.75821821 61.9243 54619.9401967593 54620.2975 503057010 16170.3 15000 16178.3 16170.3 0 16178.3 1 1 0 1 1 0 0 12890.3 12890.3 30863.9 0 PROCESSED 54636.2162615741 55003 54636.2238078704 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P22) 312.8353 32.4047 75.39493092 -7.53123997 61.4354 54620.2981134259 54620.7522453704 503058010 19287.3 15000 19287.3 19287.3 0 19287.3 2 2 0 2 1 0 0 17220.3 17220.3 39212 0 PROCESSED 54636.272337963 55003 54636.2807638889 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P23) 312.4772 32.3587 75.1675214 -7.32455162 61.8892 54620.7530439815 54621.1473842593 503059010 19457 15000 19457 19457 0 19457 1 1 0 1 1 0 0 17277.1 17277.1 34063.9 0 PROCESSED 54636.2250347222 55003 54636.2328240741 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P24) 312.134 32.2905 74.93132331 -7.14055521 61.3941 54621.1479513889 54621.6271875 503060010 18504.6 15000 18504.6 18504.6 0 18504.6 2 2 0 2 1 0 0 14999 14999 41397.9 1 PROCESSED 54636.2930787037 55003 54637.4594675926 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P25) 311.8608 32.1678 74.68970828 -7.03578766 60.8878 54621.6278472222 54622.1488888889 503061010 25995.9 20000 25995.9 25995.9 0 25995.9 2 2 0 2 1 0 0 23879.1 23879.1 45010 0 PROCESSED 54636.2414351852 55003 54636.2508217593 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P26) 314.1252 30.3135 74.46090737 -9.70687059 49.7995 54599.1203587963 54599.5474421296 503062010 16924.7 15000 16924.7 16932.7 0 16932.7 2 2 0 2 1 0 0 15441 15441 36892 1 PROCESSED 54609.1213078704 54975 54609.1293981482 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P27) 313.8328 30.0104 74.06049539 -9.7037521 49.6211 54599.5480092593 54600.0494675926 503063010 22784.3 20000 22792.3 22784.3 0 22800.3 2 2 0 2 1 0 0 20068.8 20068.8 43323.9 0 PROCESSED 54609.1316898148 54975 54609.1396990741 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y CYGNUS LOOP (P28) 313.4797 29.8934 73.77252886 -9.54040793 49.1005 54600.0501273148 54600.5334953704 503064010 18169.3 15000 18177.3 18185.3 0 18169.3 2 2 0 2 1 0 0 16443 16443 41756 0 PROCESSED 54609.1814814815 54975 54609.1904282407 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030074 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATIONS OF THE CYGNUS LOOP XIS Y RABBIT 214.6544 -60.9713 313.31134091 0.131367 105.7763 54876.850787037 54877.5224421296 503071010 21274 20000 21282 21274 0 21290 1 1 0 1 1 0 0 18012.6 18012.6 57984 0 PROCESSED 54962.2228356482 55330 54892.945162037 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030076 K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. GALACTIC DIFFUSE EMISSION 5 C KISHISHITA TETSUICHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 XIS Y EXTENDED CHIMNEY 265.9856 -29.2095 359.57541621 0.16970004 69.9995 54896.1105555556 54899.1218171296 503072010 140573.3 133000 140573.3 140573.3 0 140573.3 2 2 0 2 1 0 0 135478.4 135478.4 260128 1 PROCESSED 54963.3178935185 55330 54916.5067361111 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030086 We have discovered a chimney structure in the Sgr C region with Suzaku. The Suzaku spectrum of the chimney shows typical parameters of a super nova remnant. However, the chimney has a linear shape, which is inconsistent with a SNR. Thus, we are considering that the chimney is a blowout from super bubble in the Sgr C region. Another possible scenario is that the chimney would be a part of a shell structure formed by explosions (starburst activities, Sgr A*, magnetic reconnection) in the region of Sgr A and Sgr C. Thus, in this proposal, we would like to investigate the structure extending from the chimney. GALACTIC DIFFUSE EMISSION 5 B TSURU TAKESHI NULL NULL JAP 3 AO3 THE CHIMNEY OF SGR C : A PART OF A SUPER BUBBLE = A SUPER SHELL ? XIS Y HESSJ1614-A 243.5214 -52.1022 331.29897546 -0.76107386 283.3889 54729.7629050926 54730.562662037 503073010 53649.4 50000 53657.4 53649.4 0 53665.4 1 1 0 1 1 0 0 40871.3 40871.3 69071.9 0 PROCESSED 54777.4405092593 55148 54780.4246990741 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030088 The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 MAPPING OBSERVATION OF HESSJ1614-518 XIS Y HESSJ1614-B 243.5783 -51.8962 331.46625372 -0.63583262 283.7142 54730.5632291667 54731.2779166667 503074010 52634.2 50000 52642.2 52634.2 0 52634.2 2 2 0 2 1 0 0 42953 42953 61735.9 0 PROCESSED 54777.6201157407 55148 54780.4609490741 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030088 The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 MAPPING OBSERVATION OF HESSJ1614-518 XIS Y LOW_LATITUDE_97-10 311.8076 60.1112 96.61384914 10.40907029 101.0346 54571.1324652778 54572.8890509259 503075010 79811.9 80000 79819.9 79827.9 0 79811.9 2 2 0 2 1 0 0 80810.5 80810.5 151749.8 2 PROCESSED 54581.3064236111 54953 54581.3271643518 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030105 Suzaku observations of diffuse background emission indicate galactic-latitude dependence of OVII intensity. The result of our AO-2 observation strongly supports this dependence. This suggests that the major part of the emission is originating from the halo or the extended disk of our galaxy. In order to confirm the galactic-latitude dependency and to constrain the spatial distribution of the OVII emitting gas, we propose to observe diffuse radiation at a low galactic latitude of ~ 10 deg. GALACTIC DIFFUSE EMISSION 5 B YOSHINO TOMOTAKA NULL NULL JAP 3 AO3 RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION XIS Y HESSJ1741-A 265.3548 -30.1316 358.50289854 0.15030933 73.8229 54886.7117013889 54888.0419328704 503076010 52932.3 50000 52932.3 52932.3 0 52932.3 2 2 0 2 1 0 0 43770.8 43770.8 114915.8 1 PROCESSED 54963.002025463 55330 54902.4869791667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030113 HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. GALACTIC DIFFUSE EMISSION 5 C MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 XIS Y HESSJ1741-B 265.2407 -30.3098 358.29952005 0.1396669 74.0024 54888.0423611111 54889.4828587963 503077010 51261.6 50000 51269.6 51261.6 0 51269.6 2 2 0 2 1 0 0 43707.2 43707.2 124423.9 1 PROCESSED 54962.9170949074 55330 54908.5791550926 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030113 HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. GALACTIC DIFFUSE EMISSION 5 C MATSUMOTO HIRONORI NULL NULL JAP 3 AO3 DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 XIS Y HESS_J1809-193_N 272.4044 -19.3551 11.02929838 0.07166066 112.001 54556.5874421296 54557.6877662037 503078010 51530.9 40000 51538.9 51530.9 0 51546.1 2 2 0 2 1 0 0 34818.6 34818.6 95051.8 2 PROCESSED 54571.3490509259 54950 54571.3638888889 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030126 A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. GALACTIC DIFFUSE EMISSION 5 A ANADA TAKAYASU NULL NULL JAP 3 AO3 INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 XIS Y HESS_J1809-193_S 272.3365 -19.5311 10.84429394 0.04252392 106.4999 54557.6901851852 54558.6161805556 503079010 44248.1 40000 44248.1 44248.1 0 44248.1 2 2 0 2 1 0 0 32214.2 32214.2 79969.8 1 PROCESSED 54570.1730208333 54950 54570.1866666667 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030126 A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. GALACTIC DIFFUSE EMISSION 5 A ANADA TAKAYASU NULL NULL JAP 3 AO3 INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 XIS Y CAS A 351.0231 59.0265 111.88943817 -1.95981315 208.1115 54876.0965740741 54876.8363310185 503080010 30035.5 30000 30035.5 30035.5 0 30035.5 2 2 0 2 1 0 0 30073.1 30073.1 63913.9 0 PROCESSED 54963.3651388889 55330 54892.9889699074 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030127 Cas A is the youngest supernova remnant(SNR) in our Galaxy. Recently, the Spitzer Space Telescope discovered moving structures nearly at the speed of light outside the shell of the SNR. These structures are likely infrared echoes, where interstellar dust is heated by the outward moving photon shell of a bright flash. The bright flash is probably due to a giant flare from the central point source of Cas A, and if so, it requires that the central point source is a magnetar. Magnetars are known to emit luminous flares in the X-ray band, so it is expected that we can detect Fe-K fluorescence emission accompanied by IR echo. Here, we propose to observe on IR-emitting cloud around Cas A for 30ks to search for Fe-K emission which is naturally expected if the central point source is a magnetar. GALACTIC DIFFUSE EMISSION 5 C AONO HIROYUKI NULL NULL JAP 3 AO3 INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A XIS Y GC(0,-1.6) 268.0544 -29.7594 0.03481768 -1.65633011 65.7488 54899.6540509259 54900.8168865741 503081010 59223.3 50000 59223.3 59223.3 0 59223.3 2 2 0 2 1 0 0 57601.8 57601.8 100453.8 1 PROCESSED 54963.2991782407 55330 54916.3813194444 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030131 We propose a 50 ksec observation of very enigmatic diffuse structure at 1.6 degree south from the Galactic center. We first discovered this structure with ROSAT. Then with ASCA, we found that the spectrum exhibits thin thermal emission accompanied with a hard tail which may be nonthermal radiation from high energy electrons. These results imply presence of a strong shock in this region, possibly due to a jet from Sgr A*. The diffuse emission may be a fossil of the past activities. With the observation of Suzaku, we obtain the richest statistics ever achieved. Then we will reveal the shock front from the image, and verify the past activities of the massive blackhole. GALACTIC DIFFUSE EMISSION 5 B MURAKAMI HIROSHI NULL NULL JAP 3 AO3 NEW EVIDENCE OF THE PAST ACTIVITY IN THE GALACTIC CENTER REGION XIS Y VICINITY_OF_PKS_2155-1 329.2367 -30.5281 17.16872193 -51.86657338 55.8337 54585.7726736111 54588.3542592593 503082010 90181.2 80000 90181.2 90181.2 0 90181.2 2 2 0 2 1 0 0 76792.1 76792.1 223023.7 4 PROCESSED 54608.3057291667 54975 54608.3373726852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030135 The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. GALACTIC DIFFUSE EMISSION 5 A HAGIHARA TOSHISHIGE NULL NULL JAP 3 AO3 STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 XIS Y VICINITY_OF_PKS_2155-2 330.1861 -29.9649 18.22929909 -52.62033555 55.8323 54588.3553356482 54590.7293865741 503083010 87327.4 80000 87327.4 87327.4 0 87327.4 2 2 0 2 1 0 0 75845.1 75845.1 205105.9 3 PROCESSED 54608.235625 54975 54608.2608912037 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030135 The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. GALACTIC DIFFUSE EMISSION 5 A HAGIHARA TOSHISHIGE NULL NULL JAP 3 AO3 STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 XIS Y W49B 287.7847 9.1157 43.28157058 -0.18360003 89.2671 54919.1063888889 54920.4689583333 503084010 52154.9 40000 52154.9 52154.9 0 52154.9 2 2 0 2 1 0 0 43951.2 43951.2 117709.9 2 PROCESSED 54963.0818171296 55330 54931.3622106482 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030142 Observations of the W49B supernova remnant for 40 ks is proposed to reveal whether it is a remnant of an anomalous Type Ia supernova or not. To determine the type of the supernova, detailed measurement of less abundand elements such as Cr and Mn will be performed, and abundance of Ni and Ti will be examined. The abundance pattern of those elements in W49B will be compared to that of Tycho's SNR we measured by Suzaku. GALACTIC DIFFUSE EMISSION 5 C TAMAGAWA TORU NULL NULL JAP 3 AO3 IS W49B A REMNANT OF AN ANOMALOUS TYPE IA SUPERNOVA? XIS Y TYCHO SNR 6.3139 64.1469 120.08177164 1.42013769 53.7834 54682.0646759259 54686.9529398148 503085010 312892 400000 312916 312892 0 312908 2 2 0 2 1 0 0 289949.4 289949.4 307869.9 3 PROCESSED 54706.9683680556 54557 54707.038287037 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031003 Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. GALACTIC DIFFUSE EMISSION 5 A HUGHES JOHN NULL NULL USA 3 AO3 SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS XIS Y TYCHO SNR 6.3115 64.1447 120.08050675 1.41805528 43.1557 54689.3425578704 54690.918275463 503085020 102855.6 100000 102855.6 102855.6 0 102855.6 2 2 0 2 1 0 0 91907.8 91907.8 136103.9 1 PROCESSED 54706.7655555556 54557 54706.7896412037 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031003 Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. GALACTIC DIFFUSE EMISSION 5 A HUGHES JOHN NULL NULL USA 3 AO3 SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS XIS Y G18.0-0.7 276.56 -13.5781 18.00442084 -0.69482715 92.0001 54909.8982060185 54911.080775463 503086010 52059.2 50000 52059.2 52067.2 0 52067.2 2 2 0 2 1 0 0 46303.6 46303.6 102145.8 2 PROCESSED 54962.5928009259 55329 54923.3684490741 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031203 By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. GALACTIC DIFFUSE EMISSION 5 C GELFAND JOSEPH NULL NULL USA 3 AO3 STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE XIS Y G12.8-0.0 273.3975 -17.831 12.81826803 -0.01988984 90.5577 54894.8233680556 54896.1050810185 503087010 56202.6 50000 56202.6 56202.6 0 56205.9 2 2 0 2 1 0 0 51531.2 51531.2 110727.8 1 PROCESSED 54963.0907986111 55329 54908.5701388889 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031203 By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. GALACTIC DIFFUSE EMISSION 5 C GELFAND JOSEPH NULL NULL USA 3 AO3 STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE XIS Y B1920+10(1) 293.0298 10.9618 47.34140504 -3.87470613 252.2888 54772.350462963 54774.137662037 503090010 73603.3 70000 73612.4 73603.3 0 73611.3 2 2 0 2 1 0 0 66668.2 66668.2 154403.9 3 PROCESSED 54788.2123263889 55154 54788.4472337963 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031204 A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. GALACTIC DIFFUSE EMISSION 5 C MISANOVIC ZDENKA NULL NULL USA 3 AO3 STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU XIS Y B1920+10(2) 292.8971 10.8605 47.18977478 -3.80874006 248.6642 54783.7420833333 54785.8981365741 503091010 100457.7 100000 100457.7 100457.7 0 100457.7 2 2 0 2 1 0 0 93873.1 93873.1 186248 0 PROCESSED 54797.1290856482 55167 54797.1537731482 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031204 A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. GALACTIC DIFFUSE EMISSION 5 C MISANOVIC ZDENKA NULL NULL USA 3 AO3 STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU XIS Y HESS J1023-575 155.5616 -57.7533 284.06754503 -0.45248582 284.3289 54617.1411458333 54617.4515509259 503092010 13826 10000 13826 13826 0 13826 1 1 0 1 1 0 0 11057.3 11057.3 26815.9 1 PROCESSED 54630.1961574074 54999 54633.6961458333 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031207 We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts. GALACTIC DIFFUSE EMISSION 5 B ROBERTS MALLORY NULL NULL USA 3 AO3 SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES XIS Y SNR 0049-73.6 12.7817 -73.3677 302.96274339 -43.76053264 62.7682 54629.4818518518 54632.7605787037 503094010 120478 120000 120486 120478 0 120486 2 2 0 2 1 0 0 107707.9 107707.9 283241.9 3 PROCESSED 54642.5679398148 55008 54642.6050694444 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031211 We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6. GALACTIC DIFFUSE EMISSION 5 B PARK SANGWOOK NULL NULL USA 3 AO3 OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC XIS Y VELA FRAGMENT C 136.2696 -44.691 266.51473212 1.58715492 269.3614 54580.6978703704 54582.3056481482 503095010 84116.7 70000 84116.7 84116.7 0 84116.7 2 2 0 2 1 0 0 91354.7 91354.7 138901.8 2 PROCESSED 54594.2301273148 54960 54594.2480324074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031212 Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. GALACTIC DIFFUSE EMISSION 5 B GAETZ TERRANCE NULL NULL USA 3 AO3 SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS XIS Y VELA FRAGMENT E 119.9016 -44.3755 259.34445053 -7.61175769 281.1138 54582.309224537 54583.7849421296 503096010 79200.4 70000 79218.9 79200.4 0 79232.4 2 2 0 2 1 0 0 84252.9 84252.9 127489.9 1 PROCESSED 54594.1961805556 54960 54594.2098842593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031212 Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. GALACTIC DIFFUSE EMISSION 5 B GAETZ TERRANCE NULL NULL USA 3 AO3 SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS XIS Y GCL1 265.1726 -28.5274 359.7799359 1.13423351 69.7267 54900.8188425926 54901.4557175926 503099010 29706 25000 29724.1 29722 0 29706 2 2 0 2 1 0 0 30564.9 30564.9 55020 1 PROCESSED 54963.1238310185 55329 54916.3706828704 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031234 We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. GALACTIC DIFFUSE EMISSION 5 B YUSEF-ZADEH FARHAD NULL NULL USA 3 AO3 A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? XIS Y GCL2 264.8888 -28.9255 359.31035513 1.13376438 106.9569 54905.2789467593 54905.9169444444 503100010 25717.9 25000 25717.9 25717.9 0 25717.9 1 1 0 1 1 0 0 24146 24146 55119.9 1 PROCESSED 54963.2315162037 55329 54917.3744675926 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031234 We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. GALACTIC DIFFUSE EMISSION 5 B YUSEF-ZADEH FARHAD NULL NULL USA 3 AO3 A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? XIS Y GCL3 265.2728 -28.8569 359.5469331 0.88519 106.9023 54906.6133912037 54907.3252777778 503101010 33891.1 25000 33899.1 33899.1 0 33891.1 2 2 0 2 1 0 0 30830.9 30830.9 61497.9 0 PROCESSED 54962.8099537037 55329 54917.3115393518 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031234 We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. GALACTIC DIFFUSE EMISSION 5 B YUSEF-ZADEH FARHAD NULL NULL USA 3 AO3 A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? XIS Y GCL4 265.3437 -29.192 359.29532739 0.65531706 106.9407 54907.3257986111 54908.0711111111 503102010 33655.4 25000 33679.4 33655.8 0 33655.4 2 2 0 2 1 0 0 30052.1 30052.1 64389.9 0 PROCESSED 54963.2037847222 55329 54920.054837963 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031234 We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. GALACTIC DIFFUSE EMISSION 5 B YUSEF-ZADEH FARHAD NULL NULL USA 3 AO3 A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? XIS Y SLX 1737-282 265.2352 -28.3094 359.99405573 1.20298654 69.9745 54901.4562384259 54901.8035648148 503103010 18316 10000 18332.4 18332 0 18316 2 2 0 2 1 0 0 16365.9 16365.9 30001.9 0 PROCESSED 54963.2700115741 55329 54916.9907638889 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031234 We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. GALACTIC DIFFUSE EMISSION 5 C YUSEF-ZADEH FARHAD NULL NULL USA 3 AO3 A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? XIS Y ARC_BACKGROUND 39.2055 -35.7283 240.48717091 -66.02341726 233.8071 54830.2554861111 54835.3468055556 503104010 201877.5 140000 201957.5 201877.5 0 201981.5 2 2 0 2 1 0 0 5502.8 5502.8 14506 0 PROCESSED 54959.3581481482 55328 54851.4354166667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031235 Aside from the lengthy bright arcs in the northern sky, few X-ray bright, high latitude regions are understood. Yet, studying this gas is important for understanding the Galactic halo. Here, we propose to study a medium-sized (~7 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make Suzaku observations of the arc and nearby background. With them and an existing Suzaku observation, we will be able to determine the thermal properties of the arc plasma and if the arc is the bright limb of a hot bubble. GALACTIC DIFFUSE EMISSION 5 B SHELTON ROBIN NULL NULL USA 3 AO3 A CLOSER LOOT AT HOT HALO GAS: A SUZAKU STUDY OF AN X-RAY BRIGHT ARC XIS Y HESS J1718-385 259.5578 -38.4584 348.92137939 -0.45364037 266.9006 54706.233599537 54706.9286342593 503108010 23509.7 20000 23509.7 23509.7 0 23509.7 2 2 0 2 1 0 0 19440.2 19440.2 60047.9 1 PROCESSED 54720.299849537 55093 54720.4386689815 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 032026 HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum. GALACTIC DIFFUSE EMISSION 5 A PUEHLHOFER GERD NULL NULL EUR 3 AO3 SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385 XIS Y K3/PSR J1420-6048 215.0274 -60.7627 313.55205119 0.26755801 90.771 54842.5598263889 54843.8801388889 503110010 50269 50000 50269 50269 0 50269 1 1 0 1 1 0 0 50061.8 50061.8 114063.9 2 PROCESSED 54959.4244212963 55328 54854.3728703704 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 033076 K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. GALACTIC DIFFUSE EMISSION 5 C KISHISHITA TETSUICHI ROMANI ROGER JUS 3 AO3 SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 HXD Y HESS J1745-303A 265.7791 -30.3241 358.53258375 -0.26269922 103.33 55253.3854166667 55254.6758796296 504001010 51153.8 50000 51161.8 51153.8 0 51168.5 2 2 0 2 1 0 0 42219.6 42219.6 111458.1 1 PROCESSED 55267.237337963 55636 55267.2568634259 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040001 The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. GALACTIC DIFFUSE EMISSION 5 B KOYAMA KATSUJI NULL NULL JAP 4 AO4 DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY XIS Y HESS J1745-303B 266.0577 -30.545 358.47050833 -0.58308172 102.2921 55254.6768634259 55255.9515509259 504002010 53060.9 50000 53060.9 53060.9 0 53060.9 2 2 0 2 1 0 0 46585 46585 110121.9 1 PROCESSED 55267.2540162037 55636 55267.2715856482 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040001 The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. GALACTIC DIFFUSE EMISSION 5 B KOYAMA KATSUJI NULL NULL JAP 4 AO4 DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY XIS Y HESS J1745-303C 266.3881 -30.6242 358.55151469 -0.86700864 101.7444 55252.1897800926 55253.3842476852 504003010 50906.5 50000 50914.5 50914.5 0 50906.5 2 2 0 2 1 0 0 41270.8 41270.8 103187.8 3 PROCESSED 55264.3705671296 55632 55264.3901157407 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040001 The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. GALACTIC DIFFUSE EMISSION 5 B KOYAMA KATSUJI NULL NULL JAP 4 AO4 DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY XIS Y SGR_B2 266.8776 -28.4437 0.63615824 -0.0985299 266.3663 55095.6093518518 55096.0418287037 504004010 10057.2 200000 10057.2 10057.2 0 10057.2 2 2 0 2 1 0 0 9432.8 9432.8 37340.9 0 PROCESSED 55110.1937152778 55476 55110.2035763889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040002 The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. GALACTIC DIFFUSE EMISSION 5 A NOBUKAWA MASAYOSHI NULL NULL JAP 4 AO4 SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- XIS Y SGR_B2 266.8788 -28.4436 0.63679 -0.09938091 266.4718 55096.836412037 55102.6667592593 504004020 202094.5 200000 202094.5 202102.5 0 202094.5 3 4 0 3 1 0 0 178283.1 178283.1 303543.7 4 PROCESSED 55126.8329282407 55500 55133.4505092593 2.4.12.27 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040002 The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. GALACTIC DIFFUSE EMISSION 5 A NOBUKAWA MASAYOSHI NULL NULL JAP 4 AO4 SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- XIS Y RIM1 311.6421 31.883 74.34868893 -7.06658523 247.7276 55152.9451273148 55153.9488888889 504005010 40747.3 38000 40747.3 40747.3 0 40747.3 2 2 0 2 1 0 0 34511.2 34511.2 86715.9 0 PROCESSED 55166.4741087963 55534 55166.4923148148 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y RIM2 311.426 31.5946 74.00572356 -7.09996284 246.8661 55153.9497337963 55154.4843055556 504006010 26305.9 24000 26305.9 26305.9 0 26305.9 1 1 0 1 1 0 0 22237 22237 46183.9 0 PROCESSED 55166.4350231482 55534 55166.4447916667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y RIM3 311.3232 31.2993 73.71675058 -7.21258663 246.4181 55154.4849189815 55155.1204166667 504007010 21556.6 19000 21556.6 21556.6 0 21556.6 2 2 0 2 1 0 0 17481 17481 54903.9 0 PROCESSED 55166.4161342593 55534 55166.4304166667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y RIM4 311.4678 31.0131 73.56601773 -7.48621797 246.0303 55155.1210763889 55155.3579166667 504008010 12102.5 10000 12102.5 12118.5 0 12110.5 1 1 0 1 1 0 0 8666 8666 20455.9 0 PROCESSED 55166.3924189815 55534 55166.425787037 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y RIM5 311.5286 30.6813 73.33464134 -7.73161485 255.8951 55155.3611689815 55155.7953356482 504009010 15850.2 15000 15850.2 15850.2 0 15850.2 2 2 0 2 1 0 0 12289.1 12289.1 37503.9 0 PROCESSED 55166.4004861111 55534 55166.4265277778 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y RIM6 314.3771 31.4503 75.4881661 -9.14820234 247.047 55155.7987615741 55156.1745833333 504010010 14327.5 11000 14347.5 14343.5 0 14327.5 2 2 0 2 1 0 0 10715.2 10715.2 32468 0 PROCESSED 55166.4021180556 55534 55166.4272916667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y BLOWOUT1 312.2225 31.7347 74.53998499 -7.54540267 244.0864 55158.2754166667 55158.9655555556 504011010 24185.4 23000 24201.4 24185.4 0 24193.4 2 2 0 2 1 0 0 19476.8 19476.8 59603.9 1 PROCESSED 55176.1888541667 55545 55176.2112731482 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y BLOWOUT2 311.9515 31.5359 74.23825049 -7.48819964 243.427 55158.9662615741 55159.5106944444 504012010 26549.4 23000 26565.4 26549.4 0 26573.4 1 1 0 1 1 0 0 19940.1 19940.1 47031.9 1 PROCESSED 55176.2151851852 55545 55176.2336921296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y BLOWOUT3 311.7021 31.3134 73.92913651 -7.4588166 242.4356 55160.1363888889 55160.4723611111 504013010 16159.9 16000 16159.9 16159.9 0 16159.9 2 2 0 2 1 0 0 11810.1 11810.1 29021.9 0 PROCESSED 55176.2158680556 55545 55176.2365740741 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y BLOWOUT4 312.7282 31.6832 74.77065214 -7.91349372 242.7253 55160.4733564815 55161.0044444445 504014010 17769.6 15000 17825.7 17769.6 0 17825.6 3 2 0 2 1 0 0 14265.7 14265.7 45876 0 PROCESSED 55176.2561111111 55545 55176.2692939815 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y BLOWOUT5 312.2204 31.3402 74.2273165 -7.78955911 225.5762 55176.0660532407 55176.7307175926 504015010 30406.4 25000 30406.4 30406.4 0 30406.4 2 2 0 2 1 0 0 28692.1 28692.1 57423.9 0 PROCESSED 55189.2573148148 55555 55189.2693981482 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y BLOWOUT6 311.7638 30.9468 73.67127235 -7.72686898 241.7587 55165.8330787037 55166.2883449074 504016010 21000 19000 21008 21016 0 21000 1 1 0 1 1 0 0 17712.9 17712.9 39327.9 0 PROCESSED 55181.2533680556 55547 55181.2630324074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y FESI1 313.4345 30.6099 74.31119672 -9.05841998 226.3696 55182.5546180556 55183.3334837963 504017010 32287.6 24000 32287.6 32287.6 0 32287.6 2 2 0 2 1 0 0 27212.9 27212.9 67285.9 0 PROCESSED 55204.2505092593 55575 55204.4679976852 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y FESI2 313.183 30.3797 73.99193661 -9.03499466 225.2405 55174.9860300926 55175.7904398148 504018010 34590.4 34000 34590.4 34590.4 0 34590.4 2 2 0 2 1 0 0 30318 30318 69493.9 0 PROCESSED 55189.1496180556 55555 55189.1622916667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040007 The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. GALACTIC DIFFUSE EMISSION 5 B TSUNEMI HIROSHI NULL NULL JAP 4 AO4 OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS XIS Y RXJ1713-3946_ID1 257.9616 -39.5166 347.33828294 -0.06271892 87.0007 55242.129375 55243.2502199074 504027010 61533.1 60000 61557.8 61533.1 0 61573.8 3 2 0 2 1 0 0 46725.9 46725.9 96823.8 0 PROCESSED 55253.4576967593 55622 55253.4734259259 2.4.12.27 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040021 We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. GALACTIC DIFFUSE EMISSION 5 B TAKAHASHI TADAYUKI NULL NULL JAP 4 AO4 STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 XIS Y RXJ1713-3946_ID2 258.3083 -40.2394 346.91054647 -0.70324775 87.0013 55243.7284722222 55244.1258564815 504028010 19009.3 20000 19009.3 19017.3 0 19017.3 2 2 0 2 1 0 0 11826.3 11826.3 34331.9 0 PROCESSED 55256.0447337963 55622 55256.0518171296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040021 We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. GALACTIC DIFFUSE EMISSION 5 B TAKAHASHI TADAYUKI NULL NULL JAP 4 AO4 STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 XIS Y RXJ1713-3946_ID3 258.1658 -40.0306 347.01547145 -0.49239611 87.0009 55244.1262847222 55244.4779398148 504029010 20871.6 20000 20903.6 20903.6 0 20871.6 1 1 0 1 1 0 0 20886.8 20886.8 30375.9 0 PROCESSED 55256.0651388889 55622 55256.0720601852 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040021 We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. GALACTIC DIFFUSE EMISSION 5 B TAKAHASHI TADAYUKI NULL NULL JAP 4 AO4 STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 XIS Y RXJ1713-3946_ID4 258.9125 -40.0131 347.36417887 -0.94594655 86.0017 55244.4787384259 55244.8903587963 504030010 22153.4 20000 22177.4 22169.4 0 22153.4 2 2 0 2 1 0 0 19719.3 19719.3 35557.9 1 PROCESSED 55256.0741319444 55622 55256.0824768518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040021 We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. GALACTIC DIFFUSE EMISSION 5 B TAKAHASHI TADAYUKI NULL NULL JAP 4 AO4 STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 XIS Y HESS J1731-347 SW 263.0074 -34.9458 353.3803333 -0.77058494 92.6086 55245.72 55246.5231365741 504031010 41861.5 40000 41877.9 41861.5 0 41869.5 2 2 0 2 1 0 0 34102.8 34102.8 69382 0 PROCESSED 55257.0362037037 55623 55257.0493981482 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040026 Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. GALACTIC DIFFUSE EMISSION 5 B BAMBA AYA NULL NULL JAP 4 AO4 DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 XIS Y HESS J1731-347 N 262.8483 -34.6425 353.56257635 -0.49517094 91.6366 55244.8937037037 55245.7189699074 504032010 41526.3 40000 41526.3 41526.3 0 41526.3 2 2 0 2 1 0 0 32865.3 32865.3 71271.9 0 PROCESSED 55256.998599537 55623 55257.0108449074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040026 Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. GALACTIC DIFFUSE EMISSION 5 B BAMBA AYA NULL NULL JAP 4 AO4 DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 XIS Y HESS J1427-608 216.9609 -60.8505 314.40487303 -0.14444396 90.5578 55209.5761458333 55212.1891666667 504034010 104137.9 100000 104137.9 104137.9 0 104137.9 2 2 0 2 1 0 0 71261.1 71261.1 225737.8 1 PROCESSED 55225.4505439815 55594 55225.4958449074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040066 Pulsar wind nebula (PWN) has began to be recognized as the best candidate of a large fraction of the HESS-unidentified (unID) sources. It could be true for some sources like HESS J1825-137, while other PWN candidates are sometimes listed simply because they satisfy one or two of the necessary conditions (e.g., there is an energetic pulsar nearby). We then propose a Suzaku observation of HESS J1427-608, which is the most ``unlike'' HESS-unID source to be a PWN. The advantage that we can safely exclude a PWN for its candidate allows us to identify the emission mechanism/origin of HESS J1427-608 more unambiguously compared to other unID sources. We request a 150 ks exposure to constrain the ratio between X-ray and TeV fluxes, which is a good measure of the emission mechanism of TeV sources. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 4 AO4 A SUZAKU OBSERVATION OF HESS J1427-608 XIS Y W49B 287.7847 9.1153 43.2812159 -0.18378496 89.2674 54921.5302662037 54923.0613425926 504035010 61782.5 100000 61790.5 61784.5 0 61782.5 3 3 0 3 1 0 0 55155.6 55155.6 132273.9 3 PROCESSED 54949.0816203704 55324 54949.4493287037 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040075 Observation of the W49B supernova remnant for 100 ksec is proposed to detect Ti emission line at the 3 sigma confidence level. In order to reveal whether it is a remnant of Type Ia supernova or not, detailed measurement of the rare metal elements such as Cr, Mn, Ni, and Ti is essential. We determine the type by Ti to Cr, Mn to Cr, and Ni to Fe ratios. Furthermore, we investigate whether its plasma is in the overionized status or not. GALACTIC DIFFUSE EMISSION 5 B OZAWA MIDORI NULL NULL JAP 4 AO4 UNMASK THE NATURE OF W49B ! XIS Y TORNADO 265.1272 -30.949 357.70572925 -0.11631727 269.1137 55072.5037037037 55075.0093055556 504036010 125069.2 120000 125069.2 125077.2 0 125077.2 2 2 0 2 1 0 0 97091.3 97091.3 216459.8 3 PROCESSED 55088.2749884259 55454 55088.3064814815 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040076 The Tornado is an unusual and intense radio source located in the galactic center region. It has a polarized non-thermal radio spectrum. t has very unique morphology of elongated and loop-like structure. However, no crucial observational result determining the nature has been obtained. With the Suzaku AO3 observation of the Tornado (50ks), we found interesting signs of 2.45-keV He like S-K line, diffuse emission from the "tail" and the whole "head". The purpose of this observation is to obtain precise spectrum and spatial distribution. If the thermal S-K line is confirmed and it has a high metal abundance, the nature of the Tornado is an SNR. We also investigate the extreme structure of the tail and search for power-law component in spectra. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 4 AO4 REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION XIS Y GALACTICDISC3-1 15.309 67.9759 123.85392042 5.12169353 244.2747 55214.8348148148 55216.0225 504038010 55227.9 50000 55227.9 55227.9 0 55227.9 2 2 0 2 1 0 0 43332.9 43332.9 102599.8 2 PROCESSED 55228.1780324074 55594 55228.2005092593 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040097 To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. GALACTIC DIFFUSE EMISSION 5 C KIMURA SHUNSUKE NULL NULL JAP 4 AO4 STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE XIS Y GALACTICDISC3-2 16.1096 72.7817 123.90816526 9.93459858 241.5401 55216.0250115741 55217.5772685185 504039010 73528.2 70000 73528.2 73528.2 0 73528.2 2 2 0 2 1 0 0 54648 54648 134105.8 1 PROCESSED 55236.0900694444 55602 55236.1178240741 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040097 To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. GALACTIC DIFFUSE EMISSION 5 C KIMURA SHUNSUKE NULL NULL JAP 4 AO4 STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE XIS Y ASO0382 265.491 -20.8915 6.43327069 4.9108593 101.5727 55276.7369328704 55277.3869675926 504040010 21222.3 20000 21222.3 21222.3 0 21222.3 2 2 0 2 1 0 0 3974 3974 56108.9 2 PROCESSED 55298.6755902778 55665 55299.411875 2.5.16.28 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0078 59.472 32.09 162.76236061 -16.0043339 83.0007 55045.8202777778 55046.3273032407 504041010 21312 20000 21320 21320 0 21312 1 1 0 1 1 0 0 21295.9 21295.9 43799.9 0 PROCESSED 55064.031099537 55430 55064.0383912037 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0402 273.3436 -12.7608 17.24676471 2.45193699 68.9842 55277.3929513889 55277.9793287037 504042010 25712.5 20000 25712.5 25712.5 0 25712.5 1 1 0 1 1 0 0 16015.2 16015.2 50655.9 1 PROCESSED 55417.0765740741 55784 55417.0893865741 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0431 286.9632 6.0295 40.16756672 -0.88470452 90.0004 54936.153287037 54936.8141666667 504043010 24522.2 20000 24522.2 24522.2 0 24522.2 2 2 0 2 1 0 0 18105 18105 57073.9 0 PROCESSED 54949.3871296296 55324 54949.5652777778 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0449 299.6429 28.7759 65.87759933 -0.32938525 56.1427 54974.6386921296 54975.5786342593 504044010 38733.7 20000 38733.7 38741.7 0 38741.7 1 1 0 1 1 0 0 35220 35220 81199.9 2 PROCESSED 54987.0954861111 55356 54987.4424652778 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0218 157.1332 -58.313 285.06973918 -0.48663651 315.2825 55020.3423148148 55020.9467476852 504045010 22844.9 20000 22844.9 22844.9 0 22844.9 2 2 0 2 1 0 0 21154.4 21154.4 52217.9 1 PROCESSED 55034.2615740741 55400 55034.2716898148 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0447 298.557 28.6365 65.2636943 0.41202338 90.516 54928.7514699074 54929.253587963 504046010 20545.7 20000 20545.7 20545.7 0 20545.7 2 2 0 2 1 0 0 16907.1 16907.1 43377.9 1 PROCESSED 54949.0673032407 55324 54949.4485300926 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0147 98.4346 6.5402 205.09585789 -0.932863 292.0552 54931.9181481482 54932.5036921296 504047010 24041.3 20000 24041.3 24041.3 0 24041.3 2 2 0 2 1 0 0 23240.9 23240.9 50562 1 PROCESSED 54949.2968402778 55324 54949.5271180556 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0505 339.5988 59.0734 106.55945745 0.49758229 62.7751 55001.185775463 55001.7494675926 504048010 26361.6 20000 26369.6 26361.6 0 26377.6 2 2 0 2 1 0 0 23841.6 23841.6 48695.9 1 PROCESSED 55015.2421296296 55381 55015.2523148148 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y ASO0376 263.1417 -31.5448 356.29011362 0.99386623 267.5095 55082.1506365741 55083.1084606482 504049010 37227.8 20000 38987.8 39259.8 0 37227.8 5 4 0 4 1 0 0 31813.4 31813.4 82729.9 1 PROCESSED 55113.2099537037 55479 55113.2260069444 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040101 Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS XIS Y (L,B)=(0.107,-1.425) 267.8602 -29.5833 0.10035042 -1.42140103 68.0986 55261.1636226852 55263.893275463 504050010 100399.1 100000 100431.1 100399.1 0 100423.1 2 2 0 2 1 0 0 80536 80536 235821.8 1 PROCESSED 55278.4197453704 55645 55278.4832523148 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040109 In order to resolve origin of the Galactic bulge/ridge emission, we propose to observe the blank field 1.5 deg from the Galactic center where Chandra recently performed the deepest exposure (900 ksec) aiming to resolve the Galactic "diffuse" emission into point sources. Goals of the present observation are the following: (1) Resolve the three iron emission lines (6.41 keV, 6.67 keV and 6.97 keV) with Suzaku, and compare with the point source population determined by Chandra to clarify what kinds of sources are responsible for which emission line. (2) Study Galactic latitudinal variation of the three emission lines comparing with the existent Suzaku observation at (l,b)=(0.0, -2.0). (3) Constrain the hard-tail emission above 10 keV, and study its Galactic latitudinal variation. GALACTIC DIFFUSE EMISSION 5 B EBISAWA KEN NULL NULL JAP 4 AO4 RESOLVING ORIGIN OF THE IRON EMISSION LINES FROM THE GALACTIC BULGE XIS Y ASO0418 279.775 -5.7085 26.44714681 0.13153934 86.843 54934.6472800926 54935.7578587963 504052010 41068.4 40000 41080.2 41084.4 0 41068.4 2 2 0 2 1 0 0 33525.8 33525.8 95937.8 0 PROCESSED 54949.4674884259 55324 54949.5662268518 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040112 We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE XIS Y ASO0215 154.6836 -58.9426 284.32918046 -1.70077172 314.5017 55019.3141782407 55020.3404976852 504053010 40086.8 40000 40086.8 40086.8 0 40086.8 2 2 0 2 1 0 0 35478.2 35478.2 88659.8 0 PROCESSED 55029.2327199074 55399 55029.2468055556 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040112 We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE XIS Y ASO0304 213.3355 -62.0808 312.3597658 -0.71761471 280.2937 55036.9044907407 55038.1453935185 504054010 44248.5 40000 44248.5 44248.5 0 44248.5 2 2 0 2 1 0 0 41083.9 41083.9 107201.8 1 PROCESSED 55048.3005208333 55415 55048.3203819444 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040112 We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE XIS Y ASO0319 224.8822 -60.8823 317.89227503 -1.78687667 277.7774 55049.7078125 55051.0238425926 504055010 42361.3 40000 42361.3 42366.8 0 42377.3 2 2 0 2 1 0 0 37523.3 37523.3 113685.9 0 PROCESSED 55062.2726967593 55430 55062.2941782407 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040112 We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. GALACTIC DIFFUSE EMISSION 5 A KAWAI NOBUYUKI NULL NULL JAP 4 AO4 UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE XIS Y HESSJ1616_PSRJ1617 244.3756 -50.9175 332.50297445 -0.27465368 270.0711 55059.1110763889 55060.8328009259 504056010 65833.1 50000 65889.1 65833.1 0 65897.1 2 2 0 2 1 0 0 41750.4 41750.4 148725.8 0 PROCESSED 55071.2290625 55437 55071.2513425926 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040115 HESSJ1616-508 is one of the most energetic unidentified TeV object. Previously, we showed that there is no clear X-ray counterpart to this object with a Suzaku observation, and hence we argued that the object is a real dark particle accelerator. However, there is a young energetic pulsar PSRJ1617-5055 10 arcmin away from HESSJ1616, and another possibility has been proposed that HESSJ1616 is an offset pulsar wind nebula (PWN) driven by the pulsar. If this possibility is correct, a powerful X-ray PWN should be observed as HESSJ1825-137, but such PWN has not been reported. The lack of the detection may be due to small sensitivity of Chandra and XMM-Newton for a diffuse hard X-ray emission. We propose to observe PSRJ1617 to see if there is an extended PWN around this pulsar. GALACTIC DIFFUSE EMISSION 5 A MATSUMOTO HIRONORI NULL NULL JAP 4 AO4 IS THE MOST ENERGETIC UNIDENTIFIED TEV OBJECT HESSJ1616-508 A PULSAR WIND NEBULA? XIS Y VICINITY OF NGC 4051 180.4686 44.1146 150.13143213 70.30340869 109.3717 55184.3459606482 55186.5140509259 504062010 89630.5 80000 89638.5 89646.5 0 89630.5 3 2 0 2 1 0 0 37075.8 37075.8 187281.9 2 PROCESSED 55209.2126273148 55581 55209.4570833333 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040120 The highly ionized absorption lines of OVII and OVII at z = 0 have been unambiguously detected toward the bright AGN NGC 4051 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII and OVIII emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. GALACTIC DIFFUSE EMISSION 5 C HAGIHARA TOSHISHIGE NULL NULL JAP 4 AO4 STUDY OF WARM-HOT GAS TOWARD NGC 4051 XIS Y VELA SOUTHWEST 1 126.2671 -48.2152 264.99036518 -5.99332729 119.5649 55164.9700925926 55165.818900463 504063010 32733.1 30000 32749.2 32733.1 0 32741.1 3 2 0 2 1 0 0 23767.4 23767.4 73309.9 0 PROCESSED 55179.2546990741 55546 55179.268587963 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040121 We propose 2 pointing-observations of south western part of Vela supernova remnant. Vela SNR has the largest angular size of 8 degree in diameter, so it is suitable to carry out spatial resolved spectroscopy with Suzaku. GALACTIC DIFFUSE EMISSION 5 C HIRAGA JUNKO NULL NULL JAP 4 AO4 X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA XIS Y W51NW 290.6858 14.2133 49.11550833 -0.31636783 105.4558 55283.4893634259 55284.555 504066010 44112.5 40000 44120.5 44120.5 0 44112.5 1 1 0 1 1 0 0 8896.1 8896.1 92063.9 0 PROCESSED 55302.488912037 55671 55302.5003240741 2.5.16.28 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 040129 We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. GALACTIC DIFFUSE EMISSION 5 C KATAGIRI HIDEAKI NULL NULL JAP 4 AO4 ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C XIS Y W51SW 290.8908 14.1062 49.1149541 -0.54215584 104.3698 55285.3081944444 55286.3752314815 504067010 43728.7 40000 43728.7 43728.7 0 43728.7 2 2 0 2 1 0 0 9813.7 9813.7 92179.9 0 PROCESSED 55302.2257175926 55671 55302.2468055556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 040129 We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. GALACTIC DIFFUSE EMISSION 5 C KATAGIRI HIDEAKI NULL NULL JAP 4 AO4 ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C XIS Y SEP #1 89.966 -66.5774 276.40322057 -29.82494721 141.7136 55149.1175925926 55150.2141087963 504069010 51862.1 50000 51870.1 51862.1 0 51870.1 2 2 0 2 1 0 0 48353.4 48353.4 94725.9 2 PROCESSED 55160.1364236111 54922 55160.1496296296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y NEP #1 270.0492 66.5597 96.38280784 29.79186901 217.1802 55150.229212963 55151.1953587963 504070010 56336.7 50000 56336.7 56344.7 0 56344.7 1 1 0 1 1 0 0 41434.5 41434.5 83471.9 2 PROCESSED 55162.1951851852 54922 55162.2062268518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y SEP #2 89.966 -66.5714 276.39630454 -29.82495373 163.7813 55170.9454166667 55172.4863194444 504071010 57999.1 50000 58007.1 57999.1 0 58007.1 2 2 0 2 1 0 0 35415.2 35415.2 133112 1 PROCESSED 55187.4636226852 54922 55187.4854398148 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y NEP #2 270.0521 66.5655 96.38949161 29.79071779 194.6438 55172.5015162037 55173.6411342593 504072010 48697.7 50000 48697.7 48697.7 0 48697.7 2 2 0 2 1 0 0 38458.2 38458.2 98456 1 PROCESSED 55190.0016203704 54922 55190.01875 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y SEP #3 89.9578 -66.5683 276.39273536 -29.82821774 172.4885 55179.5059259259 55180.9169444444 504073010 44408 50000 44408 44416 0 44416 2 2 0 2 1 0 0 23878.4 23878.4 121901.8 1 PROCESSED 55200.2330555556 54922 55200.462337963 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y NEP #3 270.0483 66.5696 96.39421541 29.79223028 188.0738 55180.9320949074 55182.0557638889 504074010 50176.9 50000 50176.9 50176.9 0 50176.9 2 2 0 2 1 0 0 33337.4 33337.4 97049.9 1 PROCESSED 55200.3194212963 54922 55200.4707291667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y SEP #4 89.9798 -66.5683 276.39272547 -29.81946932 185.1981 55192.0059490741 55193.3995833333 504075010 49956.6 50000 49956.6 49956.6 0 49956.6 2 2 0 2 1 0 0 45143 45143 120393.9 1 PROCESSED 55225.2945717593 54922 55225.3094907407 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y NEP #4 270.0449 66.5788 96.40481628 29.79358389 165.3654 55193.4146875 55194.4579166667 504076010 49849.1 50000 49857.1 49857.1 0 49849.1 2 2 0 2 1 0 0 43503.9 43503.9 90114 0 PROCESSED 55246.2796990741 54922 55246.2930787037 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041101 We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. GALACTIC DIFFUSE EMISSION 5 A SNOWDEN STEVEN NULL NULL USA 4 AO4 OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE XIS Y HESS J1809-193A 273.0012 -19.0034 11.60922783 -0.25253702 270.0939 55083.2051967593 55084.4828009259 504077010 52110.9 50000 52174.5 52190.8 0 52110.9 3 3 0 3 1 0 0 44109 44109 110376 1 PROCESSED 55109.2056481482 55475 55109.4207638889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041303 We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. GALACTIC DIFFUSE EMISSION 5 A KARGALTSEV OLEG NULL NULL USA 4 AO4 CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION XIS Y HESS J1809-193B 272.6789 -19.1585 11.32661741 -0.06027609 269.0544 55084.4838773148 55085.7488310185 504078010 52474.8 50000 52474.8 52474.8 0 52474.8 2 2 0 2 1 0 0 43373.3 43373.3 109275.8 1 PROCESSED 55109.2733449074 55475 55109.4280555556 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041303 We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. GALACTIC DIFFUSE EMISSION 5 A KARGALTSEV OLEG NULL NULL USA 4 AO4 CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION XIS Y HESS J1809-193E 272.0013 -19.5033 10.71539243 0.332309 270.1011 55085.7498148148 55087.1564351852 504079010 51028.9 50000 51028.9 51028.9 0 51028.9 2 2 0 2 1 0 0 41875.3 41875.3 121519.8 2 PROCESSED 55098.3156944444 55465 55098.3372337963 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041303 We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. GALACTIC DIFFUSE EMISSION 5 A KARGALTSEV OLEG NULL NULL USA 4 AO4 CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION XIS Y G156.2+5.7 (S) 74.9073 51.0204 156.85145441 5.28162006 265.6871 55259.9832407407 55261.1495833333 504080010 52641.3 50000 52649.3 52641.3 0 52649.3 2 2 0 2 1 0 0 47656.6 47656.6 100757.8 0 PROCESSED 55323.2686342593 55689 55323.2891666667 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 041311 The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 4 AO4 REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 XIS Y G156.2+5.7 (NW2) 74.4322 52.0607 155.84514532 5.68920631 266.0115 55258.7553587963 55259.9821643518 504081010 52864.6 50000 52867.8 52867.8 0 52864.6 2 2 0 2 1 0 0 49386.6 49386.6 105991 1 PROCESSED 55322.2954282407 55689 55322.3173842593 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 041311 The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 4 AO4 REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 XIS Y G156.2+5.7 (E2) 75.2673 51.6789 156.46612231 5.86221802 271.6298 55248.7736574074 55250.0369675926 504082010 50330.8 50000 50346.8 50330.8 0 50346.8 3 2 0 2 1 0 0 46142.4 46142.4 109137.9 0 PROCESSED 55266.2809375 55632 55266.2981597222 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041311 The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 4 AO4 REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 XIS Y 330.2+1.0 240.2338 -51.588 330.14009051 0.98414205 285.0002 55078.1480671296 55080.8126736111 504083010 127774.6 150000 127782.6 127774.6 0 127774.6 2 2 0 2 1 0 0 112848.4 112848.4 230157.8 1 PROCESSED 55089.302025463 55455 55089.3295949074 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041312 Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. GALACTIC DIFFUSE EMISSION 5 B ALLEN GLENN NULL NULL USA 4 AO4 MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 XIS Y 330.2+1.0 240.2338 -51.5878 330.14022152 0.98429318 285.0004 55081.4851273148 55082.1453472222 504083020 30889.6 30000 30889.6 30889.6 0 30897.1 2 2 0 2 1 0 0 27076.4 27076.4 57037.9 0 PROCESSED 55092.1525810185 55458 55092.1620949074 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041312 Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. GALACTIC DIFFUSE EMISSION 5 B ALLEN GLENN NULL NULL USA 4 AO4 MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 XIS Y 330.2+1.0 240.2384 -51.525 330.18352169 1.02987491 98.9027 55239.832025463 55242.125150463 504083030 92505 30000 92513 92505 0 92521 2 2 0 2 1 0 0 86096.5 86096.5 198089.7 4 PROCESSED 55253.5099421296 55622 55253.5397685185 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041312 Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. GALACTIC DIFFUSE EMISSION 5 B ALLEN GLENN NULL NULL USA 4 AO4 MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 XIS Y NGC 6888 303.111 38.3992 75.54872423 2.39562358 36.3096 54999.0718981482 55001.1793287037 504084010 88846.8 75000 88854.8 88846.8 0 88854.8 2 2 0 2 1 0 0 82405.2 82405.2 182067.9 2 PROCESSED 55012.3928009259 55378 55012.4221180556 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041321 Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. GALACTIC DIFFUSE EMISSION 5 A ZHEKOV SVETOZAR NULL NULL USA 4 AO4 X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 XIS Y NGC 6888 302.9954 38.2382 75.36419968 2.38310331 253.873 55139.4126388889 55141.3127777778 504085010 77349 75000 77461 77349 0 77461 3 2 0 2 1 0 0 62100.2 62100.2 164155.8 0 PROCESSED 55152.1150231482 55518 55152.1455671296 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041321 Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. GALACTIC DIFFUSE EMISSION 5 A ZHEKOV SVETOZAR NULL NULL USA 4 AO4 X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 XIS Y MRK 421 OFFSET 166.8026 37.7335 180.50489089 65.69633084 129.0398 55144.0655092593 55145.8091087963 504086010 75259.5 75000 75267.5 75259.5 0 75267.5 2 2 0 2 1 0 0 51940 51940 150628.8 2 PROCESSED 55176.195474537 55542 55176.2291319444 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041324 The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. GALACTIC DIFFUSE EMISSION 5 B YAO YANGSEN NULL NULL USA 4 AO4 A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 XIS Y MRK 421 OFFSET 165.3836 38.6302 179.31913311 64.35556561 121.9647 55146.4480092593 55148.3176388889 504087010 86014.4 75000 86014.4 86014.4 0 86014.4 2 2 0 2 1 0 0 64880.4 64880.4 161519.9 3 PROCESSED 55160.2386226852 55531 55160.2701041667 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041324 The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. GALACTIC DIFFUSE EMISSION 5 B YAO YANGSEN NULL NULL USA 4 AO4 A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 XIS Y GALACTIC_BULGE1 267.2201 -29.3677 359.99969448 -0.83243485 274.7 55118.4798148148 55119.6453587963 504088010 47230 50000 47230 47230 0 47230 2 2 0 2 1 0 0 32613.9 32613.9 100700 2 PROCESSED 55134.0521527778 54922 55134.0688425926 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE2 267.5552 -29.599 359.95115697 -1.20153587 277.9812 55113.1708217593 55114.5903472222 504089010 55260.1 50000 55267.1 55260.1 0 55273.6 2 2 0 2 1 0 0 40226 40226 122633.8 1 PROCESSED 55131.3114699074 54922 55131.3309953704 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE7 266.6764 -30.8281 358.50617228 -1.18471698 274.4326 55117.1787037037 55118.4785416667 504090010 41260.7 50000 41260.7 52903.3 0 52903.3 3 2 0 2 1 0 0 34964 34964 112293.8 2 PROCESSED 55133.2241898148 54922 55133.2421643518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE8 267.0897 -31.0498 358.49976827 -1.60277837 260.4349 55088.8177777778 55090.3043287037 504091010 51331.6 50000 51331.6 51339.2 0 51331.6 2 2 0 2 1 0 0 47751.4 47751.4 128425.8 2 PROCESSED 55109.2394444445 54922 55109.4226736111 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE9 267.6768 -31.2805 358.55970985 -2.15232996 265.3076 55090.3066550926 55091.5758564815 504092010 50919.9 50000 50943.9 50935.9 0 50919.9 2 2 0 2 1 0 0 45574.4 45574.4 109645.9 1 PROCESSED 55109.2958796296 54922 55109.4315740741 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE10 268.297 -31.6627 358.49964198 -2.80216044 277.1297 55091.579525463 55093.1508564815 504093010 53241.6 50000 53249.5 53241.6 0 53257.5 2 2 0 2 1 0 0 46907.2 46907.2 135734 1 PROCESSED 55110.2981481482 54922 55110.3193865741 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE11 269.3164 -32.1646 358.50010375 -3.80248777 271.7893 55093.1531365741 55095.6064699074 504094010 93140.3 50000 93140.3 93140.3 0 93140.3 2 2 0 2 1 0 0 82954.3 82954.3 211953.8 1 PROCESSED 55110.3795486111 54922 55110.4114236111 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE12 270.5539 -32.7559 358.50046577 -5.00243267 271.4834 55119.6475462963 55120.7502199074 504095010 48262.2 50000 48262.2 48262.2 0 48262.2 3 2 0 2 1 0 0 38358 38358 95261.9 1 PROCESSED 55133.2591435185 54922 55133.2742824074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y G346.6-0.2 257.5822 -40.1827 346.62898747 -0.22219097 278.7363 55111.704525463 55113.1668287037 504096010 56754.3 50000 56754.3 56762.3 0 56770.3 2 2 0 2 1 0 0 42412.1 42412.1 126323.9 0 PROCESSED 55127.3600810185 54922 55127.3766898148 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y G348.5+0.1 258.6301 -38.5295 348.44223752 0.09652262 91.401 55247.6321180556 55248.7592476852 504097010 53810.6 50000 53810.6 53810.6 0 53810.6 2 2 0 2 1 0 0 46392.9 46392.9 97359.8 1 PROCESSED 55257.0207291667 54922 55257.0343287037 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y G355.6-0.0 263.7798 -32.6083 355.69106204 -0.03789327 90.0013 55246.5249074074 55247.6293287037 504098010 52504.4 50000 52527.5 52520.4 0 52504.4 2 2 0 2 1 0 0 43734.6 43734.6 95411.8 0 PROCESSED 55257.097650463 54922 55257.1119444444 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y G25.5+0.0 279.4506 -6.6057 25.50196825 0.00652115 74.2354 54927.1234490741 54928.7446064815 504099010 52737.5 50000 52737.5 52737.5 0 52737.5 2 2 0 2 1 0 0 44570.3 44570.3 140042 3 PROCESSED 54949.1324884259 54922 54949.4845023148 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y KEPLER_BG_GE 263.5353 -20.2634 5.99742641 6.79731937 272.7609 55087.1593171296 55088.3606365741 504101010 46989.5 60000 46989.5 46989.5 0 46989.5 2 2 0 2 1 0 0 40899.3 40899.3 103786 0 PROCESSED 55099.2398263889 54922 55099.2516782407 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y KEPLER_BG_GE 263.5357 -20.2632 5.99779838 6.79710869 273.0028 55072.0030208333 55072.5002662037 504101020 24722.7 60000 24746.7 24738.7 0 24722.7 2 2 0 2 1 0 0 19252.8 19252.8 42955.9 0 PROCESSED 55106.2377777778 54922 55109.4155324074 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y KEPLER_BG_GW 261.806 -22.7684 2.99933771 6.7960859 273.0885 55109.2984143518 55111.1057175926 504102010 65294.9 60000 65302.9 65294.9 0 65302.9 2 2 0 2 1 0 0 50782.1 50782.1 156128 1 PROCESSED 55125.6732407407 54922 55125.6963888889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y KEPLER_BG_GN 261.9141 -20.2308 5.199252 8.09662946 270.3619 55105.4689699074 55107.4279976852 504103010 68604.3 60000 68604.3 68604.3 0 68612.3 2 2 0 2 1 0 0 55801.4 55801.4 169227.9 1 PROCESSED 55125.6058217593 54922 55125.6331828704 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y KEPLER_BG_GS 263.1005 -22.949 3.49961978 5.69692486 272.6396 55107.43 55109.2973842593 504104010 67250.8 60000 67250.8 67280.5 0 67274.8 2 2 0 2 1 0 0 53158.5 53158.5 161329.8 1 PROCESSED 55125.3330555556 54922 55125.3521180556 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y IC443 NORTHWEST 93.9975 22.7552 188.75644855 2.86235674 91.4819 55456.3191435185 55458.2829050926 505001010 83191.7 80000 83191.7 83191.7 0 83191.7 2 2 0 2 1 0 0 69678.6 69678.6 169645.7 2 PROCESSED 55469.3764930556 55836 55469.4041087963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050001 Suzaku discovered the radiative recombination continua (RRC) of Si and S from the supernova remnant IC443. This new phenomenon (the RRC) would be due to either pre-ionization by X-ray flash of gamma-ray burst, or adiabatic cooling in a rarefied ambient medium, or yet-unknown process. In any case, the RRC have essential and new clues for the mechanisms, evolution and/or even the cosmic-ray acceleration of IC443. Spectra of the rim regions provide key information for the RRC origin. We thus propose the East and West periphery of IC443 for total 200 ksec. GALACTIC DIFFUSE EMISSION 5 C OZAWA MIDORI NULL NULL JAP 5 AO5 EXPLORING THE ORIGIN OF THE RADIATIVE RECOMBINATION CONTINUUM OF IC443 XIS Y W44 284.0351 1.3886 34.70383121 -0.41279271 90.6817 55296.8229513889 55298.1591898148 505004010 61143.3 60000 61151.3 61143.3 0 61151.3 2 2 0 2 1 0 0 53712.9 53712.9 115399.9 2 PROCESSED 55313.2711921296 55287 55313.4281597222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050002 We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM XIS Y W28_CENTER 270.074 -23.3664 6.46943001 -0.00256773 84.9544 55289.3078935185 55290.9918287037 505005010 73003.6 70000 73043.7 73003.6 0 73043.6 3 2 0 2 1 0 0 57298.1 57298.1 145451.9 2 PROCESSED 55322.3483449074 55287 55322.3694675926 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050002 We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM XIS Y W28_EASTSHELL 270.3727 -23.2858 6.67541903 -0.20080463 88.0003 55617.4542939815 55620.1723032407 505006010 99981.6 100000 99981.6 99981.6 0 99981.6 2 2 0 2 1 0 0 83677.2 83677.2 234815.7 3 PROCESSED 55642.1690046296 55287 55642.1946643518 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050002 We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM XIS Y 3C_391 282.3812 -0.9417 31.87573789 -0.00377867 261.9952 55491.0759722222 55493.8224537037 505007010 99388.7 100000 99460.7 99388.7 0 99468.7 2 2 0 2 1 0 0 89374 89374 237277.9 2 PROCESSED 55502.2992361111 55287 55502.3356597222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050002 We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM XIS Y 3C_397 286.9038 7.1223 41.11064468 -0.32936267 256.5108 55493.8258449074 55495.8022337963 505008010 69326.6 70000 69326.6 69326.6 0 69326.6 2 2 0 2 1 0 0 62165.3 62165.3 170731.9 0 PROCESSED 55505.3133796296 55287 55505.3393981482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050002 We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM XIS Y CYGNUS LOOP 1 313.2462 32.1399 75.40840203 -7.96786776 81.7816 55300.7096759259 55301.0293402778 505009010 15999.2 13000 15999.2 15999.2 0 15999.2 2 2 0 2 1 0 0 12242 12242 27612 0 PROCESSED 55362.3015740741 55287 55362.3098726852 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 2 312.7259 32.1633 75.14683323 -7.61088939 81.0273 55301.0300925926 55301.2897569444 505010010 12932 10000 12932 12932 0 12932 1 1 0 1 1 0 0 11924 11924 22431.9 0 PROCESSED 55362.2883564815 55287 55362.2959375 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 3 312.9529 31.9301 75.08571271 -7.90709143 81.0389 55301.2902777778 55301.6209953704 505011010 13444.8 12000 13444.8 13444.8 0 13444.8 2 2 0 2 1 0 0 10427 10427 28571.9 0 PROCESSED 55362.3486921296 55287 55362.3557060185 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 4 312.482 31.9468 74.84594636 -7.58533627 81.0154 55301.6216087963 55301.8912037037 505012010 12453.5 12000 12453.5 12453.5 0 12453.5 2 2 0 2 1 0 0 12182 12182 23280.1 1 PROCESSED 55362.3083796296 55287 55362.3160763889 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 5 312.0188 31.9594 74.60885135 -7.27014396 81.8368 55305.8645833333 55306.4578125 505013010 26845.2 26000 26845.2 26845.2 0 26845.2 1 1 0 1 1 0 0 21277 21277 51232 2 PROCESSED 55364.1937384259 55287 55364.2036458333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 6 314.1656 31.2305 75.19999907 -9.14964477 81.8988 55301.8924189815 55302.1398148148 505014010 12462.3 10000 12478.3 12462.3 0 12478.3 1 1 0 1 1 0 0 12068.3 12068.3 21359.9 0 PROCESSED 55362.3348958333 55287 55362.3410532407 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 7 313.929 31.0152 74.90122685 -9.13052292 81.814 55306.459212963 55306.7974189815 505015010 13591.8 12000 13591.8 13599.8 0 13599.8 2 2 0 2 1 0 0 12682 12682 29195.9 0 PROCESSED 55393.2089236111 55287 55393.2216203704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 8 313.6776 30.8178 74.60811536 -9.08900254 81.5524 55306.7979398148 55307.2786689815 505016010 23553.4 21000 23561.4 23553.4 0 23569.4 1 1 0 1 1 0 0 20198.9 20198.9 41527.9 0 PROCESSED 55364.2321180556 55287 55364.2401967593 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 9 312.876 30.2229 73.70000859 -8.9268412 80.5836 55307.2796064815 55308.0106597222 505017010 29996.8 29000 29996.8 29996.8 0 29996.8 2 2 0 2 1 0 0 27628.1 27628.1 63149.9 1 PROCESSED 55364.2562962963 55287 55364.2675347222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 10 314.1171 30.7461 74.79486269 -9.42625359 82.0017 55328.2812152778 55328.6981134259 505018010 16268 16000 16276 16276 0 16268 2 2 0 2 1 0 0 12655.1 12655.1 36012 0 PROCESSED 55393.3211805556 55287 55393.3335069445 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 11 313.8693 30.5587 74.51088669 -9.3807208 82.002 55328.698587963 55329.1251736111 505019010 18897.6 18000 18905.6 18897.6 0 18913.6 2 2 0 2 1 0 0 14904.8 14904.8 36853.9 1 PROCESSED 55393.347025463 55287 55393.3619791667 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 12 313.6077 30.3526 74.20451075 -9.33661335 82.0022 55329.1256944444 55329.8391666667 505020010 27842.7 28000 27850.7 27850.7 0 27842.7 2 2 0 2 1 0 0 21052.2 21052.2 61640 0 PROCESSED 55393.4029166667 55287 55393.4203009259 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 13 313.3172 30.1574 73.89066537 -9.26489611 82.0018 55329.8397337963 55330.4925694444 505021010 21565 21000 21565 21597 0 21565 2 2 0 2 1 0 0 18120 18120 56399.9 1 PROCESSED 55393.3470601852 55287 55393.3656712963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 14 313.0411 29.9656 73.58742167 -9.19932348 67.2195 55334.4727893518 55335.1146759259 505022010 29251.2 29000 29251.2 29251.2 0 29251.2 2 2 0 2 1 0 0 24783.2 24783.2 55451.9 0 PROCESSED 55348.0383333333 55287 55348.0488888889 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 15 313.2124 29.6854 73.46064198 -9.49078141 50.2914 55343.3019791667 55343.6994675926 505023010 19295.3 19000 19295.3 19295.3 0 19295.3 1 1 0 1 1 0 0 16514 16514 34320 1 PROCESSED 55355.1471527778 55287 55355.1545833333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y CYGNUS LOOP 16 312.8966 29.5255 73.15999246 -9.37678246 49.3574 55343.7003125 55344.4932407407 505024010 34833.8 34000 34833.8 34833.8 0 34833.8 2 2 0 2 1 0 0 32418.2 32418.2 68507.9 1 PROCESSED 55355.187337963 55287 55355.2000115741 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050005 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS XIS Y G22.0+0.0 277.823 -9.7151 22.00005623 0.00370699 89.3658 55302.6023842593 55303.7272222222 505025010 50529.4 50000 50529.4 50529.4 0 50529.4 2 2 0 2 1 0 0 44620.8 44620.8 97159.8 0 PROCESSED 55371.024837963 55737 55375.7533101852 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050009 ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. GALACTIC DIFFUSE EMISSION 5 B YAMAUCHI SHIGEO NULL NULL JAP 5 AO5 SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA XIS Y G23.5+0.1 278.489 -8.375 23.49243074 0.03918587 261.7121 55489.5657291667 55491.0730439815 505026010 48976.1 50000 48976.1 48976.1 0 48976.1 2 2 0 2 1 0 0 43788.4 43788.4 130191.9 0 PROCESSED 55502.1584490741 55868 55502.1887962963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050009 ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. GALACTIC DIFFUSE EMISSION 5 B YAMAUCHI SHIGEO NULL NULL JAP 5 AO5 SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA XIS Y G37.0-0.1 284.8009 3.5813 37.00394757 -0.09218404 68.6266 55303.7327893518 55304.8814583333 505027010 50969.4 50000 50977.4 50977.4 0 50969.4 2 2 0 2 1 0 0 45336.1 45336.1 99230 1 PROCESSED 55326.2775462963 55693 55326.2903125 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050009 ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. GALACTIC DIFFUSE EMISSION 5 B YAMAUCHI SHIGEO NULL NULL JAP 5 AO5 SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA XIS Y FVW319.8+0.3 225.913 -58.2332 319.61922846 0.28881447 278.3756 55413.1563888889 55413.9307291667 505029010 51384 50000 51400 51384 0 51400 2 2 0 2 1 0 0 45416 45416 66893.9 2 PROCESSED 55427.1387152778 55793 55427.1529976852 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050010 Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 5 AO5 SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? XIS Y FVW319.8+0.3_BGD 225.4141 -58.3766 319.32044374 0.28957352 278.3765 55413.9313888889 55414.6724768518 505030010 51626.2 50000 51626.2 51663.6 0 51647.6 2 2 0 2 1 0 0 40050.3 40050.3 64017.9 1 PROCESSED 55427.1871759259 55793 55427.2012152778 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050010 Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 5 AO5 SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? XIS Y SGR_C 266.2461 -29.3903 359.54016882 -0.1184914 267.0744 55464.5256481482 55466.608599537 505031010 99916 100000 99956.1 99916 0 99956 3 2 0 2 1 0 0 89071.2 89071.2 179949.9 2 PROCESSED 55484.313125 55853 55484.3402777778 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050018 The Sagittarius C Complex (Sgr C) @is composed of many giant molecular clouds (MCs) in two distinct velocity zones, indicating two separate line-of-sight positions of the MCs. Past X-ray flares of Sgr A* likely produced the FeI 6.4 keV emission in the MCs (XRN: X-ray Reflection Nebulae). In Sgr C, the XRN have been solely found in one of the velocity zones. We hence propose to find new XRN in the other velocity zone, which is possibly located at the different distance from the known XRN. With the Suzaku observation, we will determine the 3-dimensional positions of the XRN. Since the presence (or absence) of the XRN largely depends on the epoch of the Sgr A* flares and the 3-dimensional positions of the MCs, Sgr C is a "Rosetta Stone" of the origin and production of the XRN. GALACTIC DIFFUSE EMISSION 5 A NOBUKAWA MASAYOSHI NULL NULL JAP 5 AO5 THE SAGITTARIUS C COMPLEX A ROSETTA STONE OF THE PAST ACTIVITY OF SAGITTARIUS A* XIS Y JUPITER 0 0 96.33726965 -60.18855175 -99 NULL NULL 505032010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050026 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again under an increased Solar activity. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the Solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. GALACTIC DIFFUSE EMISSION 5 C ISHIKAWA KUMI NULL NULL JAP 5 AO5 STUDY OF DIFFUSE HARD X-RAY EMISSION AROUND JUPITER XIS N W51C-NW 290.81992 14.15403 49.12463783 -0.45897831 -99 NULL NULL 505033010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050029 We propose two XIS observations of the Galactic SNR W51C, which is believed to be interacting with molecular clouds. Significant GeV gamma-ray emission has been observed, which coincides with the entire SNR. The TeV gamma-ray emission, on the contrary, looks more compact and seems to arise from the shock-cloud interaction region, but may also be contaminated by emission from a PWN candidate. We will determine the physics of the shock in an undisturbed and a cloud interaction region through spectroscopy. The TeV emission from the shock-cloud interaction probably witnesses the production of Galactic cosmic rays. The Suzaku observations are also necessary to disentangle the possible PWN-induced TeV emission from the cosmic ray-induced emission. GALACTIC DIFFUSE EMISSION 5 C BAMBA AYA NULL NULL JAP 5 AO5 THE GALACTIC SNR W51C XIS N W51C-SE 290.97658 13.96642 49.0311116 -0.6815655 -99 NULL NULL 505034010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050029 We propose two XIS observations of the Galactic SNR W51C, which is believed to be interacting with molecular clouds. Significant GeV gamma-ray emission has been observed, which coincides with the entire SNR. The TeV gamma-ray emission, on the contrary, looks more compact and seems to arise from the shock-cloud interaction region, but may also be contaminated by emission from a PWN candidate. We will determine the physics of the shock in an undisturbed and a cloud interaction region through spectroscopy. The TeV emission from the shock-cloud interaction probably witnesses the production of Galactic cosmic rays. The Suzaku observations are also necessary to disentangle the possible PWN-induced TeV emission from the cosmic ray-induced emission. GALACTIC DIFFUSE EMISSION 5 C BAMBA AYA NULL NULL JAP 5 AO5 THE GALACTIC SNR W51C XIS N HESSJ1507-622 CENTER 226.72 -62.35 317.94552085 -3.49393593 -99 NULL NULL 505035010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050036 TeV unID sources are the plausible acceleration sites of Galactic cosmic rays, although their nature is still unknown. A TeV unID source, HESS J1507-622 is located at (l, b) = (317.9, -3.5), which is quite distant from Galactic plane compared with other TeV unIDs. It could be an old supernova remnant, a pulsar wind nebula, or a completely new type source people did not notice. We investigate its X-ray counterpart with low and stable background of Suzaku XIS. Our observations permit us to distinguish the former two cases. It is not predictable in the case this source is the new type, but our observation will be able to access its nature detecting thermal and nonthermal X-ray emission. GALACTIC DIFFUSE EMISSION 5 C BAMBA AYA NULL NULL JAP 5 AO5 CATCHING THE NATURE OF THE HIGH-GALACTIC-LATITUDE TEV UNID SOURCE XIS N HESSJ1825-137NORTH1 276.57 -13.48 18.09574729 -0.65769523 -99 NULL NULL 505037010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050037 TeV gamma-ray unidentified sources have been discovered recently. One-sided pulsar wind nebula (PWN) is a possible candidate of them because there are pulsars near them with a few arcmin offset in many cases. HESS J1825-137 is one of the most reliable TeV gamma-ray PWNe. Suzaku AO1 observation, however, revealed its size and velocity for transporting the high-energy electrons are peculiar as an X-ray PWN. Are one-sided PWNe like HESS J1825-137 common objects? What environment generates them? We propose the observation of the north side of HESS J1825-137 to come out them. High sensitivity of XIS will detect weak X-ray emission from the north for the first time. Based on this result, we will uncover what are different between the north and south and why the north is so dark. GALACTIC DIFFUSE EMISSION 5 C UCHIYAMA HIDEKI NULL NULL JAP 5 AO5 SUZAKU OBSERVATION OF THE NORTH SIDE OF HESS J1825-137 XIS N HESSJ1825-137NORTH2 276.77 -13.67 18.01817146 -0.91823197 -99 NULL NULL 505038010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050037 TeV gamma-ray unidentified sources have been discovered recently. One-sided pulsar wind nebula (PWN) is a possible candidate of them because there are pulsars near them with a few arcmin offset in many cases. HESS J1825-137 is one of the most reliable TeV gamma-ray PWNe. Suzaku AO1 observation, however, revealed its size and velocity for transporting the high-energy electrons are peculiar as an X-ray PWN. Are one-sided PWNe like HESS J1825-137 common objects? What environment generates them? We propose the observation of the north side of HESS J1825-137 to come out them. High sensitivity of XIS will detect weak X-ray emission from the north for the first time. Based on this result, we will uncover what are different between the north and south and why the north is so dark. GALACTIC DIFFUSE EMISSION 5 C UCHIYAMA HIDEKI NULL NULL JAP 5 AO5 SUZAKU OBSERVATION OF THE NORTH SIDE OF HESS J1825-137 XIS N DEM L 86 77.4674 -68.8946 279.75652902 -34.25087364 194.4731 55552.1478703704 55552.9495601852 505041010 51468.1 50000 51499.7 51499.7 0 51468.1 2 2 0 2 1 0 0 44258.9 44258.9 69257.9 0 PROCESSED 55607.0780671296 55973 55607.0926851852 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050061 Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles. GALACTIC DIFFUSE EMISSION 5 C NAKAJIMA HIROSHI NULL NULL JAP 5 AO5 UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS XIS Y DEM L 199 81.6473 -68.8371 279.33316137 -32.78488249 187.7916 55551.3246759259 55552.146099537 505042010 51743.4 50000 51756.4 51743.4 0 51756.4 2 2 0 2 1 0 0 48207.9 48207.9 70965.9 0 PROCESSED 55593.1924189815 55961 55593.2050231482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050061 Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles. GALACTIC DIFFUSE EMISSION 5 C NAKAJIMA HIROSHI NULL NULL JAP 5 AO5 UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS XIS Y L139_B-22 31.832 38.829 138.75033014 -21.70040383 -99 NULL NULL 505043010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050064 Suzaku measurements of the large scale variation of the Halo emission surrounding our Galaxy are proposed. To minimize the local emission and absorption structure, we selected three pointings toward the anti-center region (l=140) of the Galactic latitude between-20 and -40. GALACTIC DIFFUSE EMISSION 5 C YAMASAKI NORIKO NULL NULL JAP 5 AO5 STRUCTURE OF THE GALACTIC HALO EMISSION TOWARD THE ANTI-CENTER REGION XIS N L139_B-32 28.093 28.6837 138.75887563 -32.3084393 253.9538 55569.4091319444 55571.3188541667 505044010 84004.1 80000 84004.1 84004.1 0 84004.1 2 2 0 2 1 0 0 79037.7 79037.7 164983.9 0 PROCESSED 55595.1822453704 55962 55595.2037615741 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050064 Suzaku measurements of the large scale variation of the Halo emission surrounding our Galaxy are proposed. To minimize the local emission and absorption structure, we selected three pointings toward the anti-center region (l=140) of the Galactic latitude between-20 and -40. GALACTIC DIFFUSE EMISSION 5 C YAMASAKI NORIKO NULL NULL JAP 5 AO5 STRUCTURE OF THE GALACTIC HALO EMISSION TOWARD THE ANTI-CENTER REGION XIS Y G156.2+1.0 SOUTH 74.901 51.04 156.83347202 5.29052158 -99 NULL NULL 505046010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050067 G156.2+5.7 is a Galactic middle-aged supernova remnant (SNR) whose spectra show both hard-tail and thermal emission. From our previous Suzaku observation, we found the possibility of the correlation between the radio intensity and the hard-tail X-ray emission, which suggests the hard-tail emission is a non-thermal origin. We also found the thermal emission originated from the ejecta. We propose to observe the other regions of the G156.2+5.7 for 150ks in order to determine the origin of the hard-tail emission and to investigate the ejecta distribution which provides a clue to obtaining the information about the progenitor star. GALACTIC DIFFUSE EMISSION 5 C UCHIDA HIROYUKI NULL NULL JAP 5 AO5 X-RAY OBSERVATIONS OF SNR G156.2+5.7 WITH SUZAKU XIS XIS N G156.2+1.0 WEST 74.188 51.617 156.1013943 5.29604774 -99 NULL NULL 505047010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050067 G156.2+5.7 is a Galactic middle-aged supernova remnant (SNR) whose spectra show both hard-tail and thermal emission. From our previous Suzaku observation, we found the possibility of the correlation between the radio intensity and the hard-tail X-ray emission, which suggests the hard-tail emission is a non-thermal origin. We also found the thermal emission originated from the ejecta. We propose to observe the other regions of the G156.2+5.7 for 150ks in order to determine the origin of the hard-tail emission and to investigate the ejecta distribution which provides a clue to obtaining the information about the progenitor star. GALACTIC DIFFUSE EMISSION 5 C UCHIDA HIROYUKI NULL NULL JAP 5 AO5 X-RAY OBSERVATIONS OF SNR G156.2+5.7 WITH SUZAKU XIS XIS N WESTERLUND1_1 251.8398 -46.6023 339.00946678 -0.92860911 283.3468 55449.7733217593 55451.2015740741 505049010 51932 50000 51932 51932 0 51932 2 2 0 2 1 0 0 44843.7 44843.7 123386.1 1 PROCESSED 55461.2921412037 55829 55461.3235069444 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050078 TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. GALACTIC DIFFUSE EMISSION 5 A MATSUMOTO HIRONORI NULL NULL JAP 5 AO5 IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? XIS Y WESTERLUND1_2 252.808 -46.1402 339.79276992 -1.14410237 285.6981 55451.2033912037 55452.6077777778 505050010 52654.1 50000 52654.1 52654.1 0 52654.1 2 2 0 2 1 0 0 42753.6 42753.6 121309.9 0 PROCESSED 55463.1897222222 55829 55463.2091435185 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050078 TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. GALACTIC DIFFUSE EMISSION 5 A MATSUMOTO HIRONORI NULL NULL JAP 5 AO5 IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? XIS Y WESTERLUND1_3 252.0931 -46.1953 339.43313351 -0.79934014 282.1087 55462.25625 55463.3946296296 505051010 50204.6 50000 50204.6 50204.6 0 50204.6 2 2 0 2 1 0 0 40796.6 40796.6 98343.8 1 PROCESSED 55474.0561689815 55840 55474.0771180556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050078 TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. GALACTIC DIFFUSE EMISSION 5 A MATSUMOTO HIRONORI NULL NULL JAP 5 AO5 IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? XIS Y WESTERLUND1_4 253.5509 -45.3005 340.7711384 -1.01287357 288.2868 55463.3974652778 55464.5203587963 505052010 49627 50000 49627 49627 0 49627 2 2 0 2 1 0 0 40213.7 40213.7 97007.9 1 PROCESSED 55474.0821875 55840 55474.1080208333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050078 TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. GALACTIC DIFFUSE EMISSION 5 A MATSUMOTO HIRONORI NULL NULL JAP 5 AO5 IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? XIS Y G1.9+0.3 267.1951 -27.1633 1.87759006 0.32236452 104.4114 55643.1608217593 55645.2856481482 505053010 100923.5 100000 100923.5 100931.5 0 100931.5 2 2 0 2 1 0 0 83425.1 83425.1 183565.7 1 PROCESSED 55658.2211689815 56025 55658.2502546296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050084 We propose to observe the youngest (100yr) SNR G1.9+0.3 with Suzaku for 100 ks. The expected scientific fruits are to reveal the earliest stage of SNR evolution via the time variation of synchrotron emission, and to investigate the nuclear synthesis in the SN explosion via the detection of gamma-ray lines from 44Ti. GALACTIC DIFFUSE EMISSION 5 A KOKUBUN MOTOHIDE NULL NULL JAP 5 AO5 INVESTIGATION OF THE YOUNGEST SNR G1.9+0.3 WITH SUZAKU XIS Y L106_B3 337.3111 61.2453 106.66847152 2.94694679 86.3781 55332.0617013889 55333.5078587963 505054010 59380.4 60000 59380.4 59380.4 0 59380.4 3 2 0 2 1 0 0 54055.1 54055.1 124908 3 PROCESSED 55393.2429166667 55765 55393.2646759259 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050086 We propose observarions of two fields on and near midplane (b = 0 and 3 deg.) in order to study bump-like emission peaked at 0.9 keV observed in midplane. The two fields proposed for observations has been observed by Chandra. By comparing the spectra taken by Suzaku and Chandra, we will determine the contribution of point sources (stars), and investigate posisble contribution of diffuse thermal plasma. GALACTIC DIFFUSE EMISSION 5 B TAKEI YOH NULL NULL JAP 5 AO5 ORIGIN OF SOFT X-RAY EMISSION IN THE MILKY-WAY DISK XIS Y BLOWOUT SHELL 1 311.9978 28.9736 72.22846422 -9.10440661 48.7676 55360.0953587963 55361.2627546296 505055010 52194.5 50000 52218.5 52194.5 0 52218.5 1 1 0 1 1 0 0 43692.7 43692.7 100855.9 1 PROCESSED 55372.2728472222 55741 55375.7594907407 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050088 The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks. GALACTIC DIFFUSE EMISSION 5 B UCHIDA HIROYUKI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION XIS Y BLOWOUT SHELL 2 312.2035 28.7297 72.14669544 -9.39669734 48.0881 55361.263599537 55362.5155439815 505056010 52069.8 50000 52069.8 52069.8 0 52069.8 2 2 0 2 1 0 0 46082.7 46082.7 108155.8 1 PROCESSED 55375.1539814815 55741 55375.7627893518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050088 The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks. GALACTIC DIFFUSE EMISSION 5 B UCHIDA HIROYUKI NULL NULL JAP 5 AO5 X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION XIS Y VICINITY_4U1957+11 300.5977 12.1307 52.0534723 -9.74567764 252.1551 55499.6275578704 55501.8265625 505057010 80583.9 80000 80583.9 80583.9 0 80583.9 2 2 0 2 1 0 0 59204.2 59204.2 189975.9 2 PROCESSED 55515.3407638889 55882 55515.3752083333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050090 We propose for an observation of the vicinity of 4U 1957+11, in order to study the Galactic low-latitude hot gas. Recently, detection of OVII and NeIX aborption lines was reported in the spectrum of 4U 1957+11 (Yao et al. 2008). By combining a Suzaku observation of diffuse hot plasma around the object with the reported absorption line equivalnet widths, we will constrain the temperature, line-of-sight length, density of the hot plasma of the direction. Not only to understand the Galactic gas, but also to understand feedback mechanism from a galaxy to the intergalactic space will our study play an important role. GALACTIC DIFFUSE EMISSION 5 B TAKEI YOH NULL NULL JAP 5 AO5 EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC LOW-LATITUDE HOT GAS XIS Y L168_B53 153.7378 48.0763 167.64470811 53.18666692 109.5667 55519.8069328704 55521.5828356482 505058010 79499.9 80000 79499.9 79499.9 0 79499.9 2 2 0 2 1 0 0 35661.9 35661.9 153421.8 1 PROCESSED 55530.2512847222 55898 55530.2748842593 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050106 A dark patch extending degrees scale was found in the R4-band ROSAT All Sky Survey data from our re-analysis of the map based on the recent Suzaku results. The deficiency is small in R5 band . Strikingly the area well coincides with the dark patch in the 408 MHz emission. This indicates the low cosmic-ray and magnetic pressure of this area. We propose to observe this area to determine the temperature of the halo emission using Oxygen lines and to constrain the thermal pressure of hot interstellar medium. GALACTIC DIFFUSE EMISSION 5 C SEKIYA NORIO NULL NULL JAP 5 AO5 DARK PATCH IN THE GALACTIC HALO X-RAY EMISSION AND ITS POSSIBLE RELATION TO RADIO SYNCHROTRON RADIATION XIS Y W41 278.617 -8.693 23.26854845 -0.21970423 -99 NULL NULL 505059010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050120 We propose to observe the old SNR W41, which is bright in the GeV/TeV Gamma-ray and faint in the X-ray. W41 is very old ~(10^5 years old) and expected that primary electrons accelerated in the shock have been already cooled down. We detect the emission from secondary electrons of which origin are protons, and try to estimate energy densities of electrons and protons, independently, together with Fermi Gamma-ray data. GALACTIC DIFFUSE EMISSION 5 C NISHINO SHO NULL NULL JAP 5 AO5 DETECTION OF THE EMISSION FROM SECONDARY ELECTRONS IN OLD SNR W41 XIS N W30 271.3495 -21.58378 8.60138 -0.14920298 -99 NULL NULL 505060010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050123 We propose to observe the old supernova remnant (SNR) W30 with Suzaku/XIS. W30 interacts with molecular cloud, and the brightness distribution of GeV band is different from TeV band. This suggests that we see the process of diffusion and propagation of cosmic-ray from the acceleration site. To get the evidence of this, we need to determine the proton spectrum shape. But electron bremsstrahlung emission might be dominant in GeV band. Therefore we determine the electron to proton ratio (K_ep) by observing non-thermal X-ray emission from secondary electrons produced by decaying charged pions created by p-p interaction. GALACTIC DIFFUSE EMISSION 5 C HANABATA YOSHITAKA NULL NULL JAP 5 AO5 SUZAKU/XIS OBSERVATION OF NEWLY DICOVERED GEV-TEV ANTI-CORRELATION IN SUPERNOVA REMNANT W30 XIS N HE FOCUSING CONE 49.5833 10.9603 170.9618047 -37.8533007 73.6953 55410.7011921296 55413.1439699074 505061010 101965.1 100000 101973.1 101973.1 0 101965.1 2 2 0 2 1 0 0 89145.2 89145.2 211045.9 2 PROCESSED 55441.3673148148 55808 55441.4075694444 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050129 We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy. GALACTIC DIFFUSE EMISSION 5 B YOSHITAKE HIROSHI NULL NULL JAP 5 AO5 OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE XIS Y HE FOCUSING CONE 49.5928 10.9507 170.97872575 -37.85410489 253.7002 55591.1307291667 55593.7710763889 505062010 100167.8 100000 100167.8 100167.8 0 100167.8 2 2 0 2 1 0 0 82785.2 82785.2 228103.7 2 PROCESSED 55607.2706828704 55973 55607.305462963 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050129 We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy. GALACTIC DIFFUSE EMISSION 5 B YOSHITAKE HIROSHI NULL NULL JAP 5 AO5 OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE XIS Y DEM L238 83.8177 -70.5927 281.24911245 -31.77318091 307.401 55308.023125 55312.9730902778 505063010 199779.5 200000 199779.5 199779.5 0 199779.5 2 2 0 2 1 0 0 167835.5 167835.5 427629.7 5 PROCESSED 55326.6317939815 55287 55326.6889699074 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051102 Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. GALACTIC DIFFUSE EMISSION 5 A BORKOWSKI KAZIMIERZ NULL NULL USA 5 AO5 TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? XIS Y 0534-69.9 83.5094 -69.9134 280.47493809 -31.97334872 273.4822 55286.3873726852 55289.2981597222 505064010 109236.7 100000 109268.7 109236.7 0 109276.7 2 2 0 2 1 0 0 79826.2 79826.2 251443.7 2 PROCESSED 55302.3956018518 55287 55302.4291898148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051102 Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. GALACTIC DIFFUSE EMISSION 5 A BORKOWSKI KAZIMIERZ NULL NULL USA 5 AO5 TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? XIS Y 0548-70.4 86.9619 -70.4173 280.90214015 -30.75163284 12.6051 55378.8779861111 55381.6286689815 505065010 103674.6 100000 103674.6 103674.6 0 103674.6 2 2 0 2 1 0 0 156971.6 156971.6 237635.8 1 PROCESSED 55434.3578819444 55287 55434.3854513889 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051102 Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. GALACTIC DIFFUSE EMISSION 5 B BORKOWSKI KAZIMIERZ NULL NULL USA 5 AO5 TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? XIS Y HB9-WEST 74.90833 46.30111 160.57945638 2.3766747 -99 NULL NULL 505066010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051303 We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9$+$2.6) with {it Suzaku}. HB9 is a member of the class of Galactic SNRs known as mixed-morphology SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission (and whether it is produced by the SNR, a background AGN or intercluster gas associated with the cluster that harbors the AGN) is not clearly understood. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations in the X-ray emitting plasma. GALACTIC DIFFUSE EMISSION 5 C PANNUTI THOMAS NULL NULL USA 5 AO5 A SUZAKU OBSERVATION OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) XIS N HB9-EAST 75.65417 46.17583 160.99530906 2.70715632 -99 NULL NULL 505067010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051303 We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9$+$2.6) with {it Suzaku}. HB9 is a member of the class of Galactic SNRs known as mixed-morphology SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission (and whether it is produced by the SNR, a background AGN or intercluster gas associated with the cluster that harbors the AGN) is not clearly understood. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations in the X-ray emitting plasma. GALACTIC DIFFUSE EMISSION 5 C PANNUTI THOMAS NULL NULL USA 5 AO5 A SUZAKU OBSERVATION OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) XIS N VELA SNR CB1 130.2067 -44.4709 263.57895082 -1.58638955 294.2634 55318.1574074074 55318.5738425926 505068010 23666.5 20000 23666.5 23678 0 23666.5 1 1 0 1 1 0 0 18818 18818 35975.9 1 PROCESSED 55330.1280787037 55696 55330.1358449074 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051304 The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 5 AO5 IRON-RICH EJECTA BULLET IN THE VELA SNR XIS Y VELA SNR CB2 130.2058 -44.7742 263.81853128 -1.77251278 293.5729 55318.5746412037 55318.9238425926 505069010 19380.5 20000 19412.5 19404.5 0 19380.5 1 1 0 1 1 0 0 18829.8 18829.8 30167.9 0 PROCESSED 55330.2048842593 55696 55330.2121643518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051304 The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 5 AO5 IRON-RICH EJECTA BULLET IN THE VELA SNR XIS Y VELA SNR CB3 129.7826 -44.6964 263.57338638 -1.96329272 278.1748 55318.927974537 55319.3418402778 505070010 18171.8 20000 18171.8 18171.8 0 18171.8 2 2 0 2 1 0 0 17154.4 17154.4 35753.9 1 PROCESSED 55330.1199768518 55696 55330.1275925926 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051304 The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 5 AO5 IRON-RICH EJECTA BULLET IN THE VELA SNR XIS Y VELA SNR CB-LBG 130.6266 -44.6167 263.87788945 -1.43970243 293.482 55319.3460648148 55319.7940046296 505071010 27179.9 20000 27179.9 27179.9 0 27179.9 2 2 0 2 1 0 0 25094.5 25094.5 38693.9 1 PROCESSED 55330.1455092593 55696 55330.1543981482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051304 The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 5 AO5 IRON-RICH EJECTA BULLET IN THE VELA SNR XIS Y SNR G106.3+2.7 P2 336.9121 60.9439 106.34649405 2.79001657 12.2687 55423.4230787037 55424.0209837963 505072010 24556.2 50000 24572.2 24556.2 0 24572.2 1 1 0 1 1 0 0 26614.7 26614.7 51655.9 1 PROCESSED 55441.25875 55807 55441.2685069444 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051305 After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. GALACTIC DIFFUSE EMISSION 5 C ALIU ESTER NULL NULL USA 5 AO5 ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 XIS Y SNR G106.3+2.7 P3 336.5055 60.7692 106.0859109 2.74547808 12.2692 55424.0215509259 55424.9841782407 505073010 50454.8 50000 50462.8 50454.8 0 50463.2 2 2 0 2 1 0 0 50210.5 50210.5 83163.9 1 PROCESSED 55439.1147453704 55805 55439.1312037037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051305 After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. GALACTIC DIFFUSE EMISSION 5 C ALIU ESTER NULL NULL USA 5 AO5 ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 XIS Y SNR G304.6+0.1 196.4463 -62.6951 304.57643925 0.13082789 321.0575 55442.9126736111 55445.5356828704 505074010 99581.7 100000 99621.7 99581.7 0 99629.7 2 2 0 2 1 0 0 90565.3 90565.3 226531.9 1 PROCESSED 55461.3917013889 55827 55461.4231712963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051306 Galactic supernova remnants are believed to be the primary source of cosmic rays below 10^15.5 eV even though the exact acceleration mechanism remains unknown. This uncertainty results from the lack of remnants with synchrotron X-ray and GeV emission, needed to distinguish accelerated electrons from protons using broadband spectral modeling. An analysis of recent XMM and Fermi data suggests SNR G304.6+0.1 is just the third remnant with both, but the observed hard X-ray excess is also consistent with bremsstrahlung emission. We request a deep Suzaku observation of this source to determine the nature of its hard X-ray emission - critical for identifying the underlying acceleration mechanism. GALACTIC DIFFUSE EMISSION 5 B GELFAND JOSEPH NULL NULL USA 5 AO5 THE ORIGIN OF THE HARD X-RAY AND GEV GAMMA-RAY EMISSION OF SNR G304.6+0.1 XIS Y CARINA SW 160.2531 -60.104 287.34811018 -1.23919183 109.6766 55542.7308333333 55543.4438888889 505075010 47003.9 45000 47003.9 47011.9 0 47011.9 1 1 0 1 1 0 0 42434.1 42434.1 61599.9 0 PROCESSED 55592.9127662037 55960 55592.9230324074 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051312 X-ray nebulae with kT =0.1-0.8 keV, log Lx up to 35 ergs/s, and size of 1-1000 pc accompany a number of giant HII region. The Carinae Nebula is the best region to study their origin with 10-100 times more luminous soft X-rays than any other giant HII regions in our Galaxy. X-ray observations especially with Suzaku revealed that a part, or all, of the diffuse plasma would heat up by earlier supernova explosions, but it is unknown when these explosions occurred and how they made the current X-ray nebula. The Chandra Carina Complex Project displayed that the southern part of the nebula emits strong hydrogen-like oxygen line. We will measure helium-like oxygen line with Suzaku to measure its plasma temperature and abundance to help understand relation with plasma in the nebula center. GALACTIC DIFFUSE EMISSION 5 C HAMAGUCHI KENJI NULL NULL USA 5 AO5 SOUTHERN PART OF DIFFUSE PLASMA IN THE CARINA NEBULA - RICH IN OXYGEN? XIS Y AX J1714.1-3912 258.5249 -39.1972 347.85266774 -0.22742448 85.6964 55608.0538078704 55608.9654050926 505076010 32601.7 30000 32601.7 32601.7 0 32601.7 2 2 0 2 1 0 0 28336.2 28336.2 78757.9 1 PROCESSED 55621.124375 55988 55621.1409027778 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052012 Molecular clouds are predicted to emit strong non-thermal X-rays when they are close to particle-accelerating SNRs, but this emission has not been confirmed yet. We propose to observe the non-thermal X-ray source AX J1714.1-3912 to investigate its relationship with the SNR RX J1713.7-3946. ASCA observations have shown that the hard spectrum of the source may be associated with bremsstrahlung emission from particles accelerated in the SNR and diffusing in a nearby molecular cloud. This emission has never been observed in other SNRs. However, the association of the source with the remnant is still controversial and the ASCA data do not allow us to constrain the spectral properties. We aim at verifying the association with the remnant and at investigating the physical origin of the emission. GALACTIC DIFFUSE EMISSION 5 A MICELI MARCO NULL NULL EUR 5 AO5 INVESTIGATING THE PHYSICAL ORIGIN OF AX J1714.1-3912 XIS Y W41-EAST 278.56 -8.97 22.99674923 -0.29734516 -99 NULL NULL 505077010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052020 Although the properties of supernova remnants (SNRs) generically follow a standard model, individual regions do present a lot of variety, related to the SNR environment, where disentangling possible physical processes is still challenging. W41 (SNR G23.3-03) and SNR G22.7-0.2 are both well-resolved shells (26' and 27' in diameter), observed in a large multi-wavelength dataset, possibly in interaction together. Infrared data indicates unusual emission for such objects, hinting of conditions favorable to non-thermal processes. These circumstances make the region between these two SNR a good candidate for a detailed study in the keV band. GALACTIC DIFFUSE EMISSION 5 C CLAPSON ANDRE-CLAUDE NULL NULL EUR 5 AO5 EXPLORING AN INFRARED-TEV CONNECTION IN A POTENTIAL SNR-SNR INTERACTION REGION XIS N GALACTIC_BULGE3 267.9488 -29.7963 359.95634845 -1.5962466 107.1729 55624.8013310185 55626.2292939815 505078010 51275.6 50000 51275.6 51275.6 0 51275.6 2 2 0 2 1 0 0 39312.4 39312.4 123361.8 0 PROCESSED 55642.0974537037 55287 55642.1205787037 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE4 269.1417 -30.4015 359.95546853 -2.79264334 69.3552 55632.2752314815 55633.4287152778 505079010 50219.3 50000 50227.3 50219.3 0 50227.3 2 2 0 2 1 0 0 43375 43375 99648 1 PROCESSED 55645.2976388889 55287 55645.5706134259 2.5.16.29 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE5 270.1525 -30.903 359.95222621 -3.79644913 86.7823 55293.7188657407 55295.8849074074 505080010 56139.6 50000 56139.6 56139.6 0 56139.6 2 2 0 2 1 0 0 55149.8 55149.8 185005.8 1 PROCESSED 55441.1996527778 55287 55441.4355555556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE6 271.3758 -31.4828 359.95693453 -4.99276165 88.0304 55639.361087963 55640.3565162037 505081010 50166.9 50000 50171.4 50166.9 0 50179.5 3 2 0 2 1 0 0 43635.7 43635.7 85989.8 0 PROCESSED 55649.205162037 55287 55649.2186574074 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE13 264.5912 -32.1955 356.40747371 -0.39354159 92.0351 55635.5794907407 55636.621099537 505082010 48496.9 50000 48512.9 48512.9 0 48496.9 2 2 0 2 1 0 0 41255 41255 89979.8 0 PROCESSED 55648.3226157407 55287 55648.3385763889 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE14 264.9946 -32.433 356.38820164 -0.80858885 270.5244 55479.5865509259 55480.8980671296 505083010 52938.3 50000 52938.3 52938.3 0 52938.3 1 1 0 1 1 0 0 42407.3 42407.3 113303.9 1 PROCESSED 55491.0279282407 55287 55491.0402893518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE15 265.6963 -32.7784 356.40742505 -1.49294303 89.8786 55626.2338425926 55627.5424884259 505084010 50309.7 50000 50317.2 50309.7 0 50325.2 1 1 0 1 1 0 0 37509.5 37509.5 113055.9 0 PROCESSED 55645.2581828704 55287 55645.2697222222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE16 266.5113 -33.2224 356.38592507 -2.30771737 275.4625 55482.2533217593 55483.5626967593 505085010 55031.5 50000 55031.5 55031.5 0 55031.5 2 2 0 2 1 0 0 48634.1 48634.1 113113.9 1 PROCESSED 55502.2701967593 55287 55502.290150463 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE17 267.7467 -33.8391 356.3863118 -3.50805248 275.261 55483.5637731482 55485.0627893518 505086010 53126.6 50000 53126.6 54089.5 0 54089.5 2 2 0 2 1 0 0 46276.9 46276.9 129493.8 1 PROCESSED 55508.1799537037 55287 55508.2025694444 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y GALACTIC_BULGE18 269.3126 -34.5716 356.40349802 -4.99577293 70.9023 55633.4308101852 55634.5273263889 505087010 51428.4 50000 51468.4 51428.4 0 51475.5 1 1 0 1 1 0 0 44207.2 44207.2 94727.9 1 PROCESSED 55649.0303819444 55287 55649.0417824074 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y HESS J1841-55 1 279.8307 -5.8897 26.31151486 -0.00077944 87.7391 55645.2916782407 55646.4446180556 505088010 49652 50000 49652 49652 0 49652 2 2 0 2 1 0 0 39860.4 39860.4 99597.8 0 PROCESSED 55658.1409837963 55287 55658.1566087963 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y HESS J1841-55 2 280.1473 -5.9564 26.39650339 -0.31125339 87.3564 55646.4452777778 55647.6391550926 505089010 50005.3 50000 50030.4 50005.3 0 50030.4 3 2 0 2 1 0 0 43178.9 43178.9 103113.9 0 PROCESSED 55658.192974537 55287 55658.2084606482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y HESS J1841-55 3 280.1471 -5.609 26.70525302 -0.15199861 87.0298 55647.6397685185 55648.791875 505090010 49549 50000 49581 49549 0 49581 2 2 0 2 1 0 0 42793.5 42793.5 99523.9 1 PROCESSED 55666.2513888889 55287 55666.2655439815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y HESS J1841-55 4 280.4555 -5.2917 27.12788601 -0.27973073 86.6744 55648.7926273148 55649.9633449074 505091010 51253.9 50000 51253.9 51253.9 0 51253.9 2 2 0 2 1 0 0 45007.8 45007.8 101142 1 PROCESSED 55666.2838194444 55287 55666.3000115741 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y THE KEPLER SNR 262.6745 -21.5044 4.50818409 6.8092486 272.4561 55469.9826736111 55470.368287037 505092010 17714.1 620000 17722.1 17730.1 0 17714.1 2 2 0 2 1 0 0 17869.4 17869.4 33307.9 0 PROCESSED 55482.1206018518 55287 55482.4747453704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y THE KEPLER SNR 262.6737 -21.5073 4.50532186 6.80830692 272.2663 55475.6914583333 55478.2863194445 505092020 111194.1 620000 111194.1 111202.1 0 111202.1 2 2 0 2 1 0 0 99841.3 99841.3 224143.7 2 PROCESSED 55488.2966550926 55287 55488.3311689815 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y THE KEPLER SNR 262.6706 -21.4823 4.52493262 6.82424916 102.5027 55615.8474421296 55616.8174768518 505092030 34201.5 150000 34209.5 34201.5 0 34209.5 2 2 0 2 1 0 0 29119.9 29119.9 83795.8 0 PROCESSED 55628.1552777778 55287 55628.1747569444 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y THE KEPLER SNR 262.6707 -21.4823 4.52498329 6.82417088 98.3356 55620.8079166667 55624.797337963 505092040 146233.7 250000 146233.7 146254.1 0 146257.7 2 2 0 2 1 0 0 113802.2 113802.2 344657.7 6 PROCESSED 55642.3599074074 55287 55642.4090046296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y THE KEPLER SNR 262.671 -21.4826 4.5248811 6.82377384 98.1034 55628.0376736111 55632.2696643518 505092050 84591.3 100000 84591.3 85663.2 0 85719.2 4 3 0 3 1 0 0 122488.1 122488.1 365616 3 PROCESSED 55648.4411574074 55287 55648.4964699074 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y THE KEPLER SNR 262.6712 -21.4826 4.52498243 6.82361728 97.9009 55634.5331712963 55635.5759606482 505092060 46496.1 100000 46640.1 46496.1 0 46640.1 2 2 0 2 1 0 0 38611.8 38611.8 90050 1 PROCESSED 55648.2825694444 55287 55648.2987731482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y THE KEPLER SNR 262.671 -21.485 4.52284766 6.82247636 99.4153 55649.9685416667 55653.0828356482 505092070 133390.6 90000 133398.6 133398.6 0 133390.6 2 2 0 2 1 0 0 112217.2 112217.2 269027.8 1 PROCESSED 55666.4861458333 55287 55666.5226736111 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A PARK SANGWOOK NULL NULL USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y G26.0+0.0 279.67254 -6.19283 25.97001135 -9.9e-07 -99 NULL NULL 506001010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060009 ASCA galactic plane survey discovered extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they have thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. GALACTIC DIFFUSE EMISSION 5 C YAMAUCHI SHIGEO NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA XIS N G35.5+0.0 284.03112 2.28542 35.50002141 -4.55e-06 -99 NULL NULL 506002010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060009 ASCA galactic plane survey discovered extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they have thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. GALACTIC DIFFUSE EMISSION 5 C YAMAUCHI SHIGEO NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA XIS N BD+43 3654 308.4185 44.0658 82.48241574 2.36274642 104.8287 55655.0785416667 55657.0925231482 506004010 97047.8 100000 98963.8 97047.8 0 98963.8 3 2 0 2 1 0 0 88925.6 88925.6 173987.7 0 PROCESSED 55670.2807407407 56037 55670.3073842593 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060010 It is very important to search for possible particle-acceleration sites among the astrophysical objects. Very recently, synchrotron emission has been discovered with the VLA radio observation from a bow shock region of a runaway star, BD+43 3654, having a very fast stellar wind whose velocity reaches up to 2300 km/s. The maximum energy is estimated to be about 10 TeV, and thus the emission should come to the X-ray band. Here, we propose to perform the 100 ksec observation of BD+43 3654 with Suzaku, in order to determine the strength of the shock from the temperature of the post-shock plasma and to determine the maximum energy of the accelerated electrons. GALACTIC DIFFUSE EMISSION 5 A TERADA YUKIKATSU NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF NON-THERMAL EMISSION FROM A BOW SHOCK REGION OF A RUNAWAY STAR, BD+43 3654 XIS Y HB21 SOUTH 311.2512 50.6016 88.85305014 4.80482025 105.492 55660.3542361111 55662.8155208333 506005010 132363 150000 132371 132371 0 132363 3 2 0 2 1 0 0 141788.7 141788.7 212635.9 1 PROCESSED 55677.2556365741 56159 55677.2811342593 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060011 Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 6 AO6 ORIGIN OF OVER-IONIZATION OF SNR PLASMAS XIS Y HB21 SOUTH 311.2245 50.5821 88.82715261 4.80607932 6.557 55767.8922337963 55768.4953819444 506005020 23460.7 20000 23468.7 23476.7 0 23460.7 2 2 0 2 1 0 0 26264.9 26264.9 52103.9 1 PROCESSED 55792.1478125 56159 55792.1611458333 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060011 Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma. GALACTIC DIFFUSE EMISSION 5 A BAMBA AYA NULL NULL JAP 6 AO6 ORIGIN OF OVER-IONIZATION OF SNR PLASMAS XIS Y JUPITER 28.6779 10.4549 147.25964186 -49.40473582 249.1856 55929.8714467593 55930.8243865741 506006010 33533.1 160000 33533.1 33533.1 0 33533.1 2 2 0 2 1 0 0 32136.9 32136.9 82323.9 1 PROCESSED 55946.180462963 56316 55946.1978472222 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060017 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. GALACTIC DIFFUSE EMISSION 5 B ISHIKAWA KUMI NULL NULL JAP 6 AO6 STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE XIS Y JUPITER 28.7092 10.4688 147.29554938 -49.38035583 249.1847 55930.8245717593 55931.8508564815 506006020 35518 160000 35522 35518 0 35526 2 2 0 2 1 0 0 34367 34367 88659.9 0 PROCESSED 55946.2078587963 56316 55946.2294097222 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060017 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. GALACTIC DIFFUSE EMISSION 5 B ISHIKAWA KUMI NULL NULL JAP 6 AO6 STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE XIS Y JUPITER 28.9811 10.6021 147.5984875 -49.15640747 249.1843 55937.2038773148 55938.208599537 506006030 34894.2 160000 34902.2 34910.2 0 34894.2 2 2 0 2 1 0 0 32208.1 32208.1 86791.8 2 PROCESSED 55952.1530439815 56319 55952.170787037 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060017 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. GALACTIC DIFFUSE EMISSION 5 B ISHIKAWA KUMI NULL NULL JAP 6 AO6 STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE XIS Y JUPITER 29.0345 10.6283 147.65759499 -49.11229838 249.1849 55938.2087962963 55939.2481944444 506006040 38628.9 160000 38628.9 38636.7 0 38636.9 2 2 0 2 1 0 0 31769.2 31769.2 89785.9 0 PROCESSED 56020.1506481482 56388 56020.1680208333 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060017 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. GALACTIC DIFFUSE EMISSION 5 B ISHIKAWA KUMI NULL NULL JAP 6 AO6 STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE XIS Y JUPITER 29.0829 10.6504 147.71201597 -49.07381266 249.1851 55939.2483912037 55939.8634722222 506006050 23282.7 160000 23290.7 23282.7 0 23295.4 2 2 0 2 1 0 0 19267.9 19267.9 53136 0 PROCESSED 55960.1274421296 56331 55960.1390740741 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060017 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. GALACTIC DIFFUSE EMISSION 5 B ISHIKAWA KUMI NULL NULL JAP 6 AO6 STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE XIS Y CYGNUS LOOP W-B-N 311.1498 30.6623 73.11766027 -7.48614398 71.1125 55692.7736574074 55693.7709606482 506007010 45900.6 44000 45900.6 45900.6 0 45900.6 2 2 0 2 1 0 0 40833.7 40833.7 86133.9 0 PROCESSED 55705.1258796296 56072 55705.1432523148 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060042 The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 6 AO6 HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT XIS Y CYGNUS LOOP W-B-S 311.1967 30.3719 72.9110541 -7.69596159 71.021 55693.7715277778 55694.9794212963 506008010 55649.9 56000 55649.9 55649.9 0 55649.9 2 2 0 2 1 0 0 49851.6 49851.6 104325.9 1 PROCESSED 55705.1624305556 56072 55705.1847800926 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060042 The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM. GALACTIC DIFFUSE EMISSION 5 A TSUNEMI HIROSHI NULL NULL JAP 6 AO6 HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT XIS Y HESSJ1858-A 284.58333 2.09 35.57806275 -0.58016829 -99 NULL NULL 506009010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060043 HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles. GALACTIC DIFFUSE EMISSION 5 C SAKAI MICHITO NULL NULL JAP 6 AO6 DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU XIS Y HESSJ1858-B 284.42917 2.2075 35.61225232 -0.38946093 -99 NULL NULL 506010010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060043 HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles. GALACTIC DIFFUSE EMISSION 5 C SAKAI MICHITO NULL NULL JAP 6 AO6 DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU XIS Y CYGNUS LOOP BLOWOUT1 312.1499 29.2487 72.53069275 -9.03908096 78.1532 55686.7775578704 55687.8494907407 506011010 48564.1 50000 48564.1 48564.1 0 48564.1 2 2 0 2 1 0 0 42042.9 42042.9 92579.9 1 PROCESSED 55698.3095138889 56066 55698.3278472222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A UCHIDA HIROYUKI NULL NULL JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y CYGNUS LOOP BLOWOUT2 312.4423 29.4154 72.82314938 -9.13589092 78.1524 55687.8500578704 55688.6488310185 506012010 35655 35000 35655 35655 0 35655 2 2 0 2 1 0 0 31481.5 31481.5 68982.1 0 PROCESSED 55699.7475578704 56066 55700.4593865741 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A UCHIDA HIROYUKI NULL NULL JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y CYGNUS LOOP BLOWOUT3 312.3799 29.0257 72.47923846 -9.33489782 78.1517 55688.6493981482 55689.9654976852 506013010 60266.9 60000 60266.9 60274.9 0 60266.9 2 2 0 2 1 0 0 55980.3 55980.3 113628.8 1 PROCESSED 55699.7543287037 56066 55700.4602083333 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A UCHIDA HIROYUKI NULL NULL JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y CYGNUS LOOP BLOWOUT4 312.6611 29.185 72.76042835 -9.42856877 61.4261 55707.9937268518 55708.6620486111 506014010 26055.1 25000 26055.1 26063.1 0 26071.1 2 2 0 2 1 0 0 20271.3 20271.3 57737.9 0 PROCESSED 55725.2335648148 56092 55725.2494097222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A UCHIDA HIROYUKI NULL NULL JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y CYGNUS LOOP BLOWOUT5 312.5999 28.7931 72.41540255 -9.63024021 60.972 55708.6627546296 55709.5335185185 506015010 36755.2 35000 36763.2 36755.2 0 36769.5 3 2 0 2 1 0 0 31631.7 31631.7 75216 1 PROCESSED 55725.2282638889 56093 55725.2447569444 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A UCHIDA HIROYUKI NULL NULL JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y CYGNUS LOOP BLOWOUT6 312.8964 28.9665 72.71699713 -9.72555156 78.1534 55691.9894791667 55692.7710069445 506016010 36374.4 35000 36374.4 36374.4 0 36374.4 2 2 0 2 1 0 0 32756.8 32756.8 67503.9 0 PROCESSED 55701.1827430556 56068 55701.1981828704 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A UCHIDA HIROYUKI NULL NULL JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y GAMMACYGNI_NWSHELL1 304.9359 40.8711 78.38707497 2.60425327 82.9977 55664.4219675926 55665.3022222222 506017010 39027.1 40000 39027.1 39027.1 0 39027.1 2 2 0 2 1 0 0 37696.5 37696.5 76052 0 PROCESSED 55690.9438888889 56058 55690.9556597222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060059 We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band. GALACTIC DIFFUSE EMISSION 5 B TANAKA YASUYUKI NULL NULL JAP 6 AO6 SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL XIS Y GAMMACYGNI_NWSHELL2 304.652 40.6975 78.12229495 2.68416641 82.9982 55665.3027430556 55666.2688657407 506018010 39712 40000 39712 39712 0 39712 2 2 0 2 1 0 0 36116.5 36116.5 83437.9 0 PROCESSED 55690.9662268518 56058 55690.9818402778 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060059 We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band. GALACTIC DIFFUSE EMISSION 5 B TANAKA YASUYUKI NULL NULL JAP 6 AO6 SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL XIS Y HESSJ1857-A 284.2126 2.7519 35.99783049 0.0515802 269.8116 55822.9197800926 55823.984212963 506019010 40924.9 40000 40924.9 40924.9 0 40924.9 2 2 0 2 1 0 0 35846.9 35846.9 91927.9 1 PROCESSED 55865.2189699074 56233 55865.2326157407 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060061 Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 6 AO6 ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? XIS Y HESSJ1857-B 284.5485 2.7494 36.14879968 -0.24805898 252.48 55866.7917592593 55867.6946990741 506020010 40686.9 40000 40686.9 40694.9 0 40694.9 2 2 0 2 1 0 0 40051.3 40051.3 78011.9 0 PROCESSED 55879.1573726852 56246 55879.1725 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060061 Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 6 AO6 ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? XIS Y HESSJ1832 278.156 -8.4222 23.29856204 0.30967904 88.1963 55659.2543518518 55660.3454282407 506021010 40343.2 40000 40343.2 40343.2 0 40343.2 2 2 0 2 1 0 0 34851.3 34851.3 94257.8 1 PROCESSED 55673.277037037 56043 55673.2950925926 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060061 Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. GALACTIC DIFFUSE EMISSION 5 B MATSUMOTO HIRONORI NULL NULL JAP 6 AO6 ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? XIS Y HESSJ1857-BGD 284.08333 2.43333 35.6554373 0.02107939 -99 NULL NULL 506022010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060061 Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. GALACTIC DIFFUSE EMISSION 5 C MATSUMOTO HIRONORI NULL NULL JAP 6 AO6 ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? XIS N HESSJ1832-BGD 278.33333 -8.08333 23.68018299 0.31040074 -99 NULL NULL 506023010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060061 Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. GALACTIC DIFFUSE EMISSION 5 C MATSUMOTO HIRONORI NULL NULL JAP 6 AO6 ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? XIS N 3C 59 VICINITY 1 32.0992 30.0806 142.1363254 -29.90513458 254.1341 55940.8410763889 55942.215474537 506024010 55858.1 50000 55858.1 55858.1 0 55858.1 2 2 0 2 1 0 0 46040.4 46040.4 118737.9 1 PROCESSED 55960.1818055556 56331 55960.1998032407 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060067 We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed. GALACTIC DIFFUSE EMISSION 5 C SAKAI KAZUHIRO NULL NULL JAP 6 AO6 STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM XIS Y 3C 59 VICINITY 2 31.42708 28.93236 141.94266779 -31.18293681 -99 NULL NULL 506025010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060067 We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed. GALACTIC DIFFUSE EMISSION 5 C SAKAI KAZUHIRO NULL NULL JAP 6 AO6 STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM XIS Y MBM12 43.9954 19.5008 159.17119109 -34.46234987 73.4994 55776.7501388889 55780.4398263889 506026010 150320.2 150000 150320.2 150320.2 0 150320.2 2 2 0 2 1 0 0 143534.9 143534.9 280761.8 5 PROCESSED 55799.6337731482 56169 55802.465625 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060068 We propose an observation toward dense molecular cloud region MBM12 that is in front of the Local Hot Bubble. Solar wind charge exchange induced emission, reacted with neutrals in the heliosphere (H-SWCX), is considered to have significant influence to the soft diffuse X-ray background under 1 keV. However, there is no significant evidence of the H-SWCX. From this observation, we try to reveal the existence of H-SWCX induced emission by comparing the OVII line emission (0.57 keV) with Suzaku archive data. We also aim to constrain the time variability of H-SWCX emission, depending on the 12 year solar activity. GALACTIC DIFFUSE EMISSION 5 A YOSHITAKE HIROSHI NULL NULL JAP 6 AO6 OBSERVATION TOWARD MOLECULAR CLOUD MBM12 : VERIFYING SOLAR WIND CHARGE EXCHANGE EMISSION IN THE HELIOSPHERE XIS Y NGC 7618 349.8326 42.9144 105.51742003 -16.82119292 269.9991 55911.4056828704 55913.6161458333 506027010 101177.2 100000 101185.2 101177.2 0 101185.2 2 2 0 2 1 0 0 95774 95774 190939.9 0 PROCESSED 55922.0822685185 56289 55922.1112847222 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060073 We propose to observe nearby merging galaxy group NGC 7618. The asymmetric X-ray shape with a tail and a sharp brightness discontinuity were discoverd by observations of ASCA and Chandra. This is due to a merging with an another galaxy group, UGC 12491, which has similar mass of NGC 7618. The pair is in the primary stage of merging, then we need to obtain the information of the gas outside region to clarify the process of the merging. By taking advantage of low background and high energy resolution of XIS, we estimate accurately distribuion of temperature and metal abundances around both galaxy groups. Then we aim to clarify the process of the merging system of the galaxy groups. GALACTIC DIFFUSE EMISSION 5 C HAYASHI KATSUHIRO NULL NULL JAP 6 AO6 OBSERVATION OF NEARBY MERGING GALAXY GROUP NGC 7618 XIS Y H2356_VICINITY_A 359.8969 -30.2089 14.71906615 -78.22459894 68.0006 55696.8464583333 55698.0938773148 506028010 52165.7 50000 52165.7 52165.7 0 52165.7 2 2 0 2 1 0 0 46579.1 46579.1 107753.9 1 PROCESSED 55708.0495601852 56075 55708.0697106482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060075 We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium. GALACTIC DIFFUSE EMISSION 5 A TAKEI YOH NULL NULL JAP 6 AO6 EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS XIS Y H2356_VICINITY_B 359.9868 -29.9493 15.89682365 -78.35224854 69.5008 55698.0951388889 55699.3474305556 506029010 51407.2 50000 51431.2 51423.2 0 51407.2 2 2 0 2 1 0 0 42546 42546 108155.9 1 PROCESSED 55708.0827546296 56075 55708.1035069444 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060075 We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium. GALACTIC DIFFUSE EMISSION 5 A TAKEI YOH NULL NULL JAP 6 AO6 EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS XIS Y S147_NE 85.8826 28.3008 180.30181638 -0.72311498 273.9004 55996.1741666667 55997.2919097222 506030010 48014.2 45000 48030.2 48014.2 0 48038.2 2 2 0 2 1 0 0 42608 42608 96555.9 0 PROCESSED 56016.4654513889 56385 56016.6658912037 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060080 We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it. GALACTIC DIFFUSE EMISSION 5 C HANABATA YOSHITAKA NULL NULL JAP 6 AO6 STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION XIS Y S147_N 87.0463 27.5187 181.50494456 -0.25223067 273.8998 55997.2930324074 55998.555787037 506031010 54883.3 55000 54891.3 54883.3 0 54891.3 2 2 0 2 1 0 0 52191.9 52191.9 109054 1 PROCESSED 56016.4681944444 56385 56016.6668287037 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060080 We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it. GALACTIC DIFFUSE EMISSION 5 C HANABATA YOSHITAKA NULL NULL JAP 6 AO6 STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION XIS Y HESS J1834-087_1 278.68875 -8.74611 23.25407503 -0.30711673 -99 NULL NULL 506032010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060081 Recently, Suzaku discovered extremely large X-ray nebulae around very old pulsars, with excellent detection capability for diffuse faint X-rays. It is quite difficult to reproduce only with simple diffusion and cooling models. However, the number of sample is not many enough to be regarded as a typical characteristic of pulsar wind nebulae (PWNe). In order to confirm this extended emission, we propose to observe the possible oldest (in other words, largest) PWN, HESS J1834-087. Suzaku mapping observations of this source will enable us to judge whether the nebula is largely extended or not, and show us the PWN evolution up to ~120 kyr. GALACTIC DIFFUSE EMISSION 5 C FUJINAGA TAKAHISA NULL NULL JAP 6 AO6 THE OLDEST PULSAR WIND NEBULA HESS J1834-087 XIS N HESS J1834-087_2 278.86958 -8.90778 23.1928022 -0.54016722 -99 NULL NULL 506033010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060081 Recently, Suzaku discovered extremely large X-ray nebulae around very old pulsars, with excellent detection capability for diffuse faint X-rays. It is quite difficult to reproduce only with simple diffusion and cooling models. However, the number of sample is not many enough to be regarded as a typical characteristic of pulsar wind nebulae (PWNe). In order to confirm this extended emission, we propose to observe the possible oldest (in other words, largest) PWN, HESS J1834-087. Suzaku mapping observations of this source will enable us to judge whether the nebula is largely extended or not, and show us the PWN evolution up to ~120 kyr. GALACTIC DIFFUSE EMISSION 5 C FUJINAGA TAKAHISA NULL NULL JAP 6 AO6 THE OLDEST PULSAR WIND NEBULA HESS J1834-087 XIS N CTB1_SW 359.716 62.4332 116.89133919 0.1796486 252.1748 55924.1262037037 55924.6251736111 506034010 28941.9 50000 28941.9 28949.9 0 28949.9 2 2 0 2 1 0 0 25385 25385 43108 0 PROCESSED 55944.1953703704 56313 55972.6473958333 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060086 CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1. GALACTIC DIFFUSE EMISSION 5 C NAKASHIMA SHINYA NULL NULL JAP 6 AO6 NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT XIS Y CTB1_NE 0.2869 62.6043 117.18345572 0.29518062 253.7193 55923.0281134259 55924.1251736111 506035010 52666 50000 52666 52666 0 52666 2 2 0 2 1 0 0 48310.8 48310.8 94775.9 3 PROCESSED 55944.1957291667 56313 55972.6734490741 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060086 CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1. GALACTIC DIFFUSE EMISSION 5 C NAKASHIMA SHINYA NULL NULL JAP 6 AO6 NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT XIS Y W28WEST 269.8372 -23.6072 6.15250357 0.06606197 270.1135 55844.0583217593 55848.1342708333 506036010 151089.2 150000 151097.2 151089.2 0 151092.3 2 2 0 2 1 0 0 128979.7 128979.7 352125.9 2 PROCESSED 55872.455787037 56240 55872.5113425926 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060095 W28 is a mixed-morphology supernova remnant (MM SNR). Recently, GeV and TeV gamma-ray emission have been detected from the eastern edge of W28. On the other hand, we have observed the central region of W28 and have detected an over-ionized plasma, which can not be produced in the canonical evolution of SNRs. Several SNRs have been turned out to host a over-ionized plasma. All of them are MM SNR and are showing GeV and/or TeV emission. This indicates that there are some physical connections between the existence of high-energy cosmic rays and over-ionized plasma. W28 is the best place to study this possible connection due to the large apparent size. Thus, we propose Suzaku observation of western region of W28, which has not been covered by the previous mapping observations. GALACTIC DIFFUSE EMISSION 5 A SAWADA MAKOTO NULL NULL JAP 6 AO6 THE SNR W28 - SEARCHING FOR THE PHYSICAL CONNECTION BETWEEN HIGH-ENERGY COSMIC RAYS AND OVER-IONIZED PLASMA XIS Y CTB109 NOTHWEST 345.2638 59.0349 109.14185824 -0.84931137 252.0017 55908.2838078704 55909.1988078704 506037010 40748.8 40000 40748.8 40756.8 0 40764.8 2 2 0 2 1 0 0 39201 39201 79044 0 PROCESSED 55921.023275463 56288 55921.0397685185 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060100 Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. GALACTIC DIFFUSE EMISSION 5 C NAKANO TOSHIO NULL NULL JAP 6 AO6 SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 XIS Y CTB109 SOUTHWEST 345.0971 58.7572 108.94859975 -1.06655489 252.0045 55909.1993287037 55910.0807407407 506038010 41382.4 40000 41390.4 41382.4 0 41398.4 2 2 0 2 1 0 0 38779 38779 76135.8 0 PROCESSED 55921.9641550926 56289 55921.9811574074 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060100 Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. GALACTIC DIFFUSE EMISSION 5 C NAKANO TOSHIO NULL NULL JAP 6 AO6 SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 XIS Y CTB109 NORTHEAST 345.764 59.0015 109.36320905 -0.98507066 252.0025 55910.0815393518 55910.7522106482 506039010 30405.8 30000 30405.8 30405.8 0 30405.8 2 2 0 2 1 0 0 30747.3 30747.3 57921.9 1 PROCESSED 55921.9730092593 56289 55921.9865277778 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060100 Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. GALACTIC DIFFUSE EMISSION 5 C NAKANO TOSHIO NULL NULL JAP 6 AO6 SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 XIS Y CTB109 SOUTHEAST 345.764 58.7015 109.24155205 -1.25930647 252.0022 55910.7526851852 55911.4007638889 506040010 30445.5 30000 30445.5 30445.5 0 30445.5 2 2 0 2 1 0 0 28751.1 28751.1 55987.9 1 PROCESSED 55921.9922337963 56289 55922.0080555556 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060100 Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. GALACTIC DIFFUSE EMISSION 5 C NAKANO TOSHIO NULL NULL JAP 6 AO6 SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 XIS Y VELA PWN NE1 129.3684 -44.9817 263.62243766 -2.36980886 142.6395 55916.6230439815 55917.0070601852 506041010 15408 15000 15424 15408 0 15424 1 1 0 1 1 0 0 11568.1 11568.1 33175.9 1 PROCESSED 55932.1421064815 56305 55937.7788310185 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN NE2 130.6211 -44.2844 263.6136326 -1.23809583 141.8635 55917.0080439815 55917.6126273148 506042010 18514 15000 18538 18514 0 18514 2 2 0 2 1 0 0 16875.5 16875.5 52225.9 0 PROCESSED 55932.1430324074 56305 55937.7869212963 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN NE3 131.0442 -44.0836 263.64329985 -0.87547181 123.9937 55895.188900463 55895.621724537 506043010 17799.9 15000 17806.6 17799.9 0 17806.6 2 2 0 2 1 0 0 13012 13012 37395.9 0 PROCESSED 55907.1515740741 56274 55907.1603703704 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E1 129.1398 -45.2732 263.75797839 -2.67419196 142.334 55916.0561226852 55916.622337963 506044010 17718 15000 17718 17718 0 17718 2 2 0 2 1 0 0 16628.4 16628.4 48895.9 0 PROCESSED 55932.1270023148 56305 55937.7696527778 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 C KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E2 129.5733 -45.3227 263.98172095 -2.46094632 304.5019 55711.9038773148 55712.1328935185 506045010 13904 15000 13920 13904 0 13920 1 1 0 1 1 0 0 8404 8404 19775.9 0 PROCESSED 55725.2488194444 56092 55725.2563888889 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E3 129.9962 -45.3672 264.19786494 -2.25193357 304.5033 55712.1335069444 55712.4099305556 506046010 14178.7 15000 14202.7 14194.7 0 14178.7 2 2 0 2 1 0 0 12659.9 12659.9 23875.9 0 PROCESSED 55725.9899421296 56093 55725.9978240741 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E4 130.4202 -45.4045 264.40968594 -2.03918199 304.5026 55712.4105902778 55712.7362268518 506047010 17031.4 15000 17035.4 17054.9 0 17031.4 2 2 0 2 1 0 0 15107.8 15107.8 28128 0 PROCESSED 55726.0201736111 56093 55726.0290046296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E5 130.8405 -45.4455 264.62375514 -1.83200273 304.5067 55712.7368402778 55712.9570601852 506048010 15919.6 15000 15919.6 15919.6 0 15943.6 1 1 0 1 1 0 0 11912.9 11912.9 19015.9 0 PROCESSED 55726.0552662037 56093 55726.0610185185 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E6 131.2685 -45.4809 264.83769354 -1.61837696 304.5065 55712.9576273148 55713.2292939815 506049010 18196.8 15000 18204.8 18196.8 0 18212.8 2 2 0 2 1 0 0 14209 14209 23469.9 0 PROCESSED 55735.9309143518 56103 55735.9387268518 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y VELA PWN E7 131.6969 -45.5129 265.05012769 -1.40367097 303.5042 55713.2300925926 55713.4688310185 506050010 13045.4 15000 13049.4 13045.4 0 13053.4 1 1 0 1 1 0 0 11075.1 11075.1 20622 0 PROCESSED 55726.0940509259 56093 55726.0999768518 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061302 Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. GALACTIC DIFFUSE EMISSION 5 B KATSUDA SATORU NULL NULL USA 6 AO6 THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA XIS Y G18.8+0.3 275.9435 -12.3781 18.78460262 0.39706413 83.4994 55994.9180324074 55996.1598958333 506051010 52020.5 50000 52020.5 52028.5 0 52036.5 2 2 0 2 1 0 0 44882 44882 107263.9 1 PROCESSED 56016.5156712963 56382 56016.6717708333 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061311 We propose a 50 ks exploratory observation of an interesting first-quadrant supernova remnant, G18.8+0.3, for which radio-continuum and CO data indicate interaction with a molecular cloud. Prior X-ray studies are limited to a 14 ks ROSAT PSPC observation producing about 500 counts. We expect about 12,000 counts with Suzaku, which should permit basic characterization of the spectrum and morphology of X-rays: shell-type, mixed-morphology (central thermal emission) or even composite (central PWN). Spectral analysis will allow us to determine or estimate shock speed, age, ambient density, and swept-up mass. As more middle-aged remnants are found to have unusual properties such as GeV-TeV emission, the study of objects like G18.8+0.3 assumes greater importance. GALACTIC DIFFUSE EMISSION 5 C REYNOLDS STEPHEN NULL NULL USA 6 AO6 G18.8+0.3: A SUPERNOVA REMNANT WITH STRONG MOLECULAR INTERACTION XIS Y G352.7-0.1 261.9227 -35.1119 352.75195989 -0.12120729 94.0335 55988.8605671296 55993.5536111111 506052010 201547.4 200000 201547.4 201547.4 0 201547.4 2 2 0 2 1 0 0 171544 171544 405439.6 4 PROCESSED 56008.353287037 56375 56008.397337963 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061315 Supernova remnants showing strong Fe K emission are relatively rare, and primarily of Type Ia. We propose a long observation of one of the least well-studied Fe-rich Galactic SNRs, G352.7-0.1, with the goal of characterizing the Fe emission, confirming its likely identification as the remnant of a Type Ia supernova, and constraining the properties of ejected material and the dynamics of the explosion. Its thermal X-ray spectrum is strikingly similar to Tycho's SNR, but unexpectedly X-rays are uniformly distributed throughout the remnant. Our proposed observation will produce high-quality spectra, adequate for detailed studies with some spatial information, that will greatly aid in understanding of this very interesting young remnant. GALACTIC DIFFUSE EMISSION 5 C BORKOWSKI KAZIMIERZ NULL NULL USA 6 AO6 STRONG IRON EMISSION IN THE SUPERNOVA REMNANT G352.7-0.1 XIS Y MONOGEM RING W1 100.4191 15.2834 198.20484712 4.79777248 269.9998 55998.5603356482 56000.0002314815 506053010 61126.6 60000 61126.7 61126.6 0 61126.6 3 2 0 2 1 0 0 59074 59074 124373.9 1 PROCESSED 56016.5296875 56382 56016.6737152778 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061316 We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. GALACTIC DIFFUSE EMISSION 5 C PLUCINSKY PAUL NULL NULL USA 6 AO6 STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING XIS Y MONOGEM RING W2 97.483 17.0349 195.35325463 3.08684005 270 56001.1430439815 56002.5487384259 506054010 62593.3 60000 62593.3 62593.3 0 62593.3 2 2 0 2 1 0 0 59966.9 59966.9 121443.9 1 PROCESSED 56019.3119212963 56385 56019.3467592593 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061316 We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. GALACTIC DIFFUSE EMISSION 5 C PLUCINSKY PAUL NULL NULL USA 6 AO6 STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING XIS Y G236+38 ON 146.5345 0.5057 235.93345442 38.21375915 307.3884 55713.4761574074 55715.0002314815 506055010 69802.5 70000 69802.5 69802.5 0 69802.5 2 2 0 2 1 0 0 64348.8 64348.8 131674 0 PROCESSED 55748.6194907407 56127 55757.6954050926 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061321 Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. GALACTIC DIFFUSE EMISSION 5 B HENLEY DAVID NULL NULL USA 6 AO6 UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS XIS Y G236+38 OFF 149.4117 1.4719 237.07053965 41.11953464 293.1755 55719.6375462963 55721.2780092593 506056010 70813.5 70000 70821.5 70829.5 0 70813.5 2 2 0 2 1 0 0 64444.4 64444.4 141727.8 0 PROCESSED 55748.6644212963 56127 55757.6968518518 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061321 Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. GALACTIC DIFFUSE EMISSION 5 B HENLEY DAVID NULL NULL USA 6 AO6 UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS XIS Y VELAFRAGG TAIL 125.0448 -47.7009 264.09848727 -6.37839252 263.1844 55658.0366898148 55658.8565162037 506057010 49354.3 50000 49370.3 49354.3 0 49370.3 3 2 0 2 1 0 0 43958.1 43958.1 70825.9 1 PROCESSED 55673.1850578704 56043 55673.1976736111 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062021 The Vela supernova remnant (SNR) displays remarkable features which appear to be ejecta ``shrapnel'' visible beyond the main shell. One of these shrapnel (A) is distinct from the others in that its X-ray spectrum exhibits a high Si abundance, while the other shrapnel exhibit enhanced O, Ne, and Mg abundances. One unexplored ejecta shrapnel (G) is located on the opposite side of the remnant from shrapnel A, suggesting that the SN explosion may have resulted in a jet-counterjet Si-rich structure, reminiscent of Cas A. We propose to observe this shrapnel for the first time to determine if it is also Si-rich like shrapnel A. If this is the case, the Vela SNR may be the first direct evidence of a jet-induced SN explosion. GALACTIC DIFFUSE EMISSION 5 A BOCCHINO FABRIZIO NULL NULL EUR 6 AO6 ASYMMETRIC SN EXPLOSION IN VELA SNR XIS Y KES 79 283.1953 0.6959 33.70438491 0.01846016 73.5801 55674.9437152778 55676.4716782407 506059010 50897 50000 50897 50897 0 50897 2 2 0 2 1 0 0 40897.8 40897.8 131960 2 PROCESSED 55697.1247337963 55652 55697.1427083333 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y G272.2-3.2 136.7114 -52.1231 272.22308022 -3.18374401 297.1287 55709.5476041667 55711.9009490741 506060010 130078.2 150000 130086.2 130094.2 0 130078.2 2 2 0 2 1 0 0 121830.3 121830.3 203305.8 3 PROCESSED 55735.3244444444 55652 55735.3493171296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y G272.2-3.2 136.7067 -52.1223 272.22054405 -3.18534238 101.7643 55877.9477777778 55878.6272916667 506060020 25526.5 20000 25534.5 25534.5 0 25526.5 2 2 0 2 1 0 0 27028 27028 58706 0 PROCESSED 55895.0629398148 55652 55895.0737962963 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y G290.1-0.8 165.7447 -60.8884 290.11957377 -0.7436408 293.2659 55737.4551388889 55740.5883333333 506061010 110593.1 110000 110609.1 110593.1 0 110601.1 2 2 0 2 1 0 0 99359.6 99359.6 270659.6 4 PROCESSED 55775.3353819444 55652 55775.3693287037 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y G292.0+1.8 171.1489 -59.2723 292.03159099 1.74911685 309.5957 55764.9604050926 55765.6883449074 506062010 43659.2 40000 43659.2 43659.2 0 43659.2 2 2 0 2 1 0 0 40236.4 40236.4 62885.9 1 PROCESSED 55784.9994444444 55652 55785.0141782407 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y KES 27 237.1872 -53.7777 327.32071311 0.47884394 101.6269 55983.5400231482 55985.4633217593 506063010 109353.5 120000 109401.5 109353.5 0 109401.5 3 2 0 2 1 0 0 115332.1 115332.1 166148 4 PROCESSED 55995.1751157407 55652 55995.1904976852 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y G349.7+0.2 259.4954 -37.4452 349.72102569 0.17051597 282.4112 55833.4324537037 55838.1341898148 506064010 160402.4 160000 160426.4 160402.4 0 160434.4 2 2 0 2 1 0 0 144615.1 144615.1 404220 5 PROCESSED 55858.495162037 55652 55858.5356018518 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y G350.1-0.3 260.2697 -37.4549 350.06545974 -0.33871818 266.4234 55821.2580787037 55822.9126388889 506065010 70181.3 70000 70197.3 70181.3 0 70197.3 2 2 0 2 1 0 0 60070.4 60070.4 142915.9 0 PROCESSED 55865.2526157407 55652 55865.2679282407 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y FERMI_BUBBLE_N1 234.25 5.09039 11.25503987 44.87092967 -99 NULL NULL 507001010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N2 234.40492 4.13061 10.26350243 44.20344481 -99 NULL NULL 507002010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N3 234.03421 6.09761 12.27959639 45.60588507 -99 NULL NULL 507003010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N4 233.83392 7.08661 13.32153532 46.30806269 -99 NULL NULL 507004010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N5 233.62292 8.0795 14.3878526 47.01092149 -99 NULL NULL 507005010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N6 233.40071 9.07639 15.48003007 47.71435161 -99 NULL NULL 507006010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N7 234.5505 3.17431 9.29114556 43.53691258 -99 NULL NULL 507007010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_N8 234.71308 2.19961 8.33368291 42.83756382 -99 NULL NULL 507008010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS N FERMI_BUBBLE_S1 329.068 -46.6182 351.41726681 -50.59485428 44.0071 56034.6949884259 56035.2070717593 507009010 25314.9 20000 25314.9 25322.9 0 25322.9 2 2 0 2 1 0 0 24797.3 24797.3 44239.9 0 PROCESSED 56049.2044791667 88068 56049.2134722222 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS Y FERMI_BUBBLE_S2 330.2693 -46.4894 351.28666586 -51.42688059 44.0074 56035.2081018518 56035.6736921296 507010010 20349.6 20000 20357.6 20349.6 0 20364.8 2 2 0 2 1 0 0 14278 14278 40213.9 0 PROCESSED 56049.1777546296 88068 56049.1880555556 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS Y FERMI_BUBBLE_S3 327.8758 -46.7423 351.52788223 -49.77060768 44.0052 56035.6752777778 56036.133587963 507011010 21233.6 20000 21233.6 21233.6 0 21233.6 2 2 0 2 1 0 0 20914 20914 39596 0 PROCESSED 56049.189525463 88068 56049.1986458333 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS Y FERMI_BUBBLE_S4 331.4735 -46.34789 351.14878111 -52.26468367 -99 NULL NULL 507012010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS Y FERMI_BUBBLE_S5 332.6607 -46.1905 351.01438321 -53.09632639 44.0062 56036.5915625 56037.1140972222 507013010 21004.4 20000 21012.4 21020.4 0 21004.4 2 2 0 2 1 0 0 20885.4 20885.4 45109.9 0 PROCESSED 56049.2513541667 88068 56049.260787037 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS Y FERMI_BUBBLE_S6 326.677 -46.8481 351.64382858 -48.94656928 44.0056 56037.1166087963 56037.6009027778 507014010 19643.9 20000 19651.9 19643.9 0 19659.9 1 1 0 1 1 0 0 14182.7 14182.7 41839.9 1 PROCESSED 56054.1759259259 88068 56054.1845833333 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070006 Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. GALACTIC DIFFUSE EMISSION 5 A KATAOKA JUN NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER XIS Y IC 443 94.3 22.75 188.89323884 3.10563666 -99 NULL NULL 507015010 -99 400000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 070015 The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 7 AO7 DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- XIS N RADIO_ARC_SOUTH 266.98267 -29.06742 0.15000074 -0.49998916 -99 NULL NULL 507016010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070016 The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. GALACTIC DIFFUSE EMISSION 5 A RYU SYUKYO NULL NULL JAP 7 AO7 X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- XIS N RADIO_ARC_S_E 267.18904 -28.76767 0.49998604 -0.49999554 -99 NULL NULL 507017010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070016 The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. GALACTIC DIFFUSE EMISSION 5 A RYU SYUKYO NULL NULL JAP 7 AO7 X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- XIS N RADIO_ARC_S_W 266.775 -29.36667 359.80012776 -0.49979732 -99 NULL NULL 507018010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070016 The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. GALACTIC DIFFUSE EMISSION 5 A RYU SYUKYO NULL NULL JAP 7 AO7 X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- XIS N HESS J1356-645 1 209.4375 -64.5 309.99457331 -2.54139966 -99 NULL NULL 507019010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070017 Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission. GALACTIC DIFFUSE EMISSION 5 C FUJINAGA TAKAHISA NULL NULL JAP 7 AO7 OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 XIS N HESS J1356-645 2 208.8125 -64.5 309.73376551 -2.47426316 -99 NULL NULL 507020010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070017 Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission. GALACTIC DIFFUSE EMISSION 5 C FUJINAGA TAKAHISA NULL NULL JAP 7 AO7 OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 XIS N W43_CENTER 281.90417 -1.95111 30.75993479 -0.03981951 -99 NULL NULL 507021010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070032 The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose the deep observation of gamma-ray bright star-forming region W43 by Suzaku. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. GALACTIC DIFFUSE EMISSION 5 C MIZUNO TSUNEFUMI NULL NULL JAP 7 AO7 SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN GAMMA-RAY BRIGHT STAR-FORMING REGION W43 XIS N W43_BGD1 281.67083 -2.40472 30.24990485 -0.03931367 -99 NULL NULL 507022010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070032 The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose the deep observation of gamma-ray bright star-forming region W43 by Suzaku. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. GALACTIC DIFFUSE EMISSION 5 C MIZUNO TSUNEFUMI NULL NULL JAP 7 AO7 SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN GAMMA-RAY BRIGHT STAR-FORMING REGION W43 XIS N HESSJ1507-622_CENTER 226.72 -62.35 317.94552085 -3.49393593 -99 NULL NULL 507025010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070033 HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator. GALACTIC DIFFUSE EMISSION 5 B TERADA YUKIKATSU MATSUMOTO HIRONORI JAP 7 AO7 SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE XIS N HESSJ1507-622_OFFSET 227.17167 -62.16847 318.21884024 -3.44175265 -99 NULL NULL 507026010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070033 HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator. GALACTIC DIFFUSE EMISSION 5 B TERADA YUKIKATSU MATSUMOTO HIRONORI JAP 7 AO7 SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE XIS N HESS J1457-593 224.441 -59.47719 318.35776917 -0.44305632 -99 NULL NULL 507027010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070037 We propose an X-ray observation of the putative SNR-molecular cloud interaction HESS J1457-593 with the Suzaku XIS detector for 30 ks. The aim of the observation is to clarify whether the TeV gamma-ray emission is of a leptonic or hadronic origin by searching for an X-ray counterpart to a level down to $10^{-14}$~erg cm$^{-2}$ s$^{-1}$. A non-detection of an X-ray nebula would strongly disfavor a leptonic origin of the TeV emission and add to the already strong multi-wavelength data which all suggests a hadronic origin of the emission. Since the spectrum of this unique source extends above many tens of TeV this would mean that we see, for the first time, evidence for hadronic cosmic rays being accelerated up to PeV energies. GALACTIC DIFFUSE EMISSION 5 B ODAKA HIROKAZU NULL NULL JAP 7 AO7 INVESTIGATING A PUTATIVE COSMIC-RAY PEVATRON WITH SUZAKU XIS N GC_SOUTH_1 268.09713 -29.47619 0.29762667 -1.54420019 -99 NULL NULL 507028010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070042 We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. GALACTIC DIFFUSE EMISSION 5 A NAKASHIMA SHINYA NULL NULL JAP 7 AO7 OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER XIS N GC_SOUTH_2 268.37325 -29.70717 0.22049449 -1.86832638 -99 NULL NULL 507029010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070042 We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. GALACTIC DIFFUSE EMISSION 5 A NAKASHIMA SHINYA NULL NULL JAP 7 AO7 OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER XIS N GC_SOUTH_3 268.17825 -29.20442 0.56768984 -1.46689773 -99 NULL NULL 507030010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070042 We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. GALACTIC DIFFUSE EMISSION 5 A NAKASHIMA SHINYA NULL NULL JAP 7 AO7 OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER XIS N GC_SOUTH_4 268.41292 -29.45 0.45982454 -1.76780045 -99 NULL NULL 507031010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070042 We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. GALACTIC DIFFUSE EMISSION 5 A NAKASHIMA SHINYA NULL NULL JAP 7 AO7 OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER XIS N ERIDANUS_ARCB_SPOT 53.31167 -9.68786 196.20015659 -48.09983113 -99 NULL NULL 507032010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070046 We propose Suzaku spectroscopic observations of the Edinanus Super Bubble, the nearest super bubble in our Galaxy. This is a good site to study the density, temperature, metalicity, and ionization status etc. at the rim of super bubbles which might be sources of the Galactic halo or fountains. A series of observations will reveal how the hot plasma is heated and expands as a bubble. GALACTIC DIFFUSE EMISSION 5 C YAMASAKI NORIKO NULL NULL JAP 7 AO7 SUZAKU OBSERVATION OF THE ERIDANUS SUPER BUBBLE XIS N G32.8-0.1 NORTH 282.8355 -0.0511 32.87550481 -0.00195799 74.4992 56037.6100347222 56038.7897685185 507035010 55147.5 50000 55147.5 55147.5 0 55147.5 3 2 0 2 1 0 0 53483.4 53483.4 101925.9 0 PROCESSED 56054.2235300926 88068 56054.2396990741 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070047 A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. GALACTIC DIFFUSE EMISSION 5 B BAMBA AYA NULL NULL JAP 7 AO7 SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS XIS Y G32.8-0.1 SOUTH 282.8163 -0.2514 32.68848527 -0.07620379 74.5004 56038.7902430556 56039.916087963 507036010 52232.4 50000 52240.4 52232.4 0 52248.4 2 2 0 2 1 0 0 50243.2 50243.2 97268 1 PROCESSED 56055.0094560185 88068 56055.0208564815 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 070047 A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. GALACTIC DIFFUSE EMISSION 5 B BAMBA AYA NULL NULL JAP 7 AO7 SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS XIS Y G298.6-0.0 183.4 -62.62 298.59719832 -0.06713649 -99 NULL NULL 507037010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070047 A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. GALACTIC DIFFUSE EMISSION 5 B BAMBA AYA NULL NULL JAP 7 AO7 SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS XIS N CAS A 350.85 58.815 111.7347425 -2.12956823 -99 NULL NULL 507038010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070050 We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. GALACTIC DIFFUSE EMISSION 5 C MAEDA YOSHITOMO NULL NULL JAP 7 AO7 MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A XIS N MSH15-56_SW 238.05279 -56.31619 326.1159236 -1.80991773 -99 NULL NULL 507039010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070055 The magnetic field upstream the shock front of the SN blast wave is the key parameter for discussing particle acceleration. In this study we try to constrain the upstream magnetic field and its amplification based on the ionization parameter of heated ISM just behind the shock. For this purpose, we propose a 100 ks XIS observation of an middle aged SNR MSH 15-56 with non-thermal filaments and an anomalously large ionization age for its dynamical age. GALACTIC DIFFUSE EMISSION 5 C YATSU YOICHI NULL NULL JAP 7 AO7 A STUDY OF PARTICLE ACCELERATION BASED ON THE THERMAL PLASMA BEHIND THE SHOCK XIS N CYG_COCOON 306.7875 40.94556 79.25012093 1.49980129 -99 NULL NULL 507040010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070060 The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. GALACTIC DIFFUSE EMISSION 5 C MIZUNO TSUNEFUMI NULL NULL JAP 7 AO7 SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X XIS N CYG_BGD1 306.6375 39.4925 78.00038033 0.7492866 -99 NULL NULL 507041010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070060 The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. GALACTIC DIFFUSE EMISSION 5 C MIZUNO TSUNEFUMI NULL NULL JAP 7 AO7 SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X XIS N CYG_BGD2 306.94167 42.39806 80.49931815 2.25094415 -99 NULL NULL 507042010 -99 25000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070060 The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. GALACTIC DIFFUSE EMISSION 5 C MIZUNO TSUNEFUMI NULL NULL JAP 7 AO7 SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X XIS N HESSJ1841 280.5 -5.83 26.66945273 -0.56535167 -99 NULL NULL 507043010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070063 HESSJ1841-055 is one of the largest and most complex unidentified HESS sources in the Galaxy. The search for counterparts up to this point has brought out the fact that a group of sources has to create the diffuse emission. Most of them are already covered in X-ray. However one of the peaks of HESSJ1841-055 does not have coverage by the current X-ray experiments: at this location the only plausible counterpart is a HMXB 1RXSJ184135.3-055032. Suzaku, thanks to the high sensitivity, can study in detail this source, reveal if it can explain the VHE emission peak and eventually detect additional diffuse emission. Moreover, if this part will be observed, HESSJ1841-055 will be completely covered by X-ray and gamma-ray experiments, allowing detailed studies on the nature of this source. GALACTIC DIFFUSE EMISSION 5 C MATSUMOTO HIRONORI NULL NULL JAP 7 AO7 HOW SUZAKU CAN HELP TO UNDERSTAND THE UNIDENTIFIED HESS SOURCE HESS J1841-055 XIS N (L,B)=(-20,0) 276.66675 -11.86572 19.56797982 0.01121005 -99 NULL NULL 507044010 -99 200000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070084 We will observe the region at (l,b)=(19.57, 0.0112) to measure spatial and temporal fluctuations of the Galactic Ridge X-ray Emission (GRXE). Measuring these fluctuations is a good test to check the scenarios of point sources and star flare for the GRXE origin. Combined with archival data of XMM-Newton, 200 ks observation of Suzaku makes us able to detect the fluctuations lager than 3% of the GRXE flux. The observation mode of XIS is planed to be a normal clocking mode with no window option. GALACTIC DIFFUSE EMISSION 5 B UCHIYAMA HIDEKI NULL NULL JAP 7 AO7 SUZAKU STUDY OF SPATIAL AND TEMPORAL FLUCTUATIONS IN THE GALACTIC RIDGE X-RAY EMISSION XIS N HC40_NORTH 293.3125 19.23333 54.72702122 -0.12886137 -99 NULL NULL 507045010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070087 We propose the measurement of the non-thermal radiation from the relativistic electrons accelerated in the supernova remnant HC40 by a Suzaku observation. It is located in a stellar wind cavity with very low density. In such an environment, very efficient acceleration can be operated. We found the possible non-thermal hard X-ray emission and GeV emission from the northern part of it. HC40 is a relatively young SNR and it has started to interact with the molecular clouds. Therefore, we can expect to obtain the spectrum of the pure accelerated particles through the gamma-ray spectrum using the molecular clouds as a tracer. We aim to constrain the maximum energy of the accelerated protons by determination of the electron spectrum with the multi-wavelength modeling. GALACTIC DIFFUSE EMISSION 5 C HANABATA YOSHITAKA NULL NULL JAP 7 AO7 STUDYING THE SUPERNOVA REMNANT HC40 IN A STELLAR WIND CAVITY XIS N HC40_WEST 293.0625 19.08333 54.48160122 0.00544313 -99 NULL NULL 507046010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070087 We propose the measurement of the non-thermal radiation from the relativistic electrons accelerated in the supernova remnant HC40 by a Suzaku observation. It is located in a stellar wind cavity with very low density. In such an environment, very efficient acceleration can be operated. We found the possible non-thermal hard X-ray emission and GeV emission from the northern part of it. HC40 is a relatively young SNR and it has started to interact with the molecular clouds. Therefore, we can expect to obtain the spectrum of the pure accelerated particles through the gamma-ray spectrum using the molecular clouds as a tracer. We aim to constrain the maximum energy of the accelerated protons by determination of the electron spectrum with the multi-wavelength modeling. GALACTIC DIFFUSE EMISSION 5 C HANABATA YOSHITAKA NULL NULL JAP 7 AO7 STUDYING THE SUPERNOVA REMNANT HC40 IN A STELLAR WIND CAVITY XIS N HC40_BGD 293.4875 19.79694 55.30002681 -0.00029805 -99 NULL NULL 507047010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070087 We propose the measurement of the non-thermal radiation from the relativistic electrons accelerated in the supernova remnant HC40 by a Suzaku observation. It is located in a stellar wind cavity with very low density. In such an environment, very efficient acceleration can be operated. We found the possible non-thermal hard X-ray emission and GeV emission from the northern part of it. HC40 is a relatively young SNR and it has started to interact with the molecular clouds. Therefore, we can expect to obtain the spectrum of the pure accelerated particles through the gamma-ray spectrum using the molecular clouds as a tracer. We aim to constrain the maximum energy of the accelerated protons by determination of the electron spectrum with the multi-wavelength modeling. GALACTIC DIFFUSE EMISSION 5 C HANABATA YOSHITAKA NULL NULL JAP 7 AO7 STUDYING THE SUPERNOVA REMNANT HC40 IN A STELLAR WIND CAVITY XIS N VELA PWN N1 128.83267 -44.93833 263.3595943 -2.6466298 -99 NULL NULL 507048010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070103 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 7 AO7 HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? XIS N VELA PWN N2 128.83196 -44.64144 263.12127605 -2.46925588 -99 NULL NULL 507049010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070103 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 7 AO7 HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? XIS N VELA PWN N3 128.83125 -44.34458 262.88304238 -2.29186141 -99 NULL NULL 507050010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070103 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 7 AO7 HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? XIS N VELA PWN N4 128.83054 -44.04775 262.6448887 -2.11444946 -99 NULL NULL 507051010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070103 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 7 AO7 HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? XIS N VELA PWN N5 128.82983 -43.75097 262.40682646 -1.93703508 -99 NULL NULL 507052010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070103 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 7 AO7 HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? XIS N VELA PWN N6 128.82913 -43.45428 262.16888747 -1.7596395 -99 NULL NULL 507053010 -99 15000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070103 We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. GALACTIC DIFFUSE EMISSION 5 C MORI KOJI NULL NULL JAP 7 AO7 HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? XIS N G359.0-0.9 266.74696 -30.20564 359.07000619 -0.91388522 -99 NULL NULL 507054010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070108 From the launch of Fermi gamma-ray satellite in 2008, some of GeV-bright supernova remnants (SNRs) have been discovered, such as IC443, W49B. Recently, radiative recombination continua spectra were discovered from these SNRs by the Suzaku X-ray observation. Since there are no heavenly bodies which have such strange features except these SNRs, these features might have some causal relationships. All of them are Mixed-Morphology SNRs. Therefore, we propose observing the MM SNR G359.0-0.9 to understand the natures of the such MM SNRs. GALACTIC DIFFUSE EMISSION 5 C FUKUYAMA TARO NULL NULL JAP 7 AO7 EXPLORATION OF RECOMBINING PLASMA BY DEEP OBSERVATION OF MIXED-MORPHLOGY SUPERNOVA REMNANT G359.0-0.9 XIS N G18.8+0.3 275.99167 -12.38333 18.8020147 0.35304292 -99 NULL NULL 507055010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071315 We propose a 50 ks exploratory observation of an interesting first-quadrant supernova remnant, G18.8+0.3, for which radio-continuum and CO data indicate interaction with a molecular cloud. Prior X-ray studies are limited to a 14 ks ROSAT PSPC observation producing about 500 counts. We expect about 12,000 counts with Suzaku, which should permit basic characterization of the spectrum and morphology of X-rays: shell-type, mixed-morphology (central thermal emission) or even composite (central PWN). Spectral analysis will allow us to determine or estimate shock speed, age, ambient density, and swept-up mass. As more middle-aged remnants are found to have unusual properties such as GeV-TeV emission, the study of objects like G18.8+0.3 assumes greater importance. GALACTIC DIFFUSE EMISSION 5 C REYNOLDS STEPHEN NULL NULL USA 7 AO7 G18.8+0.3: A SUPERNOVA REMNANT WITH STRONG MOLECULAR INTERACTION XIS N SNR HB3 SE-A 35.59167 61.93333 133.40862698 0.92532929 -99 NULL NULL 507056010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071316 We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. GALACTIC DIFFUSE EMISSION 5 C KATSUTA JUNICHIRO NULL NULL USA 7 AO7 SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 XIS N SNR HB3 SE-B 35.75 62.2 133.38620556 1.20121191 -99 NULL NULL 507057010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071316 We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. GALACTIC DIFFUSE EMISSION 5 C KATSUTA JUNICHIRO NULL NULL USA 7 AO7 SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 XIS N SNR HB3 SE-C 36.025 62.46667 133.41304396 1.495656 -99 NULL NULL 507058010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071316 We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. GALACTIC DIFFUSE EMISSION 5 C KATSUTA JUNICHIRO NULL NULL USA 7 AO7 SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 XIS N G352.7-0.1 261.9 -35.09083 352.75914623 -0.09405569 -99 NULL NULL 507059010 -99 110000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071317 We propose a 110-ks observation of G352.7-0.1, a possible candidate of a Type Ia supernova remnant (SNR) categorized in the mixed-morphology (MM) class. So far, MM-SNRs have been considered to be associated with core-collapse supernova explosions. This observation will, therefore, provide an important suggestion that the formation mechanism of MM-SNRs is not related to progenitors nature but rather associated with their environment, if the SNR will be confirmed to have a Type Ia origin. Our primary objectives are clear detection of Fe-K emission and accurate measurement of its center energy to determine its origin (i.e., fluorescence or Fe-rich ejecta), which will help distinguish its progenitor type. We will also search for emission from low-abundance elements, such as Al, Cr, and Mn. GALACTIC DIFFUSE EMISSION 5 C YAMAGUCHI HIROYA NULL NULL USA 7 AO7 G352.7-0.1: CAN A TYPE IA SUPERNOVA FORM A MIXED-MORPHOLOGY REMNANT? XIS N FERMI BUBBLE 1 267.09229 -13.57681 13.53571404 7.35613343 -99 NULL NULL 507060010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071324 We propose to investigate the spectrum of X-ray emission from the edge of the recently discovered Galactic gamma-ray features known as the Fermi bubbles. The bubbles extend 50 degrees above and below the Galactic center, with a width of about 40 degrees in longitude. These structures could result from a large-scale accretion-driven outflow from the central black hole, or winds from a nuclear starburst. ROSAT X-ray maps (bands R6 and R7) show closely related features with a relatively hard spectrum. This spectrum may be thermal bremsstrahlung emission, may contain significant line emission, or may contain a non-thermal component. Dedicated Suzaku observations can constrain the different spectral components. GALACTIC DIFFUSE EMISSION 5 C SU MENG NULL NULL USA 7 AO7 PROBING THE FERMI BUBBLES WITH SUZAKU XIS N FERMI BUBBLE 2 267.00321 -13.44061 13.61028104 7.4996095 -99 NULL NULL 507061010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071324 We propose to investigate the spectrum of X-ray emission from the edge of the recently discovered Galactic gamma-ray features known as the Fermi bubbles. The bubbles extend 50 degrees above and below the Galactic center, with a width of about 40 degrees in longitude. These structures could result from a large-scale accretion-driven outflow from the central black hole, or winds from a nuclear starburst. ROSAT X-ray maps (bands R6 and R7) show closely related features with a relatively hard spectrum. This spectrum may be thermal bremsstrahlung emission, may contain significant line emission, or may contain a non-thermal component. Dedicated Suzaku observations can constrain the different spectral components. GALACTIC DIFFUSE EMISSION 5 C SU MENG NULL NULL USA 7 AO7 PROBING THE FERMI BUBBLES WITH SUZAKU XIS N FERMI BUBBLE 3 266.87392 -13.21 13.74714891 7.72456462 -99 NULL NULL 507062010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071324 We propose to investigate the spectrum of X-ray emission from the edge of the recently discovered Galactic gamma-ray features known as the Fermi bubbles. The bubbles extend 50 degrees above and below the Galactic center, with a width of about 40 degrees in longitude. These structures could result from a large-scale accretion-driven outflow from the central black hole, or winds from a nuclear starburst. ROSAT X-ray maps (bands R6 and R7) show closely related features with a relatively hard spectrum. This spectrum may be thermal bremsstrahlung emission, may contain significant line emission, or may contain a non-thermal component. Dedicated Suzaku observations can constrain the different spectral components. GALACTIC DIFFUSE EMISSION 5 C SU MENG NULL NULL USA 7 AO7 PROBING THE FERMI BUBBLES WITH SUZAKU XIS N FERMI BUBBLE 4 266.74458 -12.93739 13.92057306 7.97088526 -99 NULL NULL 507063010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071324 We propose to investigate the spectrum of X-ray emission from the edge of the recently discovered Galactic gamma-ray features known as the Fermi bubbles. The bubbles extend 50 degrees above and below the Galactic center, with a width of about 40 degrees in longitude. These structures could result from a large-scale accretion-driven outflow from the central black hole, or winds from a nuclear starburst. ROSAT X-ray maps (bands R6 and R7) show closely related features with a relatively hard spectrum. This spectrum may be thermal bremsstrahlung emission, may contain significant line emission, or may contain a non-thermal component. Dedicated Suzaku observations can constrain the different spectral components. GALACTIC DIFFUSE EMISSION 5 C SU MENG NULL NULL USA 7 AO7 PROBING THE FERMI BUBBLES WITH SUZAKU XIS N G299.5-0.6 184.7875 -63.16194 299.29711498 -0.51828518 -99 NULL NULL 507064010 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A PRINZ TOBIAS NULL NULL EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS N G7.6+2.0 268.79583 -21.39 7.58954998 2.00957075 -99 NULL NULL 507065010 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A PRINZ TOBIAS NULL NULL EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS N G276.2-7.7 135.44167 -58.09639 276.22935228 -7.69002952 -99 NULL NULL 507066010 -99 10000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A PRINZ TOBIAS NULL NULL EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS N G278.0+12.4 158.15 -43.70194 278.00851851 12.34946517 -99 NULL NULL 507067010 -99 17500 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072014 We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. GALACTIC DIFFUSE EMISSION 5 A PRINZ TOBIAS NULL NULL EUR 7 AO7 IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS XIS N G337.2-0.7 249.97917 -47.83333 337.25131481 -0.7810479 -99 NULL NULL 507068010 -99 300000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KOYAMA KATSUJI NULL NULL JAP 7 Ao7 NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS N GRXE_E_2 267.62113 -27.24761 2.00000073 -0.04599482 -99 NULL NULL 507069010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N GRXE_E_3 267.76496 -27.03286 2.25000042 -0.04598925 -99 NULL NULL 507070010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N GRXE_E_4 267.90825 -26.81797 2.4999995 -0.04599279 -99 NULL NULL 507071010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N GRXE_E_5 268.051 -26.60294 2.74999651 -0.0459993 -99 NULL NULL 507072010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N GRXE_E_6 268.19321 -26.38775 3.00000722 -0.04599246 -99 NULL NULL 507073010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N GRXE_E_9 268.08637 -26.15686 3.14999102 0.15399099 -99 NULL NULL 507074010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N GRXE_E_10 267.90375 -25.94333 3.25001105 0.40400991 -99 NULL NULL 507075010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TSURU TAKESHI NULL NULL JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS N MBM16 49.76708 11.58111 170.60308837 -37.27275129 -99 NULL NULL 507076010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A GALEAZZI MASSIMILIANO NULL NULL USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS N MBM16 49.76708 11.58111 170.60308837 -37.27275129 -99 NULL NULL 507076020 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A GALEAZZI MASSIMILIANO NULL NULL USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS N MBM36 238.36042 -4.78528 4.00973864 35.70253576 -99 NULL NULL 507077010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A GALEAZZI MASSIMILIANO NULL NULL USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS N LDN1563 75.525 13.86667 187.15073338 -16.70689044 -99 NULL NULL 507078010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A GALEAZZI MASSIMILIANO NULL NULL USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS N MBM20 68.94 -14.62722 211.40116988 -36.56186667 -99 NULL NULL 507079010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A GALEAZZI MASSIMILIANO NULL NULL USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS N 3C120 68.2984 5.3555 190.37315865 -27.39441526 237.4585 53775.1527199074 53776.2433217593 700001010 41932.1 160000 41932.1 41932.1 41932.1 41932.1 2 2 2 2 1 0 0 34094.1 34094.1 94221.9 1 PROCESSED 54324.7308680556 54247 53906.2470601852 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001003 Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 0 SWG BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES XIS N 3C120 68.298 5.3556 190.3728125 -27.39468757 237.4583 53782.5602199074 53783.5876967593 700001020 41554.5 160000 41554.5 41554.5 41554.5 41554.5 2 2 2 2 1 0 0 36846.1 36846.1 88772 2 PROCESSED 54405.6820601852 54247 54041.2956365741 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001003 Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 0 SWG BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES XIS N 3C120 68.2993 5.3535 190.3755878 -27.39480435 262.4873 53789.4598726852 53790.8748958333 700001030 40907.3 160000 40907.3 40907.3 40907.3 40907.3 2 2 2 2 1 0 0 38481.7 38481.7 77876 2 PROCESSED 54322.9678009259 54247 54041.5149189815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001003 Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 0 SWG BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES XIS N 3C120 68.2979 5.3541 190.37414386 -27.39561637 262.5053 53796.9456828704 53797.8606365741 700001040 40905.1 160000 40913.1 40921.1 40921.1 40905.1 2 2 2 2 1 0 0 40311.8 40311.8 79045.9 0 PROCESSED 54327.1246990741 54247 54041.627025463 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001003 Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 0 SWG BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES XIS N MCG -5-23-16 146.9445 -30.9023 262.72964912 17.28396386 118.3849 53711.9526388889 53714.4939699074 700002010 95677.4 100000 95677.4 95717.4 95717.4 95685.4 2 2 2 2 1 0 0 85564.7 85564.7 219525.1 3 PROCESSED 54405.5569212963 54247 54039.1988310185 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001006 We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off. EXTRAGALACTIC COMPACT SOURCES 7 A REEVES JAMES NULL NULL JAP 0 SWG PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA HXD N NGC 4051 180.8556 44.5807 148.68917976 70.06918189 135.3482 53684.8015509259 53687.4315277778 700004010 119578 150000 119610 119610 119586 119578 2 2 2 2 1 0 0 120004.7 120004.7 227191.8 3 PROCESSED 54331.2897569444 54247 54037.5713078704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001012 We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 0 SWG THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM HXD N NGC 2992 146.4352 -14.2714 249.66741784 28.82528499 102.6298 53680.5956481482 53681.5850925926 700005010 37502.9 120000 37502.9 38756.8 37518 37715 2 2 2 2 1 0 0 32073 32073 85485.9 1 PROCESSED 54323.9501157407 54247 54037.5593518518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001013 NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 0 SWG THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING XIS N NGC 2992 146.4207 -14.2696 249.65504756 28.81616071 88.7924 53693.8781597222 53694.9759722222 700005020 37493.5 120000 37656.5 39691.5 37493.5 37820.5 1 1 1 1 1 0 0 33899.1 33899.1 94847.9 1 PROCESSED 54324.1513657407 54247 54037.7316087963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001013 NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 0 SWG THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING HXD N NGC 2992 146.4592 -14.2821 249.69438343 28.83515423 128.4959 53717.4275462963 53718.506412037 700005030 46836.1 120000 46844.1 46868.1 46836.1 46860.1 2 2 2 2 1 0 0 44298.3 44298.3 93207.9 1 PROCESSED 54327.737974537 54247 54039.2254861111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001013 NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 0 SWG THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING HXD N ARP220 233.7664 23.5658 36.73879852 53.01919685 114.8377 53742.3490856482 53744.9654398148 700006010 98550.6 100000 98558.6 98550.6 98558.6 98558.6 2 2 2 2 1 0 0 93362.3 93362.3 226041.9 2 PROCESSED 54330.7553125 54247 54040.0356597222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001033 We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation. EXTRAGALACTIC COMPACT SOURCES 7 A IWASAWA KAZUSHI NULL NULL JAP 0 SWG HARD X-RAY EMISSION FROM THE NEAREST ULTRALUMINOUS INFRARED GALAXY ARP220 HXD N MCG-6-30-15 203.9706 -34.2946 313.28931603 27.68170589 107.0204 53744.9738310185 53749.1390277778 700007010 143196.5 300000 143196.5 143316.2 143268.5 143244.5 2 2 2 2 1 0 0 126290.3 126290.3 359839.9 4 PROCESSED 54332.0573958333 54247 54040.4060416667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001035 The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . EXTRAGALACTIC COMPACT SOURCES 7 A FABIAN ANDREW NULL NULL JAP 0 SWG REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 XIS N MCG-6-30-15 203.9717 -34.2976 313.28966663 27.67858669 102.4356 53758.5062962963 53761.0835648148 700007020 98483.4 300000 98483.4 98483.4 98483.4 98483.4 2 2 2 2 1 0 0 81892.2 81892.2 222649.7 3 PROCESSED 54405.6241203704 54247 54059.5463773148 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001035 The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . EXTRAGALACTIC COMPACT SOURCES 7 A FABIAN ANDREW NULL NULL JAP 0 SWG REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 XIS N MCG-6-30-15 203.9713 -34.2978 313.28925681 27.67845448 102.4359 53762.928275463 53765.368275463 700007030 96691.9 300000 96691.9 96691.9 96699.9 96699.9 2 2 2 2 1 0 0 89819.4 89819.4 210801.9 5 PROCESSED 54405.682962963 54247 54040.8156828704 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001035 The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . EXTRAGALACTIC COMPACT SOURCES 7 A FABIAN ANDREW NULL NULL JAP 0 SWG REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 XIS N 1H 0707-495 107.1586 -49.5558 260.16951247 -17.68246857 144.7199 53707.1759143518 53710.0974537037 700008010 97229.1 100000 97852.9 100389.1 97229.1 97814.9 4 2 4 4 1 0 0 91800.8 91800.8 252368.8 4 PROCESSED 54405.5865625 54247 54059.7078472222 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001040 We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. EXTRAGALACTIC COMPACT SOURCES 7 A MINIUTTI GIOVANNI NULL NULL JAP 0 SWG THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495 XIS N PG 1211+143 183.6045 14.1097 267.53559231 74.37841457 120.7913 53698.7348263889 53701.3397453704 700009010 96324.1 100000 96590 97580.2 96324.1 96324.1 3 2 3 3 1 0 0 84008.7 84008.7 225043.8 2 PROCESSED 54331.6772222222 54247 54038.7422106482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001041 A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band. EXTRAGALACTIC COMPACT SOURCES 7 A REEVES JAMES NULL NULL JAP 0 SWG EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143 HXD N 0836+714 130.267 70.829 143.62710847 34.4182022 294.8268 53809.7578125 53810.5836111111 700010010 55626.1 50000 55634.1 55634.1 55626.1 55634.1 2 2 2 2 1 0 0 47405.8 47405.8 71341.9 1 PROCESSED 54327.0498611111 54247 54041.9651851852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001061 We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales. EXTRAGALACTIC COMPACT SOURCES 7 A MADEJSKI GREG NULL NULL JAP 0 SWG TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS HXD N SWIFT J0746.3+2548 116.6142 25.8792 194.5201067 22.91801121 97.0095 53678.357974537 53680.5862847222 700011010 99428.4 100000 99523.5 100452.4 99428.4 99723.5 2 2 2 2 1 0 0 87699.5 87699.5 192472 4 PROCESSED 54330.3416435185 54247 54037.5799074074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001087 Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution. EXTRAGALACTIC COMPACT SOURCES 7 A TAKAHASHI TADAYUKI NULL NULL JAP 0 SWG SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT NULL N PKS2155-304 329.7191 -30.2247 17.73226544 -52.24760927 254.1358 53704.7749884259 53706.3613888889 700012010 63911.4 80000 63919.4 63911.4 63919.4 63916.6 2 2 2 2 1 0 0 58011.4 58011.4 137049.8 3 PROCESSED 54329.7850694444 54247 54038.8920138889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001100 Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates. EXTRAGALACTIC COMPACT SOURCES 7 A TAKAHASHI TADAYUKI NULL NULL JAP 0 SWG-TOO RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS XIS N NGC4418 186.7074 -0.9383 290.03230216 61.31559989 292.8039 53929.4791898148 53931.280775463 701001010 68348.5 70000 68348.5 68348.5 68348.5 68348.5 2 2 2 2 1 0 0 57110.3 57110.3 155634 1 PROCESSED 54328.0029166667 54408 53942.4601388889 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010001 We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. EXTRAGALACTIC COMPACT SOURCES 7 A IMANISHI MASATOSHI NULL NULL JAP 1 AO1 COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES HXD N UGC5101 143.841 61.3185 152.55229096 42.85621781 331.581 53825.1798148148 53826.3509722222 701002010 48990.2 70000 48990.2 48990.2 48990.2 48990.2 2 2 2 2 1 0 0 43974.8 43974.8 101177.9 0 PROCESSED 54324.2409722222 54735 53905.890625 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010001 We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. EXTRAGALACTIC COMPACT SOURCES 7 A IMANISHI MASATOSHI NULL NULL JAP 1 AO1 COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES HXD N UGC5101 144.0189 61.4178 152.38145034 42.89433298 112.6892 54039.7635300926 54040.396087963 701002020 42166 35000 42166 42174 42182 42182 2 2 2 2 1 0 0 33558.9 33558.9 54651.9 0 PROCESSED 54322.6373726852 54735 54063.3945949074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010001 We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. EXTRAGALACTIC COMPACT SOURCES 7 A IMANISHI MASATOSHI NULL NULL JAP 1 AO1 COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES HXD Y IRAS13224-3809 201.327 -38.416 310.18598264 23.97820794 118.5234 54126.2420601852 54131.0849421296 701003010 197937.6 200000 197953.6 197937.6 0 197951.6 2 2 0 2 1 0 0 169652.6 169652.6 418397.8 4 PROCESSED 54406.0383680556 54777 54139.7293287037 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010028 We propose a 200 ks continuous observation of the narrow-line Seyfert 1 galaxy IRAS13224-3809 in order to understand its remarkable and puzzling spectral and variability properties. Suzaku data will enable us to disentangle the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. If the latter then the appearance of the source is controlled by general relativistic effects. In addition, the ability for Suzaku to conduct long continuous observations will allow us to monitor IRAS13224-3809 for giant amplitude flaring (as seen with ROSAT); therefore enabling us to enhance our understanding of AGN variability. EXTRAGALACTIC COMPACT SOURCES 7 B TANAKA YASUO NULL NULL JAP 1 AO1 THE REMARKABLE NARROW LINE SEYFERT 1 GALAXY IRAS13224-3809 XIS Y SDSSJ084234.9+362503 130.6534 36.3531 186.36195466 37.19411123 266.2333 53868.6856018518 53871.41625 701004010 109955.6 120000 109971.6 109963.6 109955.6 109963.6 2 2 2 2 1 0 0 127230.6 127230.6 235894.8 1 PROCESSED 54405.8024189815 54400 53920.287650463 2.1.6.15 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010036 Type 2 QSOs are one of the key class to understand the structure and evolution of AGN, origin of the Cosmic X-ray background, and the history of black hole growth. We propose to measure a hard X-ray spectrum of the most luminous and brightest type 2 QSO candidate in the Sloan Digital Sky Survey. The selection by optical narrow line spectra is not biased toward Compton-thin AGNs and enables us to investigate the true nature of type 2 QSOs. The data will be used to measure the absorption column density, intrinsic luminosity, and to constrain the structure of the absorber. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 1 AO1 THE MOST LUMINOUS TYPE 2 QSO IN SDSS HXD N NGC 4968 196.7464 -23.7282 307.51234678 39.00523278 298.8345 53954.7307523148 53955.6822222222 701005010 39050.8 40000 39050.8 39050.8 39050.8 39050.8 2 2 2 2 1 0 0 35617 35617 82197.9 1 PROCESSED 54323.6258101852 54408 54020.7898148148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010037 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 1 AO1 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD N NGC 1667 72.1445 -6.2644 203.99435404 -30.10712566 81.9813 53964.3614814815 53965.2536805556 701006010 39253 40000 39253 39261 39261 39261 2 2 2 2 1 0 0 35728.1 35728.1 77075.9 0 PROCESSED 54323.3851157407 54526 54020.7803009259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010037 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 1 AO1 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD N MRK 1073 48.7401 42.0969 149.47083071 -13.26071681 81.0781 53949.235162037 53949.3834722222 701007010 3474.6 40000 3474.6 3480.6 3478.6 3476.6 1 1 1 1 1 0 0 4135.8 4135.8 12806 0 PROCESSED 54320.6285532407 54735 54132.9684490741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010037 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 1 AO1 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD N MRK 1073 48.7759 41.9723 149.56255257 -13.3516285 258.3737 54135.7651851852 54136.6641087963 701007020 39511.1 40000 39519.1 39511.1 0 39519.1 2 2 0 2 1 0 0 37181.4 37181.4 77651.9 0 PROCESSED 54322.8057291667 54735 54151.4969444445 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010037 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 1 AO1 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD Y IRASF11223-1244 171.2239 -12.9662 272.54538498 44.73919633 107.3062 54064.7275347222 54065.5709953704 701008010 40941.5 40000 41101.5 40941.5 0 41109.5 1 1 0 1 1 0 0 37680.4 37680.4 72863.9 1 PROCESSED 54322.6747916667 54735 54088.8556828704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010038 The source of huge energy output from ultraluminous infrared galaxies (ULIRGs) is still under debate. We propose to search for a hidden QSO as the energy source by observing ULIRGs with high luminosity optical emission lines classified as a Seyfert 2. The data will be used to constrain the power of the central AGN and to study the nature of infrared selected type 2 QSOs. EXTRAGALACTIC COMPACT SOURCES 7 C TERASHIMA YUICHI NULL NULL JAP 1 AO1 A SEARCH FOR HIDDEN QSO IN ULTRALUMINOUS INFRARED GALAXIES HXD Y PKS 0558-504 89.9338 -50.4417 257.95388656 -28.57696937 207.8266 54117.4686226852 54118.1127777778 701011010 20620.7 20000 20620.7 20620.7 0 20620.7 2 2 0 2 1 0 0 18914 18914 55647.9 0 PROCESSED 54323.357025463 54735 54133.0355787037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010057 Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 C HABA YOSHITO NULL NULL JAP 1 AO1 SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 XIS Y PKS 0558-504 89.9338 -50.4409 257.95298672 -28.57684464 209.1054 54118.6998032407 54119.2654976852 701011020 18875.3 20000 18875.3 18875.3 0 18875.3 2 2 0 2 1 0 0 18049.7 18049.7 48870 1 PROCESSED 54323.3504050926 54735 54133.3967361111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010057 Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 C HABA YOSHITO NULL NULL JAP 1 AO1 SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 XIS Y PKS 0558-504 89.9334 -50.4402 257.95215413 -28.57698713 210.2147 54119.7661805556 54120.3203009259 701011030 21256.3 20000 21256.3 21256.3 0 21256.3 2 2 0 2 1 0 0 19114.5 19114.5 47870 0 PROCESSED 54323.3215393518 54735 54133.3934259259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010057 Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 C HABA YOSHITO NULL NULL JAP 1 AO1 SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 XIS Y PKS 0558-504 89.9324 -50.4401 257.95192858 -28.57760064 211.3321 54120.8400925926 54121.3279976852 701011040 19738.1 20000 19754.1 19738.1 0 19754.1 1 1 0 1 1 0 0 17175 17175 42135.9 0 PROCESSED 54320.8041319444 54735 54137.1036921296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010057 Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 C HABA YOSHITO NULL NULL JAP 1 AO1 SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 XIS Y PKS 0558-504 89.9335 -50.4395 257.95137808 -28.57681508 212.4401 54121.9091203704 54122.3529976852 701011050 19515.4 20000 19531.4 19515.4 0 19531.4 1 1 0 1 1 0 0 16123.6 16123.6 38312 0 PROCESSED 54323.275 54735 54137.0453240741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010057 Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 C HABA YOSHITO NULL NULL JAP 1 AO1 SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 XIS Y KAZ 102 270.6661 67.6374 97.62313354 29.55178422 2.066 53895.6833101852 53896.5343055556 701012010 41454 40000 41454 41462 41470 41470 2 2 2 2 1 0 0 40950.7 40950.7 73519.9 2 PROCESSED 54327.0013888889 54394 53928.2501157407 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010112 We propose to make a detailed broad-band X-ray spectroscopic study of the radio quiet QSO (RQQ) Kaz 102. This RQQ had a power-law spectrum with a photon index ~ 1 with our ASCA observation. We also found a spectral variability over the time scale of years, from ~ 2.2 during the ROSAT All Sky Survey to ~ 1 during the Einstein / ASCA observations. From our ASCA spectra, we couldn't discriminate whether the apparently unusual hard spectrum was caused by warm absorber, Compton reflection, or a simple featureless power-law continuum. High quality and wide-band spectroscopy with Suzaku is essential to unveil the physical nature of the enigmatic hardness and spectral variability of Kaz 102. EXTRAGALACTIC COMPACT SOURCES 7 B ISHISAKI YOSHITAKA NULL NULL JAP 1 AO1 WHAT IS THE PHYSICAL NATURE OF KAZ 102: AN ENIGMATIC X-RAY HARD RADIO QUIET QSO? HXD N SWIFT J0255.2-0011 43.8161 -0.2397 175.95402612 -49.91735431 256.3177 54123.6209490741 54126.2294560185 701013010 101632.1 100000 101632.1 101632.1 0 101632.1 2 2 0 2 1 0 0 86282.4 86282.4 225337.9 3 PROCESSED 54330.4804050926 54735 54137.3009027778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010122 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y SWIFT J0505.7-2348 76.4285 -23.9055 225.00444872 -33.15769393 284.9903 53826.9254166667 53829.1216898148 701014010 78554.4 80000 78554.4 78554.4 78554.4 78554.4 2 2 2 2 1 0 0 53493.7 53493.7 189697.9 1 PROCESSED 54328.5694097222 54439 53945.2822569444 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010122 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD N SWIFT J0138.6-4001 24.6022 -39.9757 268.75310615 -73.8819888 44.7851 53890.7590740741 53891.2085532407 701015010 21197.9 20000 21213.9 21197.9 21213.9 21213.9 1 1 1 1 1 0 0 17477.1 17477.1 38831.9 1 PROCESSED 54320.7253472222 54394 53926.7722337963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010133 Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE HXD N SWIFT J1628.1+5145 246.9541 51.8388 79.81767806 42.92326404 60.2479 53840.7843518518 53841.3904976852 701016010 23589 20000 23605 23597 23589 23597 1 1 1 1 1 0 0 20626.1 20626.1 52359.9 2 PROCESSED 54323.1452777778 54394 53905.7494444444 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010133 Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE HXD N SWIFT J0350.1-5019 57.5315 -50.3337 259.74491819 -49.02538792 320.5309 53838.5046875 53838.6752199074 701017010 2699.8 20000 2715.8 2715.8 2699.8 2707.8 2 2 2 2 1 0 0 1177.1 1177.1 9165 0 PROCESSED 54320.4716782407 54750 53905.4679398148 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010133 Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE HXD N SWIFT J0350.1-5019 57.6662 -50.2998 259.65657878 -48.95336771 180.7044 54062.0888078704 54062.5647453704 701017020 19271 23000 19271 19271 0 19271 1 1 0 1 1 0 0 16740 16740 41097 0 PROCESSED 54322.5005787037 54750 54088.5939583333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010133 Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE HXD Y SWIFT J0350.1-5019 57.5863 -50.3518 259.75531799 -48.98660415 277.9348 54162.2927777778 54162.5036921296 701017030 8148.7 10000 8156.7 8148.7 0 8156.7 1 1 0 1 1 0 0 7059.7 7059.7 18215.9 0 PROCESSED 54320.5471412037 54750 54167.6235763889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010133 Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE HXD Y SWIFT J0601.9-8636 91.1523 -86.6779 299.2555588 -27.75439578 292.1727 53838.6834259259 53839.0779976852 701018010 19765.7 20000 19781.7 19781.7 19765.7 19773.7 2 2 2 2 1 0 0 16661.4 16661.4 34059.9 0 PROCESSED 54323.0281828704 54397 53905.4682060185 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010133 Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 1 AO1 DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE HXD N TON S180 14.333 -22.3803 138.98529016 -85.06726133 237.1425 54078.5680671296 54081.3584953704 701021010 120660.9 120000 120684.9 120660.9 0 120676.9 2 2 0 2 1 0 0 109312.8 109312.8 241052 3 PROCESSED 54329.9281018518 54735 54094.4773958333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010141 TON S180 is a luminous Narrow Line Seyfert 1 galaxy, chracterizing enhanced Soft X-ray emission component without complex absorption/emission structures. The source is considered to be at super Eddington accretion rate. We aim to track change (or no change) in soft X-ray spectrum of this source according to factor of two ,rapid flux variation this source show. We partciularly focus on the slim disk model propsed for super Eddington accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 C HAYASHIDA KIYOSHI NULL NULL JAP 1 AO1 SOFT X-RAY EMISSION FROM SUPER-EDDINGTON ACCRETION DISK IN TON S180 XIS Y M81 148.8559 68.9951 142.17660014 40.93097712 281.1688 53863.0052083333 53864.5209953704 701022010 103518.6 100000 103526.6 103526.6 103526.6 103518.6 2 2 2 2 1 0 0 70736.9 70736.9 130942.1 0 PROCESSED 54327.4538078704 54397 53913.9816550926 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010151 We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. EXTRAGALACTIC COMPACT SOURCES 7 A ITOH TAKESHI NULL NULL JAP 1 AO1 OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI HXD N MRK421 166.0521 38.1644 179.96763761 64.99940635 318.3733 53853.2821412037 53854.2711226852 701024010 41470.9 40000 41478.9 41470.9 41478.9 41478.9 2 2 2 2 1 0 0 34703.3 34703.3 85430.1 1 PROCESSED 54327.9540046296 54394 53908.0343055556 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010157 We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) EXTRAGALACTIC COMPACT SOURCES 7 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC HXD N 1ES1218+304 185.3064 30.1169 186.88913956 82.72978014 298.9428 53874.8006365741 53876.706412037 701025010 79869.2 80000 79885.2 79869.2 79885.2 79877.2 2 2 2 2 1 0 0 70511.8 70511.8 164637.9 2 PROCESSED 54328.0823958333 54398 53927.8564930556 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010157 We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) EXTRAGALACTIC COMPACT SOURCES 7 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC HXD N 1ES1426+428 217.0716 42.6249 77.44668506 64.96380656 316.1862 53902.7388310185 53904.2225 701026010 60914.9 60000 60914.9 60914.9 60914.9 60914.9 2 2 2 2 1 0 0 54091.1 54091.1 128160 1 PROCESSED 54325.0427546296 54400 53928.3009143518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010157 We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) EXTRAGALACTIC COMPACT SOURCES 7 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC HXD N MRK 501 253.4 39.7089 63.52834502 38.90621529 316.9908 53934.7872569444 53935.7272916667 701027010 42427.1 40000 42438.9 42438.9 42427.1 42435.1 2 2 2 2 1 0 0 39971.1 39971.1 81209.9 0 PROCESSED 54327.2523263889 54408 53971.6784259259 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010157 We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) EXTRAGALACTIC COMPACT SOURCES 7 A TAKAHASHI TADAYUKI NULL NULL JAP 1 AO1 SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC HXD N BO 375 11.4476 41.6573 121.80050832 -21.20204189 232.9596 54135.3691666667 54135.7592476852 701028010 12779.8 13000 12779.8 12779.8 0 12779.8 1 1 0 1 1 0 0 12838.6 12838.6 33664 1 PROCESSED 54320.5282523148 54695 54151.4930324074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011120 There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. EXTRAGALACTIC COMPACT SOURCES 7 A KONG ALBERT NULL NULL USA 1 AO1 PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 XIS Y BO 375 11.4497 41.6556 121.80214792 -21.2037783 231.6187 54137.6100810185 54137.9737731482 701028020 15537.1 13000 15537.1 15537.1 0 15537.1 1 1 0 1 1 0 0 14942 14942 31415.9 0 PROCESSED 54323.2705208333 54695 54151.4987731482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011120 There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. EXTRAGALACTIC COMPACT SOURCES 7 A KONG ALBERT NULL NULL USA 1 AO1 PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 XIS Y BO 375 11.4497 41.6556 121.80214792 -21.2037783 231.4176 54142.8248032407 54143.2167824074 701028030 15087.8 13000 15087.8 15087.8 0 15087.8 2 2 0 2 1 0 0 15716.4 15716.4 33837.9 1 PROCESSED 54320.6731944444 54695 54153.1806828704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011120 There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. EXTRAGALACTIC COMPACT SOURCES 7 A KONG ALBERT NULL NULL USA 1 AO1 PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 XIS Y NGC 7213 332.316 -47.1629 349.59497628 -52.58020545 231.3714 54030.2323611111 54032.2759722222 701029010 90736 100000 90760 90744 90736 90752 2 2 2 2 1 0 0 90341.8 90341.8 176535.8 0 PROCESSED 54328.3152777778 54695 54056.3665162037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011305 We propose a 100ks Suzaku observation of the low luminosity AGN, NGC 7213. Previous observations show a complex iron line and weak or no Compton reflection. However the iron line and reflection hump are poorly constrained, so the line emitting matter could arise from a truncated disk, BLR or a Compton-thin torus. A high quality Suzaku observation will constrain the iron line profile, resolve the ionized emission and unambiguously determine its origin. Using the unique broad bandpass of Suzaku above 10 keV we will place tight constraints on any reflection hump, enabling us to determine if the iron line originates from a truncated disk. This could provide a direct test of the paradigm that the X-ray emission in low accretion rate AGN occurs in a truncated disk system such as an ADAF. EXTRAGALACTIC COMPACT SOURCES 7 B REEVES JAMES NULL NULL USA 1 AO1 DOES THE LOW LUMINOSITY AGN NGC7213 CONTAIN A TRUNCATED ACCRETION DISK? XIS Y NGC 5506 213.312 -3.2124 339.14600253 53.80603682 287.3743 53955.6875578704 53957.003900463 701030010 47753.1 150000 47753.1 47753.1 47753.1 47753.1 2 2 2 2 1 0 0 41097.3 41097.3 113725.9 2 PROCESSED 54324.1601041667 54695 54116.2715740741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011312 NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 A TURNER TRACEY NULL NULL USA 1 AO1 SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 XIS N NGC 5506 213.3121 -3.2119 339.14659218 53.80640928 287.3747 53958.1015972222 53959.4488425926 701030020 53296.2 63000 53304.2 53296.2 53304.2 53304.2 2 2 2 2 1 0 0 47983.2 47983.2 116386 1 PROCESSED 54326.7989351852 54695 54116.3307291667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011312 NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 A TURNER TRACEY NULL NULL USA 1 AO1 SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 XIS N NGC 5506 213.3095 -3.2029 339.1508826 53.81542712 91.2728 54131.0918055556 54132.6279513889 701030030 57406.3 150000 57414.3 57406.3 0 57414.3 2 2 0 2 1 0 0 47702.7 47702.7 132685.8 0 PROCESSED 54327.5252546296 54695 54139.3642361111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011312 NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. EXTRAGALACTIC COMPACT SOURCES 7 A TURNER TRACEY NULL NULL USA 1 AO1 SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 XIS Y MARKARIAN 335 1.5539 20.2624 108.74842011 -41.36053721 68.4831 53907.0624537037 53910.7585532407 701031010 151288.4 150000 151296.4 151288.4 151296.4 151296.4 2 2 2 2 1 0 0 140981.2 140981.2 319302.8 4 PROCESSED 54331.4392592593 54401 53928.5392361111 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011323 We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme. EXTRAGALACTIC COMPACT SOURCES 7 B MILLER JON NULL NULL USA 1 AO1 REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU HXD N NGC 3783 174.7611 -37.7364 287.45850943 22.95048745 293.6402 53910.7726388889 53912.8571412037 701033010 75719.3 75000 75719.3 75719.3 75719.3 75719.3 2 2 2 2 1 0 0 68299.3 68299.3 180023.7 0 PROCESSED 54328.3834375 54401 53926.8847453704 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011325 We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder. EXTRAGALACTIC COMPACT SOURCES 7 B MARKOWITZ ALEX NULL NULL USA 1 AO1 PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783 XIS N NGC 4151 182.6375 39.4139 155.05374688 75.05753801 112.1087 54087.8369097222 54090.3848726852 701034010 124979.6 125000 124979.6 124979.6 0 124979.6 2 2 0 2 1 0 0 131274.1 131274.1 220105.9 3 PROCESSED 54330.2256018518 54702 54132.849537037 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011327 We propose a 100 ks Suzaku observation of the brightest Seyfert Galaxy in the sky. Given the broad band-pass, and high sensitivity, the proposed observations will provide a high-quality spectrum which will allow us to search for variability in the high-ionized absorber (compared to previous observations). We will be able to obtain stringent constraints on the "Reflection Hump" and compare it to the strength of the Fe Kalpha emission line - thus providing a direct test of Reflection models. The proposed program will also complement observations of fainter and more exotic Seyferts likely to be observed during AO-1. EXTRAGALACTIC COMPACT SOURCES 7 A GEORGE IAN NULL NULL USA 1 AO1 DECOUPLING THE COMPONENTS IN THE BRIGHTEST SEYFERT: NGC 4151 XIS Y MRK 766 184.6154 29.8184 190.63186084 82.27243688 133.2599 54055.0242361111 54057.363900463 701035010 97869.3 150000 98175.6 97869.3 0 98167.6 2 2 0 2 1 0 0 96893.1 96893.1 202129.9 2 PROCESSED 54329.576400463 54800 54132.8396990741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011328 X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components EXTRAGALACTIC COMPACT SOURCES 7 B TURNER TRACEY NULL NULL USA 1 AO1 DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 XIS N MRK 766 184.6147 29.8197 190.62410896 82.27145087 134.9989 54421.893287037 54423.2363310185 701035020 59363.5 50000 59363.5 59363.5 0 59363.5 1 1 0 1 1 0 0 51151.7 51151.7 116023.8 1 PROCESSED 54433.260787037 54800 54433.2716666667 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011328 X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components EXTRAGALACTIC COMPACT SOURCES 7 B TURNER TRACEY NULL NULL USA 1 AO1 DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 XIS Y CIRCINUS GALAXY 213.2971 -65.3336 311.32997737 -3.80345965 276.4798 53937.5207986111 53939.0475 701036010 108021.7 100000 108045.7 108021.7 108045.7 108029.7 2 2 2 2 1 0 0 94272 94272 131887.9 1 PROCESSED 54327.3812152778 54401 53943.5986574074 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011331 The light of AGN dominates the hard cosmic X-ray background. However, the contribution of Compton thick objects is poorly constrained because they emit chiefly above the energy range where Chandra and XMM are sensitive. Here we propose to observe the Circinus galaxy, one of the two brightest AGN reflection sources below 10 keV and with a known high column density. Our observations below 10 keV will provide CCD spectra of the rich emission line and continuum spectra, allowing limited photoionization modelling and searches for variability, possibly seen in Circinus. In the range 10 - 60 keV, we shall obtain a spectrum of the directly viewed continuum with unprecedented S/N in the key band for the HCXB. Above 60 keV, we will detect Circinus and check whether the spectrum has a rollover. EXTRAGALACTIC COMPACT SOURCES 7 B WILSON ANDREW NULL NULL USA 1 AO1 THE HARD X-RAY BACKGROUND, COMPTON-THICK AGN AND WATER VAPOR MEGAMASERS XIS N NGC 4552 188.9456 12.612 287.9907408 75.02773792 120.0696 54072.312974537 54072.8405092593 701037010 20439.8 20000 20439.8 20439.8 0 20439.8 1 1 0 1 1 0 0 16553 16553 45543.9 0 PROCESSED 54320.7070833333 54455 54088.5410069444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011333 The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. EXTRAGALACTIC COMPACT SOURCES 7 C STEFFEN AARON NULL NULL USA 1 AO1 MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S HXD N NGC 1068 40.6928 -0.0667 172.18986515 -51.95763403 248.588 54141.0038078704 54141.9168287037 701039010 41622.9 35000 41630.9 41630.9 0 41622.9 2 2 0 2 1 0 0 41802.4 41802.4 78883.9 0 PROCESSED 54322.7992476852 54525 54151.5012962963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011333 The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. EXTRAGALACTIC COMPACT SOURCES 7 C STEFFEN AARON NULL NULL USA 1 AO1 MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S HXD N MRK 1 19.06 33.0289 128.90716196 -29.55492804 249.7486 54111.5318171296 54114.5836111111 701047010 126444.1 120000 126444.1 126444.1 0 126444.1 2 2 0 2 1 0 0 126008.2 126008.2 263635.9 2 PROCESSED 54330.9421064815 54702 54133.1552314815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011336 The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators. EXTRAGALACTIC COMPACT SOURCES 7 B LEVENSON NANCY NULL NULL USA 1 AO1 TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN HXD Y MRK 273 206.1319 55.8192 108.09580624 59.75355315 290.8776 53923.3108333333 53925.3356481482 701050010 79904.6 80000 79912.6 79904.6 79920.6 79920.6 2 2 2 2 1 0 0 82807.6 82807.6 174905.9 3 PROCESSED 54328.5733333333 54401 53930.7076851852 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011341 We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. EXTRAGALACTIC COMPACT SOURCES 7 A VEILLEUX SYLVAIN NULL NULL USA 1 AO1 THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES HXD N IRAS 19254-7245 292.8508 -72.6492 322.5078751 -28.76929596 279.8892 54041.9830208333 54044.5967476852 701052010 113512.3 120000 113520.3 113520.3 113512.3 113520.3 2 2 2 2 1 0 0 151977.8 151977.8 225809.9 1 PROCESSED 54329.7103935185 54455 54088.8285185185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011342 We propose a 120 ksec Suzaku exposure of the ULIRG IRAS19254-7245. A previous XMM-Newton observation revealed the presence of a strong iron emission line and a flat continuum, both suggesting that this source hosts a Compton-thick AGN. In this scenario, the 2-10 keV luminosity of IRAS19254-7245 could be greater than 10e44 erg/s. However since no direct continuum is visible in the XMM bandpass, a direct measure of the absorbing column density was not feasible, thus the intrinsic X-ray luminosity of this source was derived only through indirect arguments. The unique bandpass and sensititvity of Suzaku above 10 keV will allow us to confirm the Compton-thick nature of this source and to measure for the first time the intrinsic X-ray luminosity of the AGN hosted in IRAS 19254-7245. EXTRAGALACTIC COMPACT SOURCES 7 C BRAITO VALENTINA NULL NULL USA 1 AO1 ASSESSING THE ENERGETIC BUDGET IN THE SUPERANTENNAE XIS N IRAS08572+3915 135.0664 39.0091 183.47368885 40.96543811 300.022 53839.0903240741 53840.7752199074 701053010 77197.4 75000 77221.4 77197.4 77213.4 77221.4 2 2 2 2 1 0 0 62333.9 62333.9 145499.9 9 PROCESSED 54327.3290972222 54401 53906.2114699074 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011344 Ultraluminous infrared galaxies (ULIRGs) produce the energy outputs of quasars with nearly all the power emerging in the far-IR via reprocessing of optical, UV, and X-ray radiation by dust. The ultimate nuclear power source, be it AGN or compact starburst, of ULIRGs has been the focus of much debate since their discovery with the IRAS mission. While observations with Spitzer are unlocking the secrets of many nearby ULIRGs, some have nuclei that are apparently so obscured as to be optically thick even in the mid-IR. We have chosen three local ULIRGs, IRAS 08572+3915, IRAS15250+3609, and IRAS20551-4250 that are IR-bright, yet highly obscured for deep Suzaku observations to search for the tell-tale signs of a buried AGN: hard X-ray emission behind significant column densities of HI gas. EXTRAGALACTIC COMPACT SOURCES 7 A GALLAGHER SARAH NULL NULL USA 1 AO1 ULTRAHARD X-RAY CASE STUDIES OF ULIRGS WITH DEEP SILICATE ABSORPTION HXD N PDS 456 262.0807 -14.2604 10.39565911 11.16772638 98.239 54155.7486574074 54160.0355787037 701056010 190600.2 188000 190608.2 190600.2 0 190614.2 2 2 0 2 1 0 0 176470.8 176470.8 370342.8 4 PROCESSED 54389.7053356482 54757 54168.6244560185 2.1.6.14 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011351 A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole. EXTRAGALACTIC COMPACT SOURCES 7 A REEVES JAMES NULL NULL USA 1 AO1 SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456 XIS Y APM 08279+5255 127.9265 52.7635 165.74397918 36.24189551 118.0523 54020.1580902778 54022.3134143518 701057010 102332.8 100000 102340.8 102340.8 102332.8 102340.8 2 2 2 2 1 0 0 96018.7 96018.7 186185.8 3 PROCESSED 54329.5388194444 54702 54053.9467013889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011353 Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 1 AO1 VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES XIS Y APM 08279+5255 127.9229 52.7639 165.74356471 36.23970609 100.0676 54040.3996643518 54041.9690277778 701057020 102295 100000 102303 102311 102311 102295 2 2 2 2 1 0 0 95624 95624 135577.8 1 PROCESSED 54327.6775578704 54695 54088.5241782407 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011353 Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 1 AO1 VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES XIS Y APM 08279+5255 127.9195 52.7471 165.76446097 36.2381521 299.485 54183.9301041667 54186.4654513889 701057030 117143.3 125000 117143.3 117151.3 0 117143.3 2 2 0 2 1 0 0 110932.4 110932.4 219041.8 3 PROCESSED 54329.3874884259 54702 54209.5933680556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011353 Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 1 AO1 VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES XIS Y 3C 390.3 280.629 79.7686 111.4356997 27.05756334 197.286 54083.1426851852 54085.1384722222 701060010 24 100000 99367.8 99367.8 24 99367.8 2 2 1 2 1 0 0 97881.3 97881.3 172419.9 3 PROCESSED 54329.0135069445 54702 54132.9968055556 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011363 We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxies 3C382 and 3C390.3 to study their complex broad-band X-ray spectra. The HXD will constrain the continuum above 10 keV, discriminating between competing physically-different models, while at the same time the XIS will determine the parameters of the FeKalpha line and the shape of the soft X-rays. The proposed observations will allow us to shed light on the origin of reflection features in radio-loud AGN, ultimately determining the structure and ionization state of the accretion flow in these objects. EXTRAGALACTIC COMPACT SOURCES 7 C SAMBRUNA RITA NULL NULL USA 1 AO1 THE BROAD-BAND X-RAY SPECTRUM OF BROAD-LINE RADIO GALAXIES XIS Y 1ES 1553+113 238.8999 11.1305 21.81691499 43.96274027 296.7536 53940.6127777778 53941.8036342593 701070010 55635.5 55000 55643.5 55651.5 55651.5 55635.5 2 2 2 2 1 0 0 53201.5 53201.5 102881.9 0 PROCESSED 54324.9582523148 54401 53955.6133680556 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011376 Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. EXTRAGALACTIC COMPACT SOURCES 7 A REIMER ANITA NULL NULL USA 1 AO1 CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS HXD N 1ES 1101-232 165.8976 -23.5471 273.21266184 33.02701002 279.8544 53880.6859606482 53882.2161921296 701071010 62432.7 55000 62440.7 62440.7 62440.7 62432.7 2 2 2 2 1 0 0 50103.3 50103.3 132193.9 0 PROCESSED 54327.6044212963 54401 53927.4165393518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011376 Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. EXTRAGALACTIC COMPACT SOURCES 7 A REIMER ANITA NULL NULL USA 1 AO1 CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS HXD N BL LACERTAE 330.6466 42.3471 92.61224541 -10.37092111 71.9797 53882.2303703704 53883.305775463 701073010 48529.4 50000 48545.4 48545.4 48529.4 48537.4 2 2 2 2 1 0 0 35544.3 35544.3 92902 1 PROCESSED 54327.2150347222 54401 53926.2373032407 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011377 We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations. EXTRAGALACTIC COMPACT SOURCES 7 A MADEJSKI GRZEGORZ NULL NULL USA 1 AO1 SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089 HXD N 1ES 1959+650 299.9645 65.1588 98.00607393 17.68746705 45.1602 53878.0509606482 53880.1718055556 701075010 98862.2 100000 98878.2 98862.2 98870.2 98878.2 2 2 2 2 1 0 0 96106 96106 183202.8 2 PROCESSED 54331.0760416667 54408 53928.2478472222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012002 We request to observe 1ES1959+650 and 1ES2344+514 for 100 ks each with SUZAKU simultaneously with the Whipple Cherenkov telescope. Whipple will extensively monitor these sources for months in 2006-2007. There are three well defined scientific cases that we would like to address. We want to study 1) the correlation between the soft and hard X-ray and TeV fluxes and spectra, extremely variable in these sources, sometimes showing extreme conditions; 2) the mystery of the ''orphan'' flares; i.e. events observed only in the TeV gamma rays without a counterpart in the X-rays: this is currently not understood in the framework of SSC models; 3) the origin of the lag observed between soft and hard X-ray variability in some blazars and the implications for the TeV emission. EXTRAGALACTIC COMPACT SOURCES 7 A TAGLIAFERRI GIANPIERO NULL NULL EUR 1 AO1 JETS ON TEST: SIMULTANEOUS X-RAY AND TEV OBSERVATIONS OF 1ES1959+650 AND 1ES2344+514 XIS N RBS 315 36.2519 18.8398 151.73247281 -38.74296898 76.7825 53941.8167013889 53943.0404976852 701077010 47830.9 50000 47830.9 47830.9 47830.9 47830.9 2 2 2 2 1 0 0 43425 43425 105729.9 1 PROCESSED 54324.6317939815 54400 53955.7322106482 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012008 We propose to observe with Suzaku the X-ray bright blazar RBS 315, showing a very hard spectrum (Gamma<1.2) in the 2-10 keV range as determined by XMM. The requested observation will allow us to measure the continuum in the full Suzaku range (0.3-200 keV), fully exploiting the unique capabilities of the satellite. With its wide energy coverage and good response at soft energies, Suzaku will allow to determine with precision the spectral properties of the source in the hard medium and soft X-ray ranges, providing important clues on the physics and the environment of relativistic jets. A good measurement of the continuum will allow us to determine the luminosity emitted via the IC mechanism which usually dominates the radiative output and the total kinetic power carried by the outflow. EXTRAGALACTIC COMPACT SOURCES 7 B TAVECCHIO FABRIZIO NULL NULL EUR 1 AO1 SUZAKU OBSERVATION OF THE HARD BROAD BAND CONTINUUM OF THE POWERFUL BLAZAR RBS 315 HXD N NGC 5728 220.5794 -17.3095 337.26599487 38.0606459 290.4081 53935.7359143518 53936.6264930556 701079010 41307.7 40000 41307.7 41307.7 41307.7 41307.7 2 2 2 2 1 0 0 39569 39569 76941.9 0 PROCESSED 54327.1043865741 54400 53943.5061111111 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012016 The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A COMASTRI ANDREA NULL NULL EUR 1 AO1 BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD HXD N NGC 4992 197.2442 11.5776 318.61367169 73.91298788 297.9177 53904.2287615741 53905.2112615741 701080010 38788.6 40000 38788.6 38788.6 38788.6 38788.6 2 2 2 2 1 0 0 33617.9 33617.9 84881.9 1 PROCESSED 54322.8229513889 54422 53926.1865856482 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012016 The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A COMASTRI ANDREA NULL NULL EUR 1 AO1 BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD HXD N MRK 0359 21.8893 19.1757 134.6025573 -42.87605962 244.6178 54137.9789699074 54140.3738078704 701082010 107507 100000 107507 107507 0 107507 2 2 0 2 1 0 0 102576.1 102576.1 206867.8 2 PROCESSED 54329.810625 54735 54151.5150925926 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012023 Markarian 359 was the first source to be identified as a Narrow Line Seyfert 1 (NLS1) AGN, and its importance as an unusual source has been recognised for a long time. In the optical, it has unusually narrow lines for a NLS1. X-ray observations of the source are rare, but based on an XMM-Newton observation a strong reflection 'hump' is predicted. The source is therefore a critical one in the investigation of relativistically blurred photoionized disc reflection models. A detailed Suzaku observation will provide improved data quality in the XIS waveband, allow investigation of spectral variability in this waveband, and constrain the amount of reflection independently by using the HXD. EXTRAGALACTIC COMPACT SOURCES 7 C CRUMMY JAMIE NULL NULL EUR 1 AO1 NVESTIGATING REFLECTION IN MARKARIAN 359 XIS Y MKN 841 226.022 10.498 11.31218444 54.65057921 105.7688 54122.3650925926 54123.6063541667 701084010 51752.8 50000 51792.8 51752.8 0 51792.8 2 2 0 2 1 0 0 43707.7 43707.7 107237.9 1 PROCESSED 54405.8598032407 54777 54139.3030208333 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012028 We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors EXTRAGALACTIC COMPACT SOURCES 7 B PETRUCCI PIERRE-OLIVIER NULL NULL EUR 1 AO1 PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 HXD Y MKN 841 225.9811 10.3761 11.09749436 54.61837916 292.433 54304.6970949074 54306.218912037 701084020 50925.3 50000 50925.3 50933.3 0 50933.3 2 2 0 2 1 0 0 47655.6 47655.6 131473.8 2 PROCESSED 54339.4902314815 54800 54339.5240277778 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012028 We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors EXTRAGALACTIC COMPACT SOURCES 7 B PETRUCCI PIERRE-OLIVIER NULL NULL EUR 1 AO1 PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 HXD Y GB1428+4217 217.5879 42.0673 75.8575282 64.90635728 315.7011 53898.716400463 53899.8336111111 701092010 48695.6 50000 48695.6 48695.6 48695.6 48695.6 2 2 2 2 1 0 0 43494.3 43494.3 96515.9 1 PROCESSED 54324.1474074074 54394 53926.3635069444 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012043 We propose to observe GB1428+4217 at z=4.72 for 50ks with Suzaku in order to determine its spectrum up to 45 keV, corresponding to a rest-frame energy of ~250 keV. This will allow to robustly model the spectrum in terms of a hard power-law and a Comptonization component from the scattering of `cold' electrons in the jet onto the soft nuclear photon field, as qualitatively hinted by XMM-Newton available data. This would be the first detection of such a feature in blazars and would directly and uniquely give information on the power of the relativistic jets in this source. EXTRAGALACTIC COMPACT SOURCES 7 A FABIAN ANDREW NULL NULL EUR 1 AO1 JET POWER OF THE DISTANT EXTREME LUMINOSITY BLAZAR GB1428+4217 XIS N MARKARIAN 509 311.0194 -10.6637 36.02321332 -29.81091499 73.1708 53850.7831481482 53851.5252199074 701093010 24575.6 25000 24575.6 24575.6 24591.6 24591.6 2 2 2 2 1 0 0 15407 15407 64097.9 1 PROCESSED 54322.7706828704 54394 53907.6894560185 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A PONTI GABRIELE NULL NULL EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU HXD N MARKARIAN 509 311.0427 -10.7271 35.96837179 -29.85867019 254.3019 54022.3263888889 54023.0856365741 701093020 25929.8 25000 25961.8 25929.8 25953.8 25961.8 2 2 2 2 1 0 0 23449.7 23449.7 65589.9 1 PROCESSED 54326.9374305556 54526 54053.6032638889 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A PONTI GABRIELE NULL NULL EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU XIS N MARKARIAN 509 311.0428 -10.7274 35.9681072 -29.85888698 254.2043 54054.375150463 54055.0113541667 701093030 24446.6 25000 24446.6 24446.6 0 24446.6 2 2 0 2 1 0 0 18327 18327 54967.9 1 PROCESSED 54323.3565162037 54456 54088.6171875 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A PONTI GABRIELE NULL NULL EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU XIS N MARKARIAN 509 311.0451 -10.7278 35.96880101 -29.86110163 254.2048 54066.1625810185 54067.12875 701093040 33094.4 32000 33094.4 33094.4 0 33094.4 2 2 0 2 1 0 0 29454.4 29454.4 83465.9 1 PROCESSED 54323.874212963 54456 54088.5895023148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012050 We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). EXTRAGALACTIC COMPACT SOURCES 7 A PONTI GABRIELE NULL NULL EUR 1 AO1 SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU XIS N PKS 1510-089 228.2108 -9.1043 351.2856545 40.1353659 286.8003 53949.3968634259 53952.2544444445 701094010 119157.7 120000 119157.7 119157.7 119165.7 119165.7 2 2 2 2 1 0 0 106258.8 106258.8 246863.8 5 PROCESSED 54330.8922337963 54394 54018.7363194444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013016 It has been a long mystery (i) how the relativistic jets are formed, and (ii) what is the composition of a jet. In the theoretical view, strong magnetic field (u_B >> u_e) is necessary to produce such outflows with baryonic matters, but observations favor opposite scenario, namely particle dominated (u_e >> u_B), leptonic jet. Such discrepancies can be resolved if moderate numbers of protons (n_e/n_p > 50) are mixed in the non-tnermal pair populations. This can be easily tested if we can observe characteristic "soft X-ray bump" produced by the bulk-Comptonization of UV photons emitted from an accretion disk. We propose a deep observation (40ksec x3) of an EGRET quasar PKS 1510-089, which shows a clear sign of soft X-ray bump in BeppoSAX, ROSAT and ASCA observations. EXTRAGALACTIC COMPACT SOURCES 7 B KATAOKA JUN MADEJSKI GRZEGORZ JUS 1 AO1 DIRECT TESTING THE JET COMPOSITION IN A POWERFUL EGRET QUASAR PKS 1510-089 XIS N M106 184.7117 47.2376 138.43381178 68.89762168 287.1938 53896.5413078704 53898.7113425926 701095010 99817.5 100000 99881.5 99817.5 99881.5 99881.5 2 2 2 2 1 0 0 97522.9 97522.9 187483.9 1 PROCESSED 54328.0368634259 54401 53927.2308449074 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013151 We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. EXTRAGALACTIC COMPACT SOURCES 7 A ITOH TAKESHI REYNOLDS CHRISTOPHER JUS 1 AO1 OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI HXD N F05189-2524 80.2383 -25.4117 227.93752087 -30.32292957 290.8212 53835.6784259259 53837.6467708333 701097010 78155.5 80000 78155.5 78163.5 78155.5 78155.5 2 2 2 2 1 0 0 51740.2 51740.2 169989.9 2 PROCESSED 54328.8577546296 54401 53906.8811689815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014341 We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. EXTRAGALACTIC COMPACT SOURCES 7 A VEILLEUX SYLVAIN ANABUKI NAOHISA USJ 1 AO1 THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES HXD N NGC 4395 186.4111 33.4884 162.54122992 81.55189464 303.1476 54253.6042013889 54256.2981944444 702001010 101507.5 100000 101515.5 101507.5 0 101515.5 2 2 0 2 1 0 0 101929.2 101929.2 232719.8 4 PROCESSED 54329.6868055556 54745 54263.5438194445 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020001 We propose a 100 ks observation of the intermediate mass black hole (IMBH) active nucleus in the dwarf Seyfert galaxy NGC 4395. Utilising the high-energy sensitivity of Suzaku will enable us to determine the shape of the intrinsic continuum, which is significantly absorbed below 10 keV. Constraining the shape of the continuum will allow us to investigate the more general problem of the relationship between AGN flux and apparent spectral slope. In addition, with a firm grasp of the intrinsic continuum properties, we can accurately determine the physical conditions of the warm absorber in NGC 4395. EXTRAGALACTIC COMPACT SOURCES 7 A TANAKA YASUO NULL NULL JAP 2 AO2 UNCOVERING THE IMBH ACTIVE NUCLEUS IN THE DWARF SEYFERT GALAXY NGC 4395 HXD Y NGC1386 54.1629 -35.9533 237.58696036 -53.99184818 64.5172 54309.0884259259 54310.1668402778 702002010 55522.6 50000 55522.6 55530.6 0 55530.6 2 2 0 2 1 0 0 47521.3 47521.3 93143.9 1 PROCESSED 54404.8194675926 54707 54339.0775115741 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020005 Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. EXTRAGALACTIC COMPACT SOURCES 7 A AWAKI HISAMITSU NULL NULL JAP 2 AO2 REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU HXD Y NGC2273 102.5972 60.7838 155.04232679 23.32753471 246.2514 54211.2737384259 54212.5071643518 702003010 90012.6 50000 90028.6 90020.6 0 90012.6 2 2 0 2 1 0 0 69588.7 69588.7 106557.9 1 PROCESSED 54324.7668865741 54744 54216.1628703704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020005 Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. EXTRAGALACTIC COMPACT SOURCES 7 A AWAKI HISAMITSU NULL NULL JAP 2 AO2 REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU HXD Y NGC3393 162.075 -25.2139 270.6699706 29.83420275 292.9271 54243.7827662037 54245.1876041667 702004010 55227 50000 55227 55227 0 55227 2 2 0 2 1 0 0 48255 48255 121369.9 4 PROCESSED 54326.7547453704 54745 54255.6532986111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020005 Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. EXTRAGALACTIC COMPACT SOURCES 7 A AWAKI HISAMITSU NULL NULL JAP 2 AO2 REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU HXD Y NGC5135 201.4174 -29.8897 311.72101463 32.39717213 286.1252 54284.2497800926 54285.3057175926 702005010 52496.4 50000 52496.4 52496.4 0 52496.4 2 2 0 2 1 0 0 49783.7 49783.7 91220.9 2 PROCESSED 54328.4348726852 54696 54328.4497453704 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020005 Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. EXTRAGALACTIC COMPACT SOURCES 7 A AWAKI HISAMITSU NULL NULL JAP 2 AO2 REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU HXD Y 3C 326 238.0402 20.0989 33.27596058 48.22956027 119.5805 54484.6775 54486.215462963 702006010 61738.1 60000 61738.1 61738.1 0 61738.1 2 2 0 2 1 0 0 53412.6 53412.6 132859.8 1 PROCESSED 54515.017349537 54888 54515.0338078704 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020014 Suzaku observations of two giant radio galaxies, 3C 326 and 3C 35, are proposed. In 60 ks exposure on the individual targets, inverse Component X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic fields in these lobesare precisely deteremined. The size of these radio galaxies are significantly larger than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated. EXTRAGALACTIC COMPACT SOURCES 7 C ISOBE NAOKI NULL NULL JAP 2 AO2 SUZAKU OBSERVATIONS OF LOBES OF GIANT RADIO GALAXIES, 3C 326 AND 3C 35 XIS Y OJ 287 FLARE 133.7115 20.1695 206.74425687 35.84822718 98.7868 54411.475 54413.896099537 702008010 112044 100000 112052 112060 0 112044 2 2 0 2 1 0 0 102923.8 102923.8 209151.9 3 PROCESSED 54423.355462963 54791 54423.3848032407 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020024 OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions. EXTRAGALACTIC COMPACT SOURCES 7 A ISOBE NAOKI NULL NULL JAP 2 AO2-TOO MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 HXD Y OJ 287 QUIESCENT 133.689 20.0482 206.87650629 35.78772906 283.9125 54200.8243055556 54203.4654976852 702009010 102844.1 100000 102844.1 102844.1 0 102844.1 2 2 0 2 1 0 0 93624.4 93624.4 228185.9 12 PROCESSED 54330.5065740741 54744 54210.7303587963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020024 OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions. EXTRAGALACTIC COMPACT SOURCES 7 A ISOBE NAOKI NULL NULL JAP 2 AO2-TOO MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 HXD Y NGC5643 218.1422 -44.2268 321.40267054 14.9878026 293.4229 54331.8795023148 54332.9724421296 702010010 42882.3 50000 42890.3 42890.3 0 42882.3 2 2 0 2 1 0 0 40868.5 40868.5 94386 2 PROCESSED 54402.1882986111 54770 54402.2016782407 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020034 Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2. EXTRAGALACTIC COMPACT SOURCES 7 B AWAKI HISAMITSU NULL NULL JAP 2 AO2 SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 HXD Y IC 3639 190.1935 -36.8078 300.55692841 26.01476797 293.9494 54293.1966435185 54294.4133564815 702011010 53391.2 50000 53391.2 53391.2 0 53391.2 2 2 0 2 1 0 0 48485.2 48485.2 105110 1 PROCESSED 54339.5002083333 54709 54339.5331365741 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020034 Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2. EXTRAGALACTIC COMPACT SOURCES 7 B AWAKI HISAMITSU NULL NULL JAP 2 AO2 SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 HXD Y ARK 120 79.0439 -0.2064 201.74563913 -21.16237248 274.9546 54191.755162037 54193.905150463 702014010 100863.5 100000 100863.5 100863.5 0 100863.5 2 2 0 2 1 0 0 95312.1 95312.1 185743.9 1 PROCESSED 54329.4936689815 54744 54200.5657060185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020035 We propose to obtain the broad-band spectra of the bright Seyfert 1 Ark 120 with Suzaku. Since Ark 120 shows no strong absorption features in its X-ray spectrum, we can cleanly measure the shape of the continuum and Fe K line without introducing any ambiguity caused by absorption along the line of sight. The spectrum will be used to test the diskline hypothesis in Seyferts and to study the fundamental processes producing broad band spectra of AGNs. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 2 AO2 THE ORIGIN OF THE BROAD FE LINE IN THE SEYFERT 1 ARK 120 HXD Y NGC 7314 338.9055 -25.9984 27.22535085 -59.7013223 59.6979 54215.4316319444 54217.9516666667 702015010 109019.8 100000 109019.8 109019.8 0 109019.8 2 2 0 2 1 0 0 92240.8 92240.8 217713.9 2 PROCESSED 54330.1497685185 54744 54230.4096527778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020037 We propose a Suzaku observation of the highly variable Seyfert 1.9 NGC 7314. The Fe K line in this object varies on a very short time scale (<10 keV) in contrast to Seyferts observed with Suzaku in the SWG time. The data will be used to search for a weak broad Fe K line to constrain the inner radius of an optically thick disk and to study the spectral variation on short time scales to elucidate the fundamental processes producing X-rays in the vicinity of the central black hole. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 2 AO2 RAPID SPECTRAL X-RAY VARIABILITY IN THE SEYFERT GALAXY NGC 7314: UNDERSTANDING ENERGY RELEASE PROCESSES IN AGN HXD Y M82 X-1 149.1432 69.7042 141.33659361 40.60182861 163.0524 54367.135775463 54367.8716898148 702026010 35599.9 40000 36031.9 35599.9 0 36023.9 2 2 0 2 1 0 0 30474.9 30474.9 63569.9 1 PROCESSED 54402.2441782407 54770 54402.2563657407 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020092 We propose Suzaku observations of the intermediate-mass black hole candidate M82 X-1 for spectral study with a wide-band energy range including over 10 keV. In particular, the purpose is to determine a spectral cut-off energy in details in order to improve unified understanding of different mass black holes in comparison with those of stellar-mass black holes and ULXs in nearby galaxies. EXTRAGALACTIC COMPACT SOURCES 7 C MIYAWAKI RYOHEI NULL NULL JAP 2 AO2 HARD X-RAY SPECTRAL STUDY OF M82 X-1 WITH SUZAKU HXD Y IGR J21247+5058 321.1969 51.0428 93.38215801 0.42876214 108.8126 54206.5871759259 54208.4613888889 702027010 85031.9 80000 85031.9 85039.9 0 85047.9 2 2 0 2 1 0 0 70970.9 70970.9 161894.9 2 PROCESSED 54328.6750925926 54744 54214.1071412037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020097 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 2 AO2 BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y SWIFT J1922.7-1716 290.6403 -17.2233 20.73500926 -14.48356253 80.064 54198.231099537 54200.4321643518 702028010 78638.6 80000 78638.6 78638.6 0 78638.6 2 2 0 2 1 0 0 61353.3 61353.3 190129.8 0 PROCESSED 54328.9208101852 54744 54206.3754166667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020097 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 2 AO2 BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y MRK 1239 148.0816 -1.6118 239.27134701 38.21950621 286.5242 54226.0919907407 54227.5973726852 702031010 63128 80000 63128 63128 0 63128 2 2 0 2 1 0 0 53594.4 53594.4 130061.9 2 PROCESSED 54324.6011226852 54744 54235.4602662037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020127 X-ray observations of "Hidden" narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that both obscuring material and nucleus of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the evolution of supermassive black holes and host galaxies. Hence,we propose 80 ksec observation of the candidates of hidden NLS1s Mrk 1239. Large effective area and unprecedented wide energy band of Suzaku allows us to strictly constrain the column density and covering fraction of obscuring matter, intrinsic power law slope, and its luminosity. From these observations, we expect to derive more complete unified picture of AGNs EXTRAGALACTIC COMPACT SOURCES 7 B HABA YOSHITO NULL NULL JAP 2 AO2 SUZAKU VIEW OF "HIDDEN" NARROW-LINE SEYFERT 1 GALAXY MRK 1239 XIS Y LMC X-4 83.1886 -66.3594 276.32297371 -32.53740633 226.9086 54500.7929513889 54501.0521875 702036010 0 20000 0 0 0 0 0 0 0 0 1 0 0 5672.9 5672.9 22377.9 1 PROCESSED 54515.3684606482 54883 54515.6401851852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021127 We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. EXTRAGALACTIC COMPACT SOURCES 7 A HICKOX RYAN NULL NULL USA 2 AO2 SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW XIS Y LMC X-4 83.221 -66.3591 276.32094979 -32.52452295 284.2438 54561.5523842593 54562.3058333333 702036020 25339.7 20000 25342.5 25342.5 0 25339.7 2 2 0 2 1 0 0 24502 24502 65070 0 PROCESSED 54573.9719328704 54943 54574.4237152778 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021127 We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. EXTRAGALACTIC COMPACT SOURCES 7 A HICKOX RYAN NULL NULL USA 2 AO2 SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW XIS Y LMC X-4 83.1883 -66.3595 276.32310713 -32.53751505 226.9099 54507.0294560185 54507.6043287037 702037010 23381.4 20000 23389.4 23397.4 0 23381.4 1 1 0 1 1 0 0 20047 20047 49662 1 PROCESSED 54515.5505208333 54883 54515.5898842593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021127 We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. EXTRAGALACTIC COMPACT SOURCES 7 A HICKOX RYAN NULL NULL USA 2 AO2 SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW XIS Y LMC X-4 83.1804 -66.3624 276.32693529 -32.54034863 209.1491 54480.3607175926 54480.7919560185 702038010 21657.9 20000 21672.6 21657.9 0 21672.6 2 2 0 2 1 0 0 22883.7 22883.7 37252 0 PROCESSED 54490.3013773148 54860 54490.3089236111 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021127 We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. EXTRAGALACTIC COMPACT SOURCES 7 A HICKOX RYAN NULL NULL USA 2 AO2 SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW XIS Y NGC 4593 189.9131 -5.3426 297.48049807 57.40434975 112.24 54449.1962384259 54451.972349537 702040010 118841.5 107000 118841.5 118841.5 0 118841.5 2 2 0 2 1 0 0 108976 108976 239789.9 6 PROCESSED 54460.7119212963 54829 54462.4425462963 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021302 We propose a 80 ksec observation of the bright Seyfert 1 NGC 4593 to resolve the moderately relativistic Fe K line, and test for a truncated or ionized accretion disk. To achieve accurate modeling of the broad Fe line, Suzaku's broad bandpass is required to deconvolve the broadband emitting component and accurately constrain the continuum. NGC 4593 is one of the few Seyferts to also show evidence for Fe XXVI emission at 6.9 keV; we will use the XIS to confirm the line and constrain its origin. If the thin accretion disk is truncated or transitions to an ADAF, it would reveal NGC 4593 to be an analogue of low/hard-state X-ray Binaries. EXTRAGALACTIC COMPACT SOURCES 7 C MARKOWITZ ALEX NULL NULL USA 2 AO2 DOES THE SEYFERT AGN NGC 4593 HAVE A TRUNCATED OR IONIZED ACCRETION DISK? XIS Y 1H0419-577 66.5116 -57.211 266.99901337 -41.98911345 55.5914 54306.2319328704 54309.0835532407 702041010 205862.8 200000 205870.8 205870.8 0 205862.8 2 2 0 2 1 0 0 152831.7 152831.7 246357.8 2 PROCESSED 54339.6903819444 54706 54339.7211111111 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021304 A hotly debated question is whether Seyfert X-ray spectra are dominated by components that are blurred by strong gravitational effects close (< 20rg) to the central black hole. Models featuring either complex absorption or blurred disk spectra provide equally good parameterizations of the mean X-ray spectrum of many objects. To make progress with current instruments we require observations with a temporal baseline and flux that will allow us to look for key parameter correlations, as the two scenarios predict different time-dependent behavior. To that end, we propose a Suzaku observation of 1H0419-577, a target that exhibits a remarkable degree of spectral variability in the X-ray regime promising some definitive results in this important area. EXTRAGALACTIC COMPACT SOURCES 7 B TURNER TRACEY NULL NULL USA 2 AO2 HOW IMPORTANT IS STRONG RELATIVISTIC BLURRING IN SPECTRA OF SEYFERT GALAXIES? XIS Y NGC5548 214.4931 25.1284 31.93341942 70.49864062 309.3821 54269.9362847222 54270.6389814815 702042010 31118.8 30000 31118.8 31118.8 0 31118.8 2 2 0 2 1 0 0 27175.9 27175.9 60705.9 0 PROCESSED 54319.4566435185 54695 54319.4659953704 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC5548 214.4931 25.1252 31.92399813 70.49805067 305.6592 54275.9121643518 54276.6918055556 702042020 35915.2 30000 35915.2 35915.2 0 35915.2 2 2 0 2 1 0 0 33175 33175 67341.9 3 PROCESSED 54322.4809606482 54695 54322.4919675926 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC5548 214.4933 25.1285 31.9338138 70.49848107 305.6607 54289.4186921296 54290.1182175926 702042040 30699.6 30000 30699.6 30699.6 0 30699.6 1 1 0 1 1 0 0 28827.9 28827.9 60431.9 1 PROCESSED 54328.4766666667 54695 54328.4843402778 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC5548 214.4959 25.1277 31.932758 70.49602002 293.6791 54296.5817013889 54297.4168865741 702042050 30019.7 30000 30027.7 30035.7 0 30019.7 2 2 0 2 1 0 0 26300.4 26300.4 58971 1 PROCESSED 54339.2748263889 54707 54340.3894328704 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC5548 214.4955 25.1272 31.93108614 70.4962838 289.7815 54303.4447337963 54304.2711111111 702042060 28917.8 30000 28925.8 28925.8 0 28917.8 1 1 0 1 1 0 0 24818.1 24818.1 71383.9 1 PROCESSED 54339.5215856482 54706 54339.5363310185 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC5548 214.4969 25.1266 31.93001973 70.4949274 285.8791 54310.1810648148 54311.0209953704 702042070 31809.9 30000 31809.9 31809.9 0 31809.9 1 1 0 1 1 0 0 29503 29503 72527.9 1 PROCESSED 54404.8288657407 54706 54339.4245486111 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC5548 214.4979 25.1264 31.92993093 70.49400067 281.7605 54317.0262268518 54318.0211111111 702042080 38775.7 210000 38783.7 38791.7 0 38775.7 1 1 0 1 1 0 0 32649.7 32649.7 85951.9 0 PROCESSED 54404.8530671296 54714 54347.3528472222 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021307 We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 2 AO2 NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y FAIRALL 9 20.9481 -58.8141 295.06951561 -57.81752905 48.1772 54258.155462963 54260.5766666667 702043010 167798.3 164000 167798.3 167806.3 0 167814.3 2 2 0 2 1 0 0 136483.4 136483.4 209175.8 2 PROCESSED 54406.0927083333 54773 54265.5470717593 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021313 Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. EXTRAGALACTIC COMPACT SOURCES 7 A MILLER JON NULL NULL USA 2 AO2 REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN XIS Y MARKARIAN 79 115.6357 49.8015 168.6115046 28.38007803 283.4884 54193.9134953704 54195.7655439815 702044010 83703.8 82000 83711.8 83703.8 0 83711.8 2 2 0 2 1 0 0 82104.2 82104.2 160005.9 0 PROCESSED 54328.2755208333 54695 54203.4223842593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021313 Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. EXTRAGALACTIC COMPACT SOURCES 7 B MILLER JON NULL NULL USA 2 AO2 REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN XIS Y NGC 1365 53.3968 -36.1347 237.94662462 -54.6022242 221.6565 54486.2300578704 54490.0002083333 702047010 160505.7 150000 160505.7 160513.7 0 160513.7 2 2 0 2 1 0 0 146813.9 146813.9 325676.8 4 PROCESSED 54515.4053356482 54883 54515.5847800926 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021314 We propose a 150 ksec observation of the Seyfert Galaxy NGC 1365. This galaxy have a unique set of properties: FeXXV and FeXXVI Kalpha and Kbeta absorption lines (the highest S/N detection so far among AGNs), rapidly varying cold absorber (nH variations of ~10^23/cm^2 in a few hours, changes from Compton-thick to Compton-thin in two days), a relativistic iron emission line. This new long observation will use at best the unique capabilities of Suzaku to constrain the dimensions of the absorbers, and, for the first time, will investigate the dynamics and physical conditions of the hot absorber responsible of the iron absorption lines. It is likely that an occultation will occur during the observation. This occultation would directly set the dimension of the X-ray source. EXTRAGALACTIC COMPACT SOURCES 7 C RISALITI GUIDO NULL NULL USA 2 AO2 BLACK HOLE OCCULTATION AND OUTFLOW VARIABILITY IN NGC 1365 XIS Y NGC 4507 188.8987 -39.9119 299.63576127 22.85843053 109.5879 54454.5145717593 54456.5835532407 702048010 103626 80000 103634 103626 0 103634 2 2 0 2 1 0 0 110902.1 110902.1 178727.9 0 PROCESSED 54462.266875 54829 54462.288287037 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021331 Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. EXTRAGALACTIC COMPACT SOURCES 7 B REEVES JAMES NULL NULL USA 2 AO2 REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES XIS Y NGC 6300 259.2549 -62.8185 328.49505458 -14.05378352 296.7285 54390.5141087963 54392.375162037 702049010 82577 80000 82577 82577 0 82577 2 2 0 2 1 0 0 105512.7 105512.7 160779.8 1 PROCESSED 54403.3611805556 54770 54403.3802083333 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021331 Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. EXTRAGALACTIC COMPACT SOURCES 7 B REEVES JAMES NULL NULL USA 2 AO2 REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES XIS Y NGC7582 349.5472 -42.3304 348.20905034 -65.68466064 49.5845 54221.7937384259 54222.3176273148 702052010 23941.2 25000 23957.2 23941.2 0 23957.2 2 2 0 2 1 0 0 21581.6 21581.6 45256 0 PROCESSED 54323.1774884259 54695 54228.073275463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021332 We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. EXTRAGALACTIC COMPACT SOURCES 7 A CHIABERGE MARCO NULL NULL USA 2 AO2 MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 HXD Y NGC7582 349.5634 -42.322 348.21143031 -65.69925686 64.738 54248.9237152778 54249.7328587963 702052020 28769 25000 28769 28769 0 28769 2 2 0 2 1 0 0 24682.4 24682.4 69905.9 0 PROCESSED 54326.9903819444 54695 54255.6928472222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021332 We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. EXTRAGALACTIC COMPACT SOURCES 7 A CHIABERGE MARCO NULL NULL USA 2 AO2 MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 HXD Y NGC7582 349.6446 -42.4137 347.94526846 -65.70277041 233.1822 54413.9093981482 54414.6459490741 702052030 29353.8 25000 29353.8 29353.8 0 29353.8 2 2 0 2 1 0 0 24433.1 24433.1 63631.9 1 PROCESSED 54423.1829513889 54790 54423.1929398148 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021332 We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. EXTRAGALACTIC COMPACT SOURCES 7 A CHIABERGE MARCO NULL NULL USA 2 AO2 MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 HXD Y NGC7582 349.6411 -42.4153 347.94523476 -65.69973119 236.7954 54420.0722337963 54420.8960532407 702052040 31895.5 25000 31895.5 31895.5 0 31895.5 2 2 0 2 1 0 0 25780.6 25780.6 71171.9 0 PROCESSED 54430.2881597222 54797 54430.3041203704 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021332 We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. EXTRAGALACTIC COMPACT SOURCES 7 A CHIABERGE MARCO NULL NULL USA 2 AO2 MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 HXD Y PKS 1345+12 206.9131 12.3498 347.38894416 70.20282736 113.9421 54472.3082407407 54473.6799768518 702053010 52984.4 50000 52984.4 52984.4 0 52984.4 2 2 0 2 1 0 0 45203.4 45203.4 118503.8 4 PROCESSED 54483.4785185185 54854 54483.4984375 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021341 We wish to take advantage of the sensitivity of Suzaku above 10 keV to constrain the energy source -- starburst or black-hole driven activity -- in three of the brightest warm transitional ultraluminous infrared galaxies, PKS 1345+12, Mrk 463, and 3C 273. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short time scale variability, another signature of black-hole driven activity. These data will be combined with our A01 spectra and be part of S. Teng's PhD thesis at UMD. EXTRAGALACTIC COMPACT SOURCES 7 C VEILLEUX SYLVAIN NULL NULL USA 2 AO2 SPECTRA OF THE BRIGHTEST WARM ULTRALUMINOUS INFRARED GALAXIES HXD Y 3C 445 335.9528 -2.0995 61.86726076 -46.70852053 68.9567 54245.2015046296 54248.9169444444 702056010 139769.1 125000 139769.1 139769.1 0 139769.1 2 2 0 2 1 0 0 117241.2 117241.2 320991.8 4 PROCESSED 54331.1051388889 54702 54256.717662037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021352 It is well known that the circum-black hole environ of Seyferts contain warm, photoionized gas responsible for complex absorption/emission at X-rays. Evidence for such components in radio-loud AGN is, instead, rare. And yet, presence of an ionized, scattering medium is postulated by unification models for these sources, and some models for jet formation. Here we tackle this problem by proposing sensitive Suzaku observations of 3C445, the only Broad-Line Radio Galaxy exhibiting soft X-ray emission lines from 0.4-3 keV in an archival EPIC spectrum. We will: 1) Determine the broad-band continuum; 2) Study the properties of the soft emission lines, determining the gas density and location, and thus its role in jet collimation; and 3) Confirm the strong reflection component suggested by EPIC. EXTRAGALACTIC COMPACT SOURCES 7 A SAMBRUNA RITA NULL NULL USA 2 AO2 WARM GAS IN THE INNER REGIONS OF RADIO-LOUD AGN: THE CASE OF 3C445 XIS Y 4C+74.26 310.5668 75.0616 108.92036641 19.50581044 289.6922 54401.4314467593 54403.2606944444 702057010 91583 100000 91583 91583 0 91591 2 2 0 2 1 0 0 94114 94114 158029.8 1 PROCESSED 54409.2276967593 54776 54409.2446064815 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021354 We propose a 100 ks observation of the bright broad-line radio galaxy 4C+74.26. A previous 35 ks XMM-Newton observation of 4C+74.26 yielded the first indication of a relativistically broadened Fe K line in a radio-loud AGN as well as other typical AGN properties (e.g., a warm absorber). The long observation proposed here will allow a detailed investigation of the Fe K line profile and improve significantly on the previous observation by detecting the associated Compton reflection hump with the HXD/PIN instrument. Modeling of these features will allow the first accurate determination of the geometry and structure of the inner accretion disk in a radio-loud AGN, and hence provide invaluable information for modeling the physics of the disk/jet interaction. EXTRAGALACTIC COMPACT SOURCES 7 C BALLANTYNE DAVID NULL NULL USA 2 AO2 A CLOSE LOOK AT 4C+74.26 WITH SUZAKU: FOCUSING IN ON THE DISK/JET INTERACTION HXD Y NGC 1052 40.2309 -8.2134 181.91154484 -57.92833515 49.7745 54297.4313888889 54299.87875 702058010 100669.1 100000 100669.1 100669.1 0 100669.1 2 2 0 2 1 0 0 83499.8 83499.8 211427.8 2 PROCESSED 54339.7403125 54707 54339.9136458333 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021355 Accretion onto supermassive black holes is thought to play a major role in the production of relativistic jets. Our understanding of jet production remains elusive, however, because we cannot image the accretion flow. Fortunately, the Fe K line offers a direct probe of accretion. As part of a multi-mission monitoring program of the radio loud AGN NGC 1052, we propose two 100 ksec Suzaku observations to obtain best-quality X-ray spectra at two epochs to determine the true continuum shape and thus probe the relativistic iron line, determine line and continuum variability patterns and possibly investigate how the structure of the accretion disk changes when there are jet ejection events. Our aim is to determine what leads supermassive black holes to launch powerful jets. EXTRAGALACTIC COMPACT SOURCES 7 A WEAVER KIMBERLY NULL NULL USA 2 AO2 PROBING THE DISK-JET CONNECTION IN AGN WITH AN INTENSIVE MULTIWAVELENGTH MONITORING CAMPAIGN OF NGC 1052 HXD Y 3C 33 17.2445 13.2796 129.4936436 -49.368548 249.2604 54460.3029282407 54463.6390509259 702059010 127367.7 100000 127375.7 127375.7 0 127367.7 2 2 0 2 1 0 0 106588.5 106588.5 288203.6 7 PROCESSED 54483.4427199074 54854 54483.4886458333 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021356 We propose a 100 ks Suzaku observation of the nucleus of the nearby (z=0.0597) FRII radio galaxy 3C 33, to constrain the nature of its Compton reflection component, and make an accurate measurement of its Fe Ka emission line. 3C 33 (awarded category-C time in Suzaku AO-1, not observed) is the only radio-loud AGN with evidence of Compton reflection in its low-energy (< 10 keV) spectrum, and so offers a unique opportunity to study both the soft- and hard-band properties of reflection. The HXD will allow us, for the first time, to constrain the nature of the Compton reflection component in 3C 33 and, when combined with the superb sensitivity of the XIS, will enable us to determine the line-of-sight geometry and structure of the reflecting region. EXTRAGALACTIC COMPACT SOURCES 7 B EVANS DANIEL NULL NULL USA 2 AO2 CONSTRAINING THE REFLECTION PROPERTIES OF THE NARROW-LINE RADIO GALAXY 3C 33 HXD Y Q1946+7658 296.1546 77.0965 109.22346589 23.50098326 3.7704 54294.4255902778 54294.6432175926 702060010 13163.6 13000 13163.6 13163.6 0 13163.6 1 1 0 1 1 0 0 13928.2 13928.2 18775.9 0 PROCESSED 54338.9810300926 54706 54339.4067824074 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021361 The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. EXTRAGALACTIC COMPACT SOURCES 7 C CHARTAS GEORGE NULL NULL USA 2 AO2 AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q0450-1310 73.3011 -13.0912 211.74785299 -32.06702416 263.6423 54535.8878240741 54536.2502314815 702062010 15510.2 13000 15510.2 15510.2 0 15510.2 2 2 0 2 1 0 0 14988.7 14988.7 31305.9 0 PROCESSED 54550.1580902778 54916 54550.1640277778 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021361 The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. EXTRAGALACTIC COMPACT SOURCES 7 C CHARTAS GEORGE NULL NULL USA 2 AO2 AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q1017+1055 155.041 10.671 230.36219873 50.83483368 121.1263 54431.9135185185 54432.4376851852 702064010 18048.6 20000 18048.6 18048.6 0 18048.6 2 2 0 2 1 0 0 15031.6 15031.6 45281.9 0 PROCESSED 54438.2755324074 54805 54438.285150463 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021361 The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. EXTRAGALACTIC COMPACT SOURCES 7 C CHARTAS GEORGE NULL NULL USA 2 AO2 AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q1334-0033 204.1954 -0.819 326.07775276 59.99926461 306.9566 54295.3551736111 54295.7084953704 702067010 13962.1 15000 13962.1 13962.1 0 13962.1 1 1 0 1 1 0 0 13006.4 13006.4 30519.9 0 PROCESSED 54340.4650694444 54710 54340.4777430556 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021361 The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. EXTRAGALACTIC COMPACT SOURCES 7 C CHARTAS GEORGE NULL NULL USA 2 AO2 AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q1548+0917 237.6002 9.1581 18.5566992 44.16075413 106.1242 54513.4560763889 54514.16 702068010 32113.3 23000 32121.3 32121.3 0 32113.3 1 1 0 1 1 0 0 29475.6 29475.6 60815.9 0 PROCESSED 54522.1385763889 54889 54522.1462731482 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021361 The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. EXTRAGALACTIC COMPACT SOURCES 7 C CHARTAS GEORGE NULL NULL USA 2 AO2 AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y 3C 273 187.2559 1.9961 289.92713501 64.30042167 293.1671 54281.0022569444 54282.2661342593 702070010 54892.7 67000 54892.7 54892.7 0 54892.7 2 2 0 2 1 0 0 51259.2 51259.2 109143.9 1 PROCESSED 54322.4738078704 54695 54322.4904166667 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021364 We propose a Suzaku campaign on the bright z=0.158 quasar 3C 273. The source exhibits a Seyfert-like X-ray spectrum when the luminosity is low but is dominated by emission from the jet in a high state. Suzaku will be able to measure the broadband spectrum, especially X-ray reprocessed features, with greater sensitivity than ever before. Decoupling and monitoring of the disk and jet components will enable detailed spectroscopy to help understand the disk-jet connection and the wider implications for AGN physics in general. The target is bright and well-suited because for most AGN either the disk or jet component dominates. For this pilot study we propose two 50 ks observations, one in each visibility window. The science goals cannot be achieved with existing data or other missions. EXTRAGALACTIC COMPACT SOURCES 7 C YAQOOB TAHIR NULL NULL USA 2 AO2 EXPLORING THE ACCRETION DISK AND JET CONNECTION IN 3C 273 WITH SUZAKU HXD Y 3C 452 341.4131 39.7498 98.13461856 -16.98917572 65.3539 54267.3964351852 54268.8294444444 702073010 66680 53000 66696 66680 0 66696 2 2 0 2 1 0 0 61448.7 61448.7 123801.8 3 PROCESSED 54319.4771296296 54695 54319.4923032407 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021372 The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS HXD Y 3C 105 61.8399 3.6518 187.66746701 -33.63397375 251.3728 54501.5363078704 54503.0833912037 702074010 38319 53000 38319 38319 0 38319 2 2 0 2 1 0 0 48881.1 48881.1 133655.8 2 PROCESSED 54515.7480555556 54883 54515.7678819444 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 021372 The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS HXD Y SWIFT J0318.7+6828 49.4315 68.5395 135.6962435 9.37350025 42.3301 54365.4488078704 54367.125162037 702075010 77115.6 53000 77139.6 77115.6 0 77139.6 2 2 0 2 1 0 0 70685.5 70685.5 144797.8 1 PROCESSED 54403.1820949074 54770 54403.1984490741 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021372 The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS HXD Y SWIFT J0918.5+0425 139.5114 4.476 227.10001498 34.41934616 102.3204 54408.8894097222 54410.2293981482 702076010 61018.5 53000 61018.5 61040.1 0 61018.5 2 2 0 2 1 0 0 56156.5 56156.5 115765.9 2 PROCESSED 54419.0165046296 54787 54419.0312847222 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021372 The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. EXTRAGALACTIC COMPACT SOURCES 7 C MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS HXD Y MRK 417 162.3659 22.9016 214.84390845 62.11471123 281.9359 54238.6593402778 54239.5730555556 702078010 41506.6 40000 41506.6 41506.6 0 41506.6 2 2 0 2 1 0 0 39338.5 39338.5 78923.9 0 PROCESSED 54327.1706944444 54695 54245.0002430556 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021374 Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY HXD Y NGC 1142 43.7827 -0.1295 175.79604248 -49.86350093 73.9096 54302.4506481482 54303.4308333333 702079010 40569.7 40000 40569.7 40569.7 0 40569.7 2 2 0 2 1 0 0 36540.4 36540.4 84679.9 1 PROCESSED 54339.0974421296 54706 54339.1106828704 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021374 Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY HXD Y ESO 506-G027 189.6943 -27.3584 299.48164005 35.42851647 302.0467 54314.0460300926 54315.2572222222 702080010 41745.3 40000 41753.3 41761.3 0 41745.3 1 1 0 1 1 0 0 38282.8 38282.8 104639.9 2 PROCESSED 54404.8592708333 54710 54340.5553125 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021374 Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY HXD Y MCG +04-48-002 307.1488 25.8021 67.06317106 -7.53431612 93.9583 54208.4668634259 54209.4134143518 702081010 41298.8 40000 41306.8 41298.8 0 41306.8 2 2 0 2 1 0 0 37746.6 37746.6 81769.9 2 PROCESSED 54323.0106597222 54695 54217.0231712963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021374 Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 2 AO2 SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY HXD Y XBONGBLUE1 217.1061 32.8569 54.10325006 68.28811801 132.8525 54453.8528587963 54454.166875 702082010 15172.5 13000 15172.5 15172.5 0 15172.5 2 2 0 2 1 0 0 15699.6 15699.6 27125.9 0 PROCESSED 54461.0379861111 54828 54461.0450231482 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021376 We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. EXTRAGALACTIC COMPACT SOURCES 7 C JONES CHRISTINE NULL NULL USA 2 AO2 OBSCURED AGN AND XBONGS IN BOOTES XIS Y XBONGBLUE2 217.7653 34.3413 57.71878971 67.47993323 130.3787 54454.1686921296 54454.5050694445 702084010 14816.2 13000 14816.2 14816.2 0 14816.2 1 1 0 1 1 0 0 14579.4 14579.4 29055.9 0 PROCESSED 54460.6591898148 54828 54460.6654398148 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021376 We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. EXTRAGALACTIC COMPACT SOURCES 7 C JONES CHRISTINE NULL NULL USA 2 AO2 OBSCURED AGN AND XBONGS IN BOOTES XIS Y TYPE2AGN 216.4026 35.2819 60.85487771 68.34395808 307.3753 54292.1781712963 54292.6183333333 702090010 19838.7 19000 19846.7 19854.7 0 19838.7 2 2 0 2 1 0 0 20870 20870 38015.9 0 PROCESSED 54339.0031134259 54706 54339.0120833333 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021376 We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. EXTRAGALACTIC COMPACT SOURCES 7 C JONES CHRISTINE NULL NULL USA 2 AO2 OBSCURED AGN AND XBONGS IN BOOTES XIS Y PHOENIX GALAXY 120.9921 5.0644 216.72692126 18.43029643 304.6737 54222.3296296296 54223.9585069445 702111010 58867.7 50000 58867.7 58867.7 0 58867.7 2 2 0 2 1 0 0 49697.8 49697.8 140723.9 5 PROCESSED 54327.561087963 54744 54230.3771527778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022002 We propose a 50 ks Suzaku observation of the Seyfert galaxy UGC4203 (a.k.a. Mrk 1210), the ``Phoenix Galaxy''. It is one of the sources which have been discovered to change from Compton-thin to reflection-dominated states. The aim of the proposal is to understand the origin of this variation (i.e. as either due to flux or to NH variations) by measuring its column density and compare it to previous observations. Suzaku is unique for this task, because thanks to its broad band it may probe column densities up to several times 10^24 cm^-2 in this source, which has never been observed above 10 keV. EXTRAGALACTIC COMPACT SOURCES 7 B MATT GIORGIO NULL NULL EUR 2 AO2 THE NATURE OF THE VARIATIONS OF STATE IN THE PHOENIX GALAXY HXD Y MCG+8-11-11 88.7233 46.5039 165.67352488 10.43795472 91.6485 54360.0736342593 54362.2640509259 702112010 98748.1 100000 98748.1 98756.1 0 98764.1 2 2 0 2 1 0 0 89213.8 89213.8 186438.7 1 PROCESSED 54404.9212037037 54751 54371.4963078704 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022004 We propose to observe with Suzaku for 100 ks one of the X-ray brightest AGN, the Seyfert 1 galaxy MCG+8-11-11, with the aim to measure the fraction of the reflection component and the iron abundance. Suzaku provides a unique opportunity to perform this kind of analysis, thanks to its broadband coverage. Moreover, the proposed observation will provide an extremely good spectrum, which will allow us to measure the iron line width, its Compton Shoulder and the ionization stage of iron. These three measurements will contribute to provide useful information on the nature of the iron line emitting material, its distance from the central Black Hole and the mass of the latter. EXTRAGALACTIC COMPACT SOURCES 7 B BIANCHI STEFANO NULL NULL EUR 2 AO2 MCG+8-11-11: A BROADBAND SPECTRUM OF ONE OF THE X-RAY BRIGHTEST AGN HXD Y IC4329A 207.3319 -30.3107 317.49747069 30.91844112 292.4395 54313.2280092593 54314.0419444444 702113010 25453.4 25000 25453.4 25453.4 0 25453.4 2 2 0 2 1 0 0 21442.2 21442.2 70292 1 PROCESSED 54404.8868518518 54710 54340.5826273148 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022009 IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. EXTRAGALACTIC COMPACT SOURCES 7 A CAPPI MASSIMO NULL NULL EUR 2 AO2 SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF XIS Y IC4329A 207.3329 -30.3099 317.49868436 30.91898994 293.8517 54318.0289930556 54318.8786226852 702113020 30623.3 25000 30623.3 30623.3 0 30623.3 2 2 0 2 1 0 0 25746.1 25746.1 73384 3 PROCESSED 54404.8923148148 54730 54347.5971180556 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022009 IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. EXTRAGALACTIC COMPACT SOURCES 7 A CAPPI MASSIMO NULL NULL EUR 2 AO2 SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF XIS Y IC4329A 207.3319 -30.3116 317.49719871 30.9175719 295.4804 54323.458599537 54324.2127777778 702113030 26895.9 25000 26895.9 26895.9 0 26895.9 2 2 0 2 1 0 0 23872.3 23872.3 65130.9 0 PROCESSED 54404.8915162037 54730 54347.7226041667 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022009 IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. EXTRAGALACTIC COMPACT SOURCES 7 A CAPPI MASSIMO NULL NULL EUR 2 AO2 SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF XIS Y IC4329A 207.3317 -30.3084 317.49797139 30.92070724 297.0437 54328.4922106482 54329.1612731482 702113040 24219.4 25000 24219.4 24219.4 0 24219.4 2 2 0 2 1 0 0 20203.1 20203.1 57800 1 PROCESSED 54404.9209027778 54730 54351.1843171296 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022009 IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. EXTRAGALACTIC COMPACT SOURCES 7 A CAPPI MASSIMO NULL NULL EUR 2 AO2 SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF XIS Y IC4329A 207.3321 -30.3098 317.49793706 30.91926559 298.5047 54332.9765740741 54333.5558333333 702113050 24026.2 25000 24026.2 24026.2 0 24026.2 2 2 0 2 1 0 0 18825.6 18825.6 50043.9 1 PROCESSED 54404.9196296296 54730 54350.649375 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022009 IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. EXTRAGALACTIC COMPACT SOURCES 7 A CAPPI MASSIMO NULL NULL EUR 2 AO2 SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF XIS Y RBS 1124 187.6975 70.7093 125.39855918 46.31993489 339.073 54204.9538078704 54206.5786921296 702114010 86228.4 88000 86228.4 86228.4 0 86228.4 2 2 0 2 1 0 0 88855.5 88855.5 140384 3 PROCESSED 54325.1096759259 54744 54210.6501851852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022019 We propose a 70 ks observation of RBS 1124 (z=0.208). This is the X--ray brightest radio--quiet quasar (> 4e45 erg/s in the 2-10 keV band) from the ROSAT bright source catalogue. The expected number of counts (e.g. about 120,000 in just one FI XIS unit and about 11,000 in the HXD/PIN) will provide the best quality X-ray spectrum so far for such a high luminosity AGN. We will investigate the main X-ray spectral components shedding light on this extreme class of objects with unprecedented accuracy making full use of the Suzaku sensitivity across the whole band (XIS and HXD). EXTRAGALACTIC COMPACT SOURCES 7 A MINIUTTI GIOVANNI NULL NULL EUR 2 AO2 REVEALING THE X-RAY EMISSION/ACCRETION PROCESSES IN THE VERY LUMINOUS RADIO-QUIET AND X-RAY BRIGHT QUASAR RBS 1124 HXD Y IRAS 10565+2448 164.8573 24.5988 212.34078465 64.72788111 119.4619 54410.6325 54411.4675347222 702115010 39423.2 30000 39423.2 39423.2 0 39423.2 2 2 0 2 1 0 0 35738.8 35738.8 72145.9 0 PROCESSED 54423.150162037 54791 54423.1618518518 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022023 We propose for 30ks Suzaku observations of two ultra-luminous infrared galaxies that lack sensitive 2keV constraints to provide a complete census of Active Galactic Nuclei (AGN) activity in ULIRGs out to 200Mpc. Six (~75%) of the eight ULIRGs in our sample for which we already have sensitive >2keV constraints host AGN activity, indicating that black-hole growth is ubiqitious in the most luminous local galaxies. Our proposed observations are sensitive enough to identify luminous AGN activity (L_X=3x10^{43} erg/s) out to ~40keV, to accurately quantify the properties of less luminous AGN activity, and to identify and quantify the star-formation activity. In addition the results will be used to better understand the z~2 ULIRG population, the likely progenitors of todays massive galaxies. EXTRAGALACTIC COMPACT SOURCES 7 C ALEXANDER DAVID NULL NULL EUR 2 AO2 A COMPLETE CENSUS OF AGN ACTIVITY IN ULTRA-LUMINOUS GALAXIES OUT TO 200 MPC HXD Y AKN 564 340.6246 29.7785 92.13720271 -25.27363853 56.6178 54277.5375694444 54279.8002199074 702117010 99978.1 100000 99986.1 99986.1 0 99978.1 2 2 0 2 1 0 0 87225.3 87225.3 195473.9 1 PROCESSED 54333.4885532407 54703 54333.5152199074 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022024 Narrow Line Seyfert 1 galaxies show complex X-ray behaviour. At low flux levels their 2-10~keV spectra are hard, with a huge excess at lower energies. Conversely, at high fluxes, the same objects show a soft 2-10 keV spectrum, with moderate soft excess. This behaviour can be explained either by reflection or absorption models. It is important to distinguish between these scenarios as they imply critical differences in the inferred physics of the accretion flow. There is already good Suzaku data on the hard 2-10 keV spectra from a GT observation of NGC4051. We propose to compare this with 100ks of data from Akn564, the brightest NLS1 at 10keV having a soft 2-10keV spectrum, so as to use the full range of spectral behaviour seen in NLS1's to determine the origin of the soft excess. EXTRAGALACTIC COMPACT SOURCES 7 A DONE CHRIS NULL NULL EUR 2 AO2 UNDERSTANDING THE ORIGIN OF SPECTRAL COMPLEXITY IN NLS1: AKN564 HXD Y IRAS18325-5926 279.2243 -59.4565 335.92469241 -21.3483138 281.9669 54399.3814699074 54401.4169444444 702118010 78434.8 80000 78434.8 78442.8 0 78442.8 2 2 0 2 1 0 0 74291.7 74291.7 175835.7 0 PROCESSED 54409.2827893518 54777 54409.305474537 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022025 We propose a 80 ks observation of the Seyfert galaxy IRAS 18325-5926. Previous observations show evidence for reflection from highly ionized matter, absorption features in the 8-10 keV band, and a possible roll-over of the continuum spectrum at around 30 keV. The observation goal is to elucidate the continuum roll-over and to investigate variability of the spectral features, which would have many important implications for the physical condition and the geometry of the accretion disc and the illuminating source. This study will provide crucial keys to understand the geometry of primary X-ray source and immediate surroundings. The broad-band coverage and the high sensitivity at the hard X-ray band provided by Suzaku are ideally suited to study this unique AGN. EXTRAGALACTIC COMPACT SOURCES 7 C MISAKI KAZUTAMI NULL NULL EUR 2 AO2 HARD X-RAY SPECTRUM OF IRAS 18325-5926: REFLECTION FROM AN IONIZED DISC AND CONTINUUM ROLL-OVER HXD Y ESO 323-G032 193.3499 -41.5832 303.32560645 21.28704922 104.5857 54456.5856481482 54458.1459953704 702119010 79249.4 80000 80817.8 79249.4 0 80801.4 2 2 0 2 1 0 0 86896.7 86896.7 134777.8 1 PROCESSED 54483.0970023148 54854 54483.1116203704 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022033 The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. EXTRAGALACTIC COMPACT SOURCES 7 A COMASTRI ANDREA NULL NULL EUR 2 AO2 BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II HXD Y ESO 263-G013 152.4256 -42.8603 273.99206854 10.74227458 292.0779 54252.4568287037 54253.5946064815 702120010 45294.7 40000 45302.7 45302.7 0 45294.7 2 2 0 2 1 0 0 40103.5 40103.5 98299.9 2 PROCESSED 54324.2595486111 54745 54258.5006134259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 022033 The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. EXTRAGALACTIC COMPACT SOURCES 7 B COMASTRI ANDREA NULL NULL EUR 2 AO2 BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II HXD Y SWIFT J2127.4+5654 322.001 56.878 97.78160785 4.29621592 243.6186 54443.0645023148 54445.0487962963 702122010 91730.4 88000 0 91730.4 0 91730.4 0 2 0 2 1 0 0 89348.5 89348.5 171379.9 2 PROCESSED 54629.4060300926 55000 54633.7130439815 2.2.8.20 2 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 022034 We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). EXTRAGALACTIC COMPACT SOURCES 7 C MINIUTTI GIOVANNI NULL NULL EUR 2 AO2 HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU HXD Y IGR J16185-5928 244.6464 -59.4001 326.66672881 -6.44446627 90.0003 54505.6700115741 54507.0211111111 702123010 76607.6 88000 76631 76623.6 0 76607.6 2 2 0 2 1 0 0 75255.3 75255.3 116725.9 0 PROCESSED 54515.6434490741 54888 54515.6564699074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 022034 We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). EXTRAGALACTIC COMPACT SOURCES 7 B MINIUTTI GIOVANNI NULL NULL EUR 2 AO2 HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU HXD Y MRK 110 141.3383 52.3497 164.91808924 44.3703784 110.1475 54406.3443055556 54408.31625 702124010 90871.2 100000 90871.2 90879.2 0 90879.2 2 2 0 2 1 0 0 86523.1 86523.1 170355.8 2 PROCESSED 54417.6687384259 54786 54417.3880092593 2.1.6.16 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 023012 We request a 100 ks SUZAKU observation of Mrk 110 to quantify the accretion disk geometry in this high luminosity narrow line Seyfert 1 galaxy. This is an unique low mass AGN which shows an almost featureless X-ray continuum described by a two component Comptonization model. It has shown, based on an XMM-Newton data, energy dependent delays which are consistent with the idea of a Comptonized plasma confined within 10 Schwartzschild radius of the central black hole. The proposed long observation will provide high signal-to-noise hard X-ray data, thus allowing us to extend the observed delay to higher energies and also to quantify the high energy spectral parameters like cut-off energy and reflection parameters. This will help us to identify the accretion disk geometry in this source. EXTRAGALACTIC COMPACT SOURCES 7 C RAO ARIKKALA Dewangan Gulab EUS 2 AO2 PROBING THE ACCRETION DISK GEOMETRY IN THE TYPE I SEYFERT GALAXY MRK 110 HXD Y 3C382 278.7516 32.7087 61.3132426 17.46021716 69.589 54217.9621412037 54220.8119097222 702125010 130580 120000 130588 130580 0 130588 2 2 0 2 1 0 0 122470.7 122470.7 246195.8 2 PROCESSED 54405.9745717593 54777 54228.2765740741 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 024353 We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxy 3C382 to study its complex broad-band X-ray spectrum and its variability on longer timescales. To this end, we ask for 3 separate observations of 40 ks each, to be scheduled randomly but not less than a couple of days apart. We aim at probing the origin of the reflection features and strong soft excess in 3C382, ultimately determining the structure and ionization state of the accretion flow. The addition of 3C382 to the Suzaku program (already including 3C120 and 3C390.3) will allow us to explore BLRGs central engines over a wide range of accretion/jet parameters. EXTRAGALACTIC COMPACT SOURCES 7 B SAMBRUNA RITA Kataoka Jun USJ 2 AO2 THE HIGH-ENERGY SPECTRA OF BROAD-LINE RADIO GALAXIES XIS Y PKS2126-15 322.2988 -15.6437 35.92993079 -41.86589251 72.3882 54576.0912384259 54578.4238310185 703001010 81921.4 80000 81921.4 81936.4 0 81945.4 2 2 0 2 1 0 0 71541.4 71541.4 201527.9 3 PROCESSED 54594.3202546296 54961 54594.3427777778 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030003 We propose intensive Suzaku observations (80ksec each) of two "primitive" blazars at z > 3.3, with a highly unusual SED. ROXA J081009.9 (z=4.0) was recently found by a short Swift/XRT exposure (6 ksec) with a luminosity well in excess of 10^47 ergs/s, but its synchrotron power peaking above 10 keV. This may suggest the bulk Lorentz factor of the jet could reach ~1000 like GRBs, though quite conspicuous among the AGN jets. Meanwhile, unusual SED of PKS2126-15 (z=3.3) , where the synchrotron peaking at GHz and the inverse Compton peaks at ~10 keV, is most likely due to the presence of ultra-massive black hole with 2x10^10 Ms. These new-types are only found in highly distant universe, and maybe categorized as primitive blazars. EXTRAGALACTIC COMPACT SOURCES 7 B KATAOKA JUN NULL NULL JAP 3 AO3 UNVEILING NEW-TYPE "PRIMITIVE" BLAZARS WITH SUZAKU XIS Y PKS0208-512 32.6864 -51.0102 276.09849974 -61.78596913 230.2146 54814.3149074074 54815.4793171296 703002010 51959.4 40000 51983.4 51959.4 0 51983.4 2 2 0 2 1 0 0 42559 42559 100599.9 0 PROCESSED 54826.2979513889 54557 54826.3087268518 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030004 We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 3 AO3 REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS XIS Y Q0827+243 127.7159 24.1868 200.01721235 31.87611482 114.1438 54766.2156828704 54767.3363310185 703003010 48227.7 40000 48227.7 48227.7 0 48227.7 2 2 0 2 1 0 0 39303.1 39303.1 96800.1 0 PROCESSED 54788.22875 54557 54788.24125 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030004 We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 3 AO3 REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS XIS Y PKS1127-145 172.5274 -14.8245 275.2785401 43.63731171 115.9184 54799.7571180556 54800.9523611111 703004010 55545.1 40000 55551.1 55545.1 0 55551.1 2 2 0 2 1 0 0 31012.3 31012.3 103248.8 0 PROCESSED 54809.1868518518 54557 54809.1987152778 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030004 We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 3 AO3 REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS XIS Y PKS1510-089 228.2094 -9.0956 351.2919833 40.14272744 102.2005 54858.1887615741 54859.2258564815 703005010 44305.4 40000 44305.4 44305.4 0 44305.4 2 2 0 2 1 0 0 16653.7 16653.7 89597.9 0 PROCESSED 54963.1375810185 54557 54880.5404282407 2.3.12.25 3 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 030004 We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 3 AO3 REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS XIS Y 3C454.3 343.4943 16.1419 86.11034311 -38.19103065 250.8076 54792.3878703704 54793.6884143518 703006010 46923.9 40000 46923.9 46923.9 0 46923.9 2 2 0 2 1 0 0 43344 43344 112313.9 2 PROCESSED 54802.2109722222 54557 54811.7229050926 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030004 We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 3 AO3 REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS XIS Y IGR J12391-1612 189.807 -16.1292 298.65896251 46.64122293 122.9437 54818.9051273148 54822.2910648148 703007010 130274 120000 130274 130274 0 130274 2 2 0 2 1 0 0 111089.3 111089.3 292483.8 2 PROCESSED 54840.3391319444 55206 54840.5288425926 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030012 We propose a Suzaku observation of a Compton thick candidate, IGR J12391-1612. This source is a bright Seyfert 2 galaxy in the INTEGRAL AGN catalog by Beckman et al. 2006. By a follow-up observation in the optical band, this source was classified as an X-ray luminous type 2 Seyfert galaxy. A Chandra follow-up observation was also performed, but the shape of the X-ray spectrum was not well determined due to a short exposure of 3.5ks. Thank to the wide-band spectroscopy of Suzaku, we can obtain an X-ray spectrum in the 0.5-100 keV band. We will reveal the nature of this Compton thick Seyfert in a spectral analysis. EXTRAGALACTIC COMPACT SOURCES 7 A AWAKI HISAMITSU NULL NULL JAP 3 AO3 X-RAY OBSERVATION OF A COMPTON THICK CANDIDATE, IGR J12391-1612 HXD Y SWIFT J0911.2+4533 137.9062 45.5305 174.70874001 43.11152809 111.3983 54764.185787037 54766.2105787037 703008010 93879 80000 93879 93879 0 93895 2 2 0 2 1 0 0 80225.6 80225.6 174929.8 4 PROCESSED 54781.2130787037 55148 54782.4040625 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030034 The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 3 AO3 THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT HXD Y SWIFT J1200.8+0650 180.2185 6.7488 270.13481807 66.34579154 293.0035 54617.9027662037 54619.9280555556 703009010 84486.6 80000 84510.6 84486.6 0 84510.6 2 2 0 2 1 0 0 71110.9 71110.9 174963.8 3 PROCESSED 54634.1249652778 55003 54634.1479282407 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030034 The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 3 AO3 THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT HXD Y NGC 1313 49.5565 -66.5364 283.40259478 -44.62074971 201.281 54805.9606828704 54808.2814699074 703010010 91466.1 100000 91498.1 91466.1 0 91498.1 2 2 0 2 1 0 0 78759.3 78759.3 200493.7 1 PROCESSED 54822.5975694444 55188 54822.6519328704 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030038 The nature of ultra luminous X-ray sources (ULX) is one of the most important unresolved issue in the modern astrophysics. We propose a 100 ks observation of an famous ULX, NGC 1313 X1, in order to search for Fe-K absorption lines, which are important spectral feature of Galactic black holes. Through the absorption feature, we will examine the nature of the ULX. EXTRAGALACTIC COMPACT SOURCES 7 C OHSUGA KEN NULL NULL JAP 3 AO3 EXPLORING FE K-LINE ABSORPTION FEATURES FROM AN ULTRALUMINOUS X-RAY SOURCE, NGC 1313 X1 XIS Y NGC 5347 208.2716 33.4399 62.06849004 75.29189994 312.225 54627.6603703704 54628.6064699074 703011010 42161.1 40000 42161.1 42161.1 0 42161.1 2 2 0 2 1 0 0 37130.2 37130.2 81734 1 PROCESSED 54637.3108449074 55008 54637.3250810185 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030040 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 3 AO3 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD Y NGC 7130 327.065 -34.8962 10.02903365 -50.33744977 78.4767 54597.5198726852 54598.56625 703012010 44493.1 40000 44493.1 44493.1 0 44493.1 1 1 0 1 1 0 0 36767.7 36767.7 90375.9 1 PROCESSED 54609.0076388889 54975 54609.0170949074 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030040 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 3 AO3 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD Y SWIFT J0959.5-2258 149.843 -22.8716 259.02796733 24.98206567 303.2834 54635.9091087963 54636.8148611111 703013010 43663.4 40000 43671.4 43679.4 0 43663.4 2 2 0 2 1 0 0 42406.1 42406.1 78237.9 0 PROCESSED 54650.0471180556 55016 54650.0591782407 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 030045 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y SWIFT J0501.9-3239 79.8743 -32.7041 236.069923 -32.60257079 297.9191 54567.6584259259 54568.8788194444 703014010 41298.5 40000 41298.5 41298.5 0 41298.5 2 2 0 2 1 0 0 36434.2 36434.2 105425.9 0 PROCESSED 54580.4996064815 54953 54580.5155208333 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030045 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y SWIFT J2009.0-6103 302.158 -61.0495 335.84532046 -32.77756596 73.0628 54563.6948148148 54564.600775463 703015010 43726.8 40000 43726.8 43726.8 0 43726.8 2 2 0 2 1 0 0 36199.6 36199.6 78268 1 PROCESSED 54580.2327083333 54953 54580.2454976852 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030045 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y SWIFT J0134.1-3625 23.4345 -36.4661 261.71382804 -77.05672525 34.1001 54606.6796180556 54607.8390277778 703016010 48511.6 40000 48519.6 48511.6 0 48527.6 2 2 0 2 1 0 0 41292.7 41292.7 100149.8 0 PROCESSED 54616.3930208333 54985 54616.4068402778 2.2.7.18 2 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 030045 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y 4C73.08 147.4414 73.2521 138.04435007 38.07252036 100.3847 54786.9238888889 54788.4946643518 703018010 81375.2 80000 81375.2 81375.2 0 81375.2 2 2 0 2 1 0 0 72453.3 72453.3 135692 0 PROCESSED 54798.0309375 55164 54798.0487152778 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030063 Suzaku observation of two giant radio galaxies, 4C 73.08 and 3C 35, are proposed. In 80 ks exposure on the individual target, inverse Compton X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic field in these lobesare precisely determined. The size of these radio galaxies are significantly lager than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated EXTRAGALACTIC COMPACT SOURCES 7 C YAJI YUICHI NULL NULL JAP 3 AO3 SUZAKU OBSERVATION OF LOBES OF GIANT RADIO GALAXIES XIS Y IRAS 05262+4432 82.4599 44.6406 165.01766257 5.72021917 78.2999 54721.6357523148 54723.406412037 703019010 82086 80000 82097.5 82094 0 82086 2 2 0 2 1 0 0 70907.5 70907.5 152954.1 0 PROCESSED 54777.5804513889 55148 54780.4562037037 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030085 X-ray observations of obscured narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that absorbing material and nuclear emission of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the rapid evolution of supermassive black holes. We, therefore, propose 80 ksec observation of the candidate of an obscured NLS1 IRAS 05262+4432. High sensitivity throughout the 0.3-70 keV wide energy band of Suzaku allows us to strictly constrain the X-ray luminosity of primary emission and the geometry of the surrounding matter. From our observation, we expect to derive more complete unified picture of AGNs EXTRAGALACTIC COMPACT SOURCES 7 A HABA YOSHITO NULL NULL JAP 3 AO3 SUZAKU VIEW OF OBSCURED NARROW-LINE SEYFERT 1 GALAXY IRAS 05262+4432 HXD Y MRK421 166.1418 38.2711 179.67525089 65.03258412 111.0988 54803.7278240741 54805.9480324074 703020010 101307.5 100000 101331.5 101307.5 0 101331.5 2 2 0 2 1 0 0 65514.8 65514.8 191787.7 3 PROCESSED 54818.358287037 55188 54818.7659837963 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030119 Mrk421 provides our best opportunity to understand the high-energy emission of blazar jets, because it has produced the largest observed flux. Suzaku HXD has proved that spectum upto 40 keV can be measured only with an exposure of 1 ks from Mrk 421. Hard X-ray region is very crucial to study particle acceleration in the jet, since it corresponds to high energy end of electron distribution. Cooling and Acceleration phenomena will appear in this energy band. Here we will propose to monitor Mrk 421 for 200 ks, in which we can expect at least four or five flares. EXTRAGALACTIC COMPACT SOURCES 7 B TAKAHASHI TADAYUKI NULL NULL JAP 3 AO3 STUDY OF HARD X-RAY EVOLUTION FROM THE BRIGHTEST BLAZAR JET. HXD Y SWIFT J0444.1+2813 71.029 28.2793 172.68057795 -11.38105828 85.0234 54719.7173958333 54721.6306944445 703021010 81298.6 80000 81298.6 81298.6 0 81298.6 2 2 0 2 1 0 0 67765.4 67765.4 165303.9 0 PROCESSED 54777.7334606482 55148 54780.4776736111 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 030124 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 3 AO3 BROAD BAND SPECTRA OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y NGC3227 155.8766 19.8689 216.98457422 55.44588075 115.8562 54767.3422685185 54768.8487731482 703022010 58917.2 50000 58917.2 58917.2 0 58917.2 2 2 0 2 1 0 0 52033.7 52033.7 130147.8 1 PROCESSED 54788.2352662037 54557 54788.4566203704 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031013 We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 3 AO3 NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC3227 155.8772 19.8688 216.98506904 55.4463804 114.6051 54774.1503587963 54775.6780555556 703022020 53699.5 50000 53699.5 53699.5 0 53699.5 2 2 0 2 1 0 0 50289.1 50289.1 131971.8 3 PROCESSED 54788.1726388889 54557 54788.4371643518 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031013 We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 3 AO3 NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC3227 155.8768 19.8689 216.98468368 55.44605831 113.2489 54782.1173032407 54783.7293865741 703022030 56571.5 50000 56577.2 56585.2 0 56571.5 2 2 0 2 1 0 0 50223.1 50223.1 139269.8 1 PROCESSED 54797.0408101852 54557 54797.3603356482 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031013 We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 3 AO3 NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC3227 155.8768 19.8688 216.98485011 55.4460253 111.8565 54790.7083333333 54792.374525463 703022040 64567.9 50000 64575.9 64567.9 0 64575.9 2 2 0 2 1 0 0 46622 46622 143947.8 1 PROCESSED 54802.2821180556 54557 54812.4380324074 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031013 We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 3 AO3 NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC3227 155.8772 19.8684 216.98573476 55.44624837 110.6974 54797.8953703704 54799.750162037 703022050 79429.8 50000 79429.8 79433.9 0 79437.8 2 2 0 2 1 0 0 39843.9 39843.9 160241.8 1 PROCESSED 54809.3478703704 54557 54809.8059490741 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031013 We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 3 AO3 NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC3227 155.8768 19.8687 216.98501654 55.44599229 109.926 54802.6028125 54803.7231365741 703022060 51410.5 50000 51410.5 51410.5 0 51410.5 2 2 0 2 1 0 0 39683.6 39683.6 96781.8 1 PROCESSED 54812.0519444445 54557 54812.4432407407 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031013 We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. EXTRAGALACTIC COMPACT SOURCES 7 A ELVIS MARTIN NULL NULL USA 3 AO3 NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK XIS Y NGC 4051 180.7984 44.5394 148.85547697 70.08163582 138.344 54776.3187847222 54782.1112731482 703023010 274530.5 340000 274530.5 274530.5 0 274530.5 2 2 0 2 1 0 0 220199.3 220199.3 441448.8 3 PROCESSED 54795.4497222222 54557 54795.7746527778 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031014 The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit EXTRAGALACTIC COMPACT SOURCES 7 A TURNER TRACEY NULL NULL USA 3 AO3 DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? XIS Y NGC 4051 180.7952 44.5393 148.86124636 70.08047443 126.4079 54793.7 54795.572025463 703023020 78385.5 70000 78393.5 78385.5 0 78393.9 1 1 0 1 1 0 0 62760.4 62760.4 161735.8 0 PROCESSED 54805.3247453704 54557 54811.74875 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031014 The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit EXTRAGALACTIC COMPACT SOURCES 7 A TURNER TRACEY NULL NULL USA 3 AO3 DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? XIS Y SN 2005KD 60.8552 71.7156 136.84988934 14.24754739 218.8053 54568.8904976852 54570.0348842593 703025010 51628.9 50000 51628.9 51636.9 0 51644.9 1 1 0 1 1 0 0 63572.6 63572.6 98863.9 1 PROCESSED 54581.1905208333 54947 54581.1998842593 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031241 Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. EXTRAGALACTIC COMPACT SOURCES 7 B IMMLER STEFAN NULL NULL USA 3 AO3 SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE XIS Y SN 2006JD 120.5331 0.8102 220.45612728 16.05834455 284.354 54578.4377777778 54579.6807175926 703026010 54196.8 50000 54204.8 54196.8 0 54204.8 2 2 0 2 1 0 0 52048.8 52048.8 107339.8 1 PROCESSED 54588.1369675926 54957 54588.1523611111 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031241 Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. EXTRAGALACTIC COMPACT SOURCES 7 B IMMLER STEFAN NULL NULL USA 3 AO3 SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE XIS Y NGC 7469 345.7842 8.9301 83.10914575 -45.403242 63.4793 54641.7015856482 54644.683599537 703028010 112112.8 100000 112125.1 112133.1 0 112112.8 2 2 0 2 1 0 0 91557.1 91557.1 257612.6 2 PROCESSED 54658.7508796296 55027 54658.7891319444 2.2.8.20 2 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031311 We propose a 100 ksec observation of the X-ray bright Seyfert 1 AGN NGC 7469, a strong candidate for having ionized reflection from the accretion disk. Only the broad bandpass provided by Suzaku, including >12 keV coverage via the HXD, will allow us to deconvolve the broadband emitting components, including the strong Compton reflection hump, broad Fe K line, and soft excess. With the XIS, we will study in detail the Fe K emission complex, including the narrow 6.4 keV Fe K core and in particular the prominent ``blue wing'' near 6.9 keV. Our proposed observation will thus be an example of how broad bandpass X-ray observations can critically test blurred, ionized disk reflection model in Seyfert 1s. EXTRAGALACTIC COMPACT SOURCES 7 B MARKOWITZ ALEX NULL NULL USA 3 AO3 IONIZED DISK REFLECTION IN THE SEYFERT AGN NGC 7469 HXD Y MRK 348 12.1911 31.9636 122.27104531 -30.90471809 71.8836 54645.9325694444 54648.0591203704 703029010 87461.4 80000 88533.4 87461.4 0 88533.4 2 2 0 2 1 0 0 78550.4 78550.4 183723.9 0 PROCESSED 54664.1266666667 55031 54664.7845601852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031322 X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. EXTRAGALACTIC COMPACT SOURCES 7 A BRAITO VALENTINA NULL NULL USA 3 AO3 THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES XIS Y NGC 7172 330.5062 -31.8708 15.12698367 -53.06449716 59.7356 54611.0658680556 54612.8558217593 703030010 82279.7 80000 82279.7 82287.7 0 82287.7 2 2 0 2 1 0 0 71746.5 71746.5 154633.8 0 PROCESSED 54630.3212384259 54999 54633.7016203704 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031322 X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. EXTRAGALACTIC COMPACT SOURCES 7 A BRAITO VALENTINA NULL NULL USA 3 AO3 THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES XIS Y ESO 103- G 035 279.5941 -65.4238 329.78379096 -23.17817546 291.5832 54761.6331597222 54764.1717476852 703031010 91442 80000 91442 91450 0 91450 2 2 0 2 1 0 0 81009.6 81009.6 219282 2 PROCESSED 54781.3847916667 55148 54782.4220023148 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031322 X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. EXTRAGALACTIC COMPACT SOURCES 7 B BRAITO VALENTINA NULL NULL USA 3 AO3 THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES XIS Y NGC 788 30.262 -6.7593 165.15039638 -63.76864601 77.358 54660.0353819444 54661.0516666667 703032010 45907.3 40000 45915.3 45907.3 0 45915.3 1 1 0 1 1 0 0 39594 39594 87799.9 0 PROCESSED 54682.1347800926 55048 54682.1458564815 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031323 The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. EXTRAGALACTIC COMPACT SOURCES 7 A MUSHOTZKY RICHARD NULL NULL USA 3 AO3 SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN HXD Y NGC 3281 157.9591 -34.9074 273.03211125 19.73409342 278.2413 54607.8508449074 54609.2287615741 703033010 46234 40000 46242 46250 0 46234 2 2 0 2 1 0 0 41454.9 41454.9 119038 0 PROCESSED 54620.2696527778 54988 54620.2890162037 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031323 The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. EXTRAGALACTIC COMPACT SOURCES 7 A MUSHOTZKY RICHARD NULL NULL USA 3 AO3 SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN HXD Y 3C 111 64.5741 38.0889 161.62276278 -8.7838332 81.5451 54700.4141898148 54703.1836111111 703034010 122378 120000 122386 122378 0 122378 2 2 0 2 1 0 0 109706.7 109706.7 239251.7 1 PROCESSED 54713.6055208333 55084 54713.6361226852 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031332 The origin of the high-energy emission from Broad-Line Radio Galaxies is still an open issue. A plausible scenario is reprocessed emission from a cold medium (disk) diluted by variable, non-thermal jet flux. To test this scenario we propose Suzaku observations of the BLRG 3C 111, which exhibits flux variability above 10 keV from available data, suggesting a jet contribution. Moreover, 3C 111 was previously detected with EGRET at GeV energies, and synergy with GLAST will thus be exploited in the proposed program. The coupled timing and spectral information provided by Suzaku are key to disentangle the disk and jet contributions, and determine their respective role for the source energy budget. EXTRAGALACTIC COMPACT SOURCES 7 A SAMBRUNA RITA NULL NULL USA 3 AO3 SUZAKU OBSERVATIONS OF 3C 111: UNCOVERING THE JET WITHIN HXD Y Q0122-380 21.0759 -37.7461 271.91657466 -77.33125236 48.7944 54615.4511921296 54616.2009722222 703035010 28481 25000 28481 28489 0 28497 2 2 0 2 1 0 0 26810.7 26810.7 64769.9 1 PROCESSED 54630.2432986111 54999 54633.6971759259 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 B CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q0551-3637 88.2026 -36.6158 242.36930247 -26.91846995 296.4731 54575.4385763889 54575.6251041667 703036010 3895.4 22000 3895.4 3895.4 0 3895.4 1 1 0 1 1 0 0 3773 3773 16095.9 0 PROCESSED 54588.1166782407 54979 54588.1227314815 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q0551-3637 88.2027 -36.6207 242.37463259 -26.91966553 321.5977 54600.5596643518 54601.2044444444 703036020 21614.3 22000 21614.3 21614.3 0 21618.3 2 2 0 2 1 0 0 18283.1 18283.1 55684 1 PROCESSED 54613.0042476852 54979 54613.0157060185 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q0109-3518 17.9376 -35.0527 275.45528409 -80.96443984 40.3411 54606.0677199074 54606.6772453704 703037010 29958.5 18000 29966.5 29958.5 0 29966.5 1 1 0 1 1 0 0 22833.9 22833.9 52655.9 1 PROCESSED 54616.3720023148 54982 54616.3810300926 2.2.7.18 2 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q0329-385 52.7815 -38.4067 241.941352 -54.89845774 23.7676 54633.4249421296 54634.1898611111 703038010 30203 29000 30219 30203 0 30219 2 2 0 2 1 0 0 25292.5 25292.5 66082 1 PROCESSED 54644.1649074074 55010 54644.1762615741 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q1158-1843 180.1895 -18.9957 286.65628264 42.26876142 291.8577 54636.8208912037 54637.4202314815 703039010 24085 22000 24101 24085 0 24101 2 2 0 2 1 0 0 22430.9 22430.9 51781.9 1 PROCESSED 54648.0338657407 55014 54648.3349305556 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 B CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y Q0940-1050 145.7249 -11.0726 246.39011763 30.43738638 275.7617 54616.2125578704 54617.1321064815 703040010 32362.3 28000 32362.3 32362.3 0 32362.3 2 2 0 2 1 0 0 26777.6 26777.6 79437.8 1 PROCESSED 54630.3071759259 54999 54633.6981828704 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 031334 Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. EXTRAGALACTIC COMPACT SOURCES 7 A CHARTAS GEORGE NULL NULL USA 3 AO3 A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS XIS Y J081618.99+482328.4 124.0768 48.3841 171.01809871 33.69777889 298.4793 54917.0925462963 54919.0946643518 703042010 90922.4 90000 90922.4 90922.4 0 90922.4 2 2 0 2 1 0 0 81073.9 81073.9 172963.7 2 PROCESSED 54962.9352430556 55329 54930.3718055556 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031337 We have discovered polar broad absorption-line quasars (BALQSOs) from their radio variabilities. We know their inclination angles. Our results derived from the archival Chandra data of one polar BALQSO indicate that the X-ray emissions are from the jet and the X-ray absorbing gas is located at tens of parsecs above the accretion disk corona. We want to confirm these results at high confidence level using better signal to noise ratio data from a big observatory, like SUZAKU. In addition, we propose to observe three more polar BALQSOs, which have wide range of radio/UV/X-ray properties. Our primary science goal of this proposal is to determine the radial distribution of the X-ray absorbing gas in 4 polar BALQSOs. EXTRAGALACTIC COMPACT SOURCES 7 C GHOSH KAJAL NULL NULL USA 3 AO3 PROBING THE INNER STRUCTURE OF AGNS USING THE POLAR BALQSOS XIS Y MRK 421 166.1081 38.2021 179.85015534 65.02934628 313.5582 54591.1196527778 54595.3502199074 703043010 180785.1 150000 180793.1 180785.1 0 180793.1 2 2 0 2 1 0 0 163550.7 163550.7 343651.7 9 PROCESSED 54606.4942013889 54972 54606.5618287037 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 031341 We propose one 150 ksec Suzaku ToO observations of one of the three strong GeV-TeV gamma-ray blazars Mrk 421, Mrk 501, or 1ES 1959+650 during a 10 day multiwavelength campaign with coverage from radio to gamma-rays. The proposal is submitted by the VERITAS collaboration, assuring excellent TeV gamma-ray coverage. The Suzaku observations will play a key-role in interpreting the multiwavelength data set, allowing us to measure the time lag between the X-ray and gamma-ray flux variability and to scrutinize the correlation of the X-ray and gamma-ray spectral indices. The Suzaku and gamma-ray energy spectra will allow us to constrain the intensity of the IR Diffuse Extragalactic Background Radiation which absorbs TeV gamma-rays in extragalactic pairproduction processes. EXTRAGALACTIC COMPACT SOURCES 7 A KRAWCZYNSKI HENRIC NULL NULL USA 3 AO3-TOO TARGET OF OPPORTUNITY OBSERVATIONS OF THE BLAZARS MRK 421, MRK 501, AND 1ES 1959+650 HXD Y MRK 501 253.4335 39.8281 63.68387876 38.89139128 70.9919 54913.7775347222 54915.3328587963 703046010 72334.2 65000 72334.2 72334.2 0 72334.2 2 2 0 2 1 0 0 64836.5 64836.5 134358.1 1 PROCESSED 54962.9787152778 55329 54924.366724537 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031343 We propose to observe two bright TeV blazars with Suzaku, in coordination with VERITAS and MAGIC at TeV energies. The primary objective is to make use of the recently available observational capabilities in collecting the much needed simultaneous X-ray and TeV data on these intriguing sources. The data will be essential for addressing a number of unresolved issues in the study of TeV blazars, such as spectral variability, X-ray/TeV correlation and associated time lags, spectral hysteresis, etc. The results will likely provide insights into the properties of the emitting particles, as well as those of the emitting regions, emission mechanism, composition of the jets, and acceleration energetics. EXTRAGALACTIC COMPACT SOURCES 7 A CUI WEI NULL NULL USA 3 AO3 COORDINATED X-RAY/TEV OBSERVATIONS OF TEV BLAZARS HXD Y PKS 0528+134 82.7307 13.5905 191.31463869 -10.98486414 89.0231 54736.1098611111 54741.6752777778 703048010 203457.4 200000 203465.4 203465.4 0 203457.4 2 2 0 2 1 0 0 135362.9 135362.9 443861.9 4 PROCESSED 54778.3942592593 55148 54780.7843287037 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 031345 We propose a Suzaku observation of bright gamma-ray blazar PKS 0528+134, to be conducted jointly with GLAST, radio, and optical telescopes. This observation was accepted in the previous AO, but was not conducted due to GLAST launch delays. The goal is to obtain time-resolved broadband spectra. The X-ray and gamma-ray fluxes are known to be rapidly variable, but the information regarding the correlation between the X-ray and gamma-ray flux is limited. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A MADEJSKI GRZEGORZ NULL NULL USA 3 AO3 SUZAKU AND GLAST OBSERVATIONS OF PKS 0528+134 HXD Y 3C279 194.0685 -5.7338 305.14803375 57.11713803 113.6423 54850.9795833333 54853.9391203704 703049010 134110.6 200000 134110.6 134110.6 0 134110.6 2 2 0 2 1 0 0 82856.3 82856.3 255689 7 PROCESSED 54959.821412037 55328 54880.5781365741 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031346 We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A MADEJSKI GRZEGORZ NULL NULL USA 3 AO3 SUZAKU AND GLAST OBSERVATIONS OF 3C279 HXD Y 3C279 194.0699 -5.7328 305.15066173 57.11808922 113.6425 54854.8772222222 54856.125162037 703049020 56937 200000 56937 56937 0 56937 2 2 0 2 1 0 0 12626.3 12626.3 107779.9 2 PROCESSED 54959.5035069444 55328 54880.5584259259 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 031346 We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A MADEJSKI GRZEGORZ NULL NULL USA 3 AO3 SUZAKU AND GLAST OBSERVATIONS OF 3C279 HXD Y PKS1549-79 239.2836 -79.2302 311.18735019 -19.47008602 310.7048 54752.6495833333 54754.9009375 703059010 82175.5 80000 82197 82183.5 0 82175.5 2 2 0 2 1 0 0 79973.6 79973.6 194497.7 2 PROCESSED 54777.9933217593 55148 54780.6256597222 2.2.11.22 1 Hea_18Sep2008_V6.5.1_Suzaku_30Oct2008_V11 032005 Galaxy merger models predict rapid black hole growth and strong outflows late in the merger as the accretion rate increases. PKS1549-79 is a powerful, low redshift, high accretion rate active galaxy which has undergone a recent merger. It is therefore an ideal object to test our understanding of galaxy activity and mergers and for studying feedback between AGN and their host galaxies. We propose an 80 ksec Suzaku observation to: (i) determine the amount and ionisation state of the nuclear obscuring material in PKS1549-79 and hence confirm its status as a local proto-quasar; (ii) search for the massive, probably highly ionised, outflowing wind predicted by galaxy evolution models and hence complete a census of outflow components in this object; and (iii) quantify the high energy spectrum. EXTRAGALACTIC COMPACT SOURCES 7 B O'BRIEN PAUL NULL NULL EUR 3 AO3 UNVEILING PKS 1549-79 WITH SUZAKU XIS Y MCG-02-14-009 79.0657 -10.5106 211.75204832 -25.86275025 68.0451 54706.9410069444 54710.0308333333 703060010 142152.2 125000 142152.2 142152.2 0 142152.2 2 2 0 2 1 0 0 129587.9 129587.9 266919.9 1 PROCESSED 54731.4321064815 55100 54731.4652430556 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 032009 MCG--02-14-009 appears to have the strongest relativistic iron line of all the Seyfert 1s: a short 5 ks XMM-Newton observation found the line to have an EW 530-770 eV, two times larger than for MCG-6-30-15. We propose a 125 ks Suzaku observation of this AGN, which provides a unique opportunity to probe the innermost accretion disk in the region of strong gravity. The main goals are: (a) utilise the unique broad bandpass of Suzaku to detect the expected strong reflection hump and determine the form of the X-ray continuum; (b) accurately measure the relativistic iron K line profile and thereby the geometry of the X-ray emitting region and (c) determine whether the iron line responds to the continuum down to the orbital timescales of the inner disk. EXTRAGALACTIC COMPACT SOURCES 7 A REEVES JAMES NULL NULL EUR 3 AO3 MCG-02-14-009: PROBING THE PHYSICAL PROPERTIES OF THE STRONGEST IRON K LINE HXD Y NGC 1448 56.1426 -44.6942 251.59735556 -51.37690943 264.6522 54879.3481828704 54880.4501041667 703062010 52965.3 50000 52965.3 52965.3 0 52965.3 2 2 0 2 1 0 0 55086.9 55086.9 95202 1 PROCESSED 54963.0103472222 55330 54893.4451041667 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 032018 We propose for a 50 ks Suzaku observation of NGC 1448, a nearby (15 Mpc) gas-rich and dust-obscured Scd galaxy that is optically classified as an HII galaxy. From our Spitzer-IRS mid-IR spectroscopy, we have found the first evidence for an obscured AGN in NGC 1448. On the basis of this data, NGC 1448 appears to be harboring a rapidly growing small obscured black hole (M_BH ~ 6x10^5 M_Sun; Eddington ratio of >0.1), and therefore appears to be an analog of the nearby Compton-thick AGN NGC 4945. To date, no sensitive hard X-ray constraints exist for NGC 1448, which are required to provide a direct measurement of the absorption and mass accretion rate, and thus to test if NGC 1448 is also a Compton-thick AGN. EXTRAGALACTIC COMPACT SOURCES 7 C ALEXANDER DAVID NULL NULL EUR 3 AO3 NGC 1448: A MISSING COMPTON-THICK AGN IN OUR BACKYARD? HXD Y 1ES1426+428 217.0602 42.6327 77.47261603 64.96709047 324.5702 54622.8702662037 54625.0856944444 703063010 101166.2 100000 101166.2 101174.2 0 101174.2 2 2 0 2 1 0 0 92145.6 92145.6 191393.7 3 PROCESSED 54636.4803703704 55003 54636.5084953704 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 032021 Simultaneous optical/UV, X-ray and TeV observations are a powerful tool to study the innermost regions of blazar jets, probing the physical state of the jet close to its base. We propose to perform a long SUZAKU observation of the extreme hard-X-ray blazar 1ES 1426+428, simultaneously with MAGIC TeV observations, combined with a series of short Swift observations. With SUZAKU we will study the evolution of the X-ray emission over timescales of minutes-hours, providing important insight into the structure of the emission region and the physical process producing the radiation. We will characterize the synchrotron part of the SED and see how it correlates with the TeV spectrum, disentangling the main physical parameters and probing the still poorly known cosmic IR background. EXTRAGALACTIC COMPACT SOURCES 7 A TAGLIAFERRI GIANPIERO NULL NULL EUR 3 AO3 THE EXTREME BLAZAR 1ES 1426+428: TESTING THE JET HXD Y IRASF01475-0740 27.4875 -7.3766 160.69718538 -65.86110455 68.025 54661.0549652778 54662.3023032407 703065010 57914.7 50000 57914.7 57918.3 0 57926.3 2 2 0 2 1 0 0 51125.7 51125.7 107698.8 0 PROCESSED 54683.3915509259 55051 54683.4056712963 2.2.8.20 1 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 032030 We propose 50ks observations of IRASF01475-0740 and NGC 3147, both of which are Seyfert 2s apparently unobscured in X-rays. Unsatisfied with this apparent contradiction, we seek Suzaku observations with two main aims. First, high energy observations with the HXD can reveal whether a deeply buried AGN is present above 10 keV. Second, the XIS observations will probe sensitively for short time-scale variability below 10 keV, the detection of which would establish unambiguously that the objects have genuinely unobscured nuclei and rule out the alternatives of scattered light or X-ray binaries. EXTRAGALACTIC COMPACT SOURCES 7 A NANDRA KIRPAL NULL NULL EUR 3 AO3 SOLVING THE MYSTERY OF UNOBSCURED SEYFERT 2 GALAXIES HXD Y MRK 573 26.0161 2.2904 148.3199793 -57.9636564 249.71 55217.5861226852 55219.0328587963 704002010 64311.8 60000 64311.8 64311.8 0 64311.8 2 2 0 2 1 0 0 53747.1 53747.1 124992 0 PROCESSED 55245.7272106482 55612 55245.753599537 2.4.12.27 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040017 Monte Carlo simulation is one of the best tools to study the complex spectra of Compton-thick AGNs and to figure out the relation between their nuclear structures and X-ray spectra. We have simulated X-ray spectra of Compton-thick AGNs obscured by an accretion torus, and found that observed spectra of Compton thick objects, Mrk 3 and NGC 2273 are well reproduced by the simulated X-ray spectra. Furthermore, our simulation predicts that there are many obscured AGNs with a heavily absorbed reflection component. Their spectra are similar to that predicted from synthesis modeling of the Cosmic X-ray Background. We propose Suzaku observations of candidates of the Compton thick AGNs, Mrk 573 and Mrk 78. EXTRAGALACTIC COMPACT SOURCES 7 C AWAKI HISAMITSU NULL NULL JAP 4 AO4 SEARCH FOR COMPTON THICK AGNS WITH A HEAVILY ABSORBED REFLECTION COMPONENT HXD Y IC1586 11.9805 22.3783 121.86323541 -40.48615304 70.9045 55006.4686458333 55007.0280555556 704005010 23530.6 20000 23530.6 24346.6 0 24354.6 2 2 0 2 1 0 0 22277.8 22277.8 48325.9 0 PROCESSED 55019.1157407407 55385 55019.1259259259 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040049 We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 4 AO4 SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY XIS Y 1216-015 184.787 -1.8118 286.61259693 60.03288042 293.8466 55010.1063773148 55010.6043287037 704006010 20777.9 20000 20777.9 20785.9 0 20785.9 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 55019.6950462963 55388 55020.3653009259 2.4.12.26 3 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040049 We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 4 AO4 SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY XIS Y PKS1258-321 195.0396 -32.3625 305.06853624 30.47306853 293.0551 55027.0059259259 55027.6050231482 704007010 28460.7 20000 28460.7 28732.7 0 28727.4 3 2 0 2 1 0 0 24027.5 24027.5 51755.9 0 PROCESSED 55040.1077893518 55406 55040.1188657407 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040049 We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 4 AO4 SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY XIS Y 1739+518 264.9784 52.1719 79.52646168 31.85370007 22.9152 54985.7571759259 54986.3641087963 704008010 22486.8 20000 22494.8 22494.8 0 22486.8 2 2 0 2 1 0 0 28237.8 28237.8 52431.9 0 PROCESSED 54998.1875 55367 54998.1968634259 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040049 We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 4 AO4 SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY XIS Y NGC 454 18.511 -55.3853 296.21074431 -61.44696878 18.3891 54950.2291782407 54953.4023032407 704009010 128956.2 120000 128956.2 128956.2 0 128956.2 2 2 0 2 1 0 0 114596.9 114596.9 274129.6 0 PROCESSED 54973.4744097222 55342 54973.5148842593 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040050 Seyfert galaxies with a low-mass central black hole are a key class of objects to study the growth phase of supermassive black holes. We propose to observe the hard X-ray brightest and low-mass (1.6e6 Msolar) Seyfert 2 galaxy NGC 454 selected from the Swift BAT survey. The data will be used (1) to measure broad-band X-ray spectrum and its variability, (2) to compare them with properties of known Seyferts, and (3) to search for variation of absorption to constrain the structure and origin of obscuring matter. EXTRAGALACTIC COMPACT SOURCES 7 A TERASHIMA YUICHI NULL NULL JAP 4 AO4 X-RAY SPECTRAL VARIABILITY OF THE HARD X-RAY BRIGHTEST LOW-MASS SEYFERT 2 NGC 454 HXD Y SWIFT J2052.0-5704 312.9788 -57.0176 340.05945565 -38.72742848 73.9304 54945.6280671296 54946.6863310185 704010010 45160 40000 45160 45168 0 45168 2 2 0 2 1 0 0 57624.2 57624.2 91409.8 1 PROCESSED 54973.1900810185 55339 54973.4487152778 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040059 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 4 AO4 SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y SWIFT J1952.4+0237 298.0556 2.5705 42.31566647 -12.27488447 82.9116 54929.8284722222 54931.1079166667 704011010 47921.1 40000 47925.9 47921.1 0 47925.9 2 2 0 2 1 0 0 39304.4 39304.4 110525.8 2 PROCESSED 54949.2234259259 55324 54949.4878356482 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040059 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 4 AO4 SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y 2MASX J02485937+2630 42.225 26.5707 153.13364356 -29.32417791 74.088 55030.159224537 55031.3766782407 704013010 42950.1 40000 42950.1 43215.3 0 43224.7 2 2 0 2 1 0 0 29540.3 29540.3 105171.9 0 PROCESSED 55048.235474537 55415 55048.2541435185 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040060 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 4 AO4 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y UGC 12741 355.4449 30.6414 105.65559107 -29.88276227 64.429 54989.5219560185 54990.6711111111 704014010 47945.8 40000 47953.8 47945.8 0 47945.8 1 1 0 1 1 0 0 41524.4 41524.4 99279.9 0 PROCESSED 55000.9979398148 55367 55001.0091435185 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040060 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 4 AO4 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y NGC 4686 191.5508 54.5121 124.58283765 62.59936814 342.6621 54946.7002777778 54947.7564699074 704015010 44845.9 40000 44853.9 44845.9 0 44845.9 2 2 0 2 1 0 0 42327.5 42327.5 91232 0 PROCESSED 54973.9169328704 55339 54973.9296875 2.3.12.25 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040060 Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 4 AO4 DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS HXD Y M33 X8 23.4834 30.5892 133.64723816 -31.39681198 258.5185 55207.0743865741 55209.5626157407 704016010 106103.6 100000 106103.6 106106.1 0 106106.1 2 2 0 2 1 0 0 6105.3 6105.3 214957.7 1 PROCESSED 55218.5959027778 55587 55218.6414930556 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040067 The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. In order to solve the problem, it is of crucial importance to observe X-ray spectra above 10 keV from ULXs, which enables us to determine precisely their spectral states. Therefore, Suzaku observations of two bright ULX, M33 X8 and IC 342 X2, are proposed. EXTRAGALACTIC COMPACT SOURCES 7 C ISOBE NAOKI NULL NULL JAP 4 AO4 HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES HXD Y CENTAURUS_A 201.3411 -43.072 309.48969514 19.36734145 290.0008 55032.3718634259 55033.7683333333 704018010 62432.8 50000 62432.8 62688.8 0 62707.6 3 2 0 2 1 0 0 55450 55450 120649.9 3 PROCESSED 55048.3134375 55415 55048.3403356482 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040085 We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. EXTRAGALACTIC COMPACT SOURCES 7 A FUKAZAWA YASUSHI NULL NULL JAP 4 AO4 SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A HXD Y CENTAURUS_A 201.3322 -43.0688 309.48334217 19.37141452 298.7164 55048.3079513889 55049.7029398148 704018020 51278.7 50000 51278.7 51294.7 0 51286.7 2 2 0 2 1 0 0 43733.2 43733.2 120505.9 1 PROCESSED 55062.3310532407 55430 55062.3520023148 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040085 We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. EXTRAGALACTIC COMPACT SOURCES 7 A FUKAZAWA YASUSHI NULL NULL JAP 4 AO4 SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A HXD Y CENTAURUS_A 201.3281 -43.0649 309.48077241 19.37569293 303.3465 55057.3798148148 55059.1051388889 704018030 55944.2 50000 55952.2 55944.2 0 55944.2 2 2 0 2 1 0 0 46491.5 46491.5 149047.8 3 PROCESSED 55068.1422685185 55434 55068.1674768518 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040085 We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. EXTRAGALACTIC COMPACT SOURCES 7 A FUKAZAWA YASUSHI NULL NULL JAP 4 AO4 SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A HXD Y 3C 35 18.0181 49.4424 126.37585323 -13.29131796 245.0044 55200.6165509259 55202.466875 704019010 84756.6 80000 85028.6 84756.6 0 85020.6 2 2 0 2 1 0 0 66314.3 66314.3 147577.8 2 PROCESSED 55218.1191666667 55584 55218.1479050926 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040096 Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. EXTRAGALACTIC COMPACT SOURCES 7 B ISOBE NAOKI NULL NULL JAP 4 AO4 SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY XIS Y DA 240 EAST LOBE 117.3573 55.877 161.8466677 30.16323196 293.7777 55274.9306134259 55276.7238657407 704020010 81783.4 80000 81783.4 81791.4 0 81791.4 2 2 0 2 1 0 0 74303.3 74303.3 154921.8 1 PROCESSED 55286.304224537 55654 55286.3268518518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 040096 Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. EXTRAGALACTIC COMPACT SOURCES 7 B ISOBE NAOKI NULL NULL JAP 4 AO4 SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY XIS Y SWIFT J1322.2-1641 200.5819 -16.7858 313.4989766 45.45121448 290.037 55013.9738310185 55014.9981365741 704022010 41348.7 40000 41348.7 41620.7 0 41612.7 2 2 0 2 1 0 0 36236.8 36236.8 88485.8 7 PROCESSED 55027.0368171296 55393 55027.0523148148 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 043059 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO DADINA MAURO JEU 4 AO4 SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y MRK 352 14.9991 31.7575 125.05610732 -31.07894727 255.5628 55202.4718402778 55203.6009143518 704025010 45671.7 40000 45687.7 45671.7 0 45687.2 2 2 0 2 1 0 0 22369.3 22369.3 97535.8 1 PROCESSED 55235.2487847222 55602 55235.27125 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041402 The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. EXTRAGALACTIC COMPACT SOURCES 7 B WINTER LISA NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY HXD Y ESO 548-G081 55.4927 -21.1949 213.74761618 -50.8353425 69.3236 55046.3350462963 55047.1946064815 704026010 39411.2 40000 39419.2 39419.2 0 39411.2 2 2 0 2 1 0 0 36142.9 36142.9 74259.9 0 PROCESSED 55060.7965393518 55427 55060.8071875 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041402 The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. EXTRAGALACTIC COMPACT SOURCES 7 B WINTER LISA NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY HXD Y SWIFT J0904.3+5538 136.117 55.5749 161.50516347 40.6960792 282.0039 54949.092025463 54949.700162037 704027010 41943.8 40000 41943.8 41943.8 0 41943.8 1 1 0 1 1 0 0 35883.8 35883.8 52535.9 1 PROCESSED 54973.1461111111 55343 54973.440474537 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041402 The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. EXTRAGALACTIC COMPACT SOURCES 7 B WINTER LISA NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY HXD Y MCG +04-22-042 140.9461 22.9693 205.9821846 43.11036681 106.3587 55157.3309259259 55158.2634143518 704028010 40962 40000 40994 40962 0 40986 1 1 0 1 1 0 0 35896.9 35896.9 80559.9 0 PROCESSED 55176.1757060185 55542 55176.1858101852 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041402 The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. EXTRAGALACTIC COMPACT SOURCES 7 B WINTER LISA NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY HXD Y UGC 6728 176.2197 79.6106 126.64092866 37.03371002 285.5693 54988.5646759259 54989.5125925926 704029010 49003.9 40000 49003.9 49003.9 0 49003.9 2 2 0 2 1 0 0 41534.7 41534.7 81883.9 0 PROCESSED 54998.3251041667 55364 54998.3390740741 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041402 The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. EXTRAGALACTIC COMPACT SOURCES 7 B WINTER LISA NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY HXD Y MKN 279 208.2253 69.3021 115.05735618 46.87522986 345.4595 54965.2632407407 54968.6668287037 704031010 160351.4 150000 160359.4 160351.4 0 160359.4 2 2 0 2 1 0 0 150386 150386 293997.9 3 PROCESSED 54978.3597222222 55345 54978.3987152778 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041403 We aim to test if the high-luminosity Seyfert 1.5 Mkn 279 contains an ionized inner accretion disk by using Suzaku to spectroscopically separate the ionized and neutral reflectors. This source is relatively unobscured, allowing clear modeling of the shape of the strong soft excess; we will also test for a Fe K diskline component, which may be missing if the disk is ionized or truncated. Only a broadband X-ray spectrum, including simultaneous > 10 keV coverage to constrain Compton reflection, will allow us to thoroughly test blurred, ionized disk reflection models and constrain the nature of the reflector(s). EXTRAGALACTIC COMPACT SOURCES 7 A MARKOWITZ ALEX NULL NULL USA 4 AO4 DOES THE LOW-OBSCURATION, LOW-REFLECTION, HIGH-LUMINOSITY SEYFERT MKN279 CONTAIN AN IONIZED OR TRUNCATED ACCRETION DISK? XIS Y MCG-2-58-22 346.1839 -8.6878 64.09176202 -58.7610593 247.1128 55167.9420486111 55170.9356365741 704032010 138968.8 130000 139008.8 138968.8 0 139008.8 2 2 0 2 1 0 0 105495.7 105495.7 258627.7 2 PROCESSED 55187.5067013889 55553 55187.5510763889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041404 We propose a 130 ks Suzaku long-look to study the Fe K emission complex of the Seyfert 1.5 AGN MCG--2-58-22, which has the unique combination of being X-ray bright, ``bare'' (i.e., lacking a strong ionized absorber), and possibly hosting both a truncated accretion disk and ionized circumnuclear material. We aim to accurately constrain the geometry and ionization state of the accreting circumnuclear material of this likely low-Compton reflection source by resolving the Fe K alpha line and constraining its origin, which may likely be a truncated thin disk, and verifying a previous claim of emission from H-like Fe. We will also determine the origin of this object's soft excess. EXTRAGALACTIC COMPACT SOURCES 7 B MARKOWITZ ALEX NULL NULL USA 4 AO4 A SUZAKU OBSERVATION OF MCG--2-58-22: A TRUNCATED OR IONIZED ACCRETION DISK? XIS Y 1H0323+342 51.1507 34.2411 155.67406743 -18.71640786 76.7168 55038.1604513889 55040.2084722222 704034010 84088.4 80000 84088.4 84240.4 0 84352.4 2 2 0 2 1 0 0 74297.9 74297.9 176937.9 0 PROCESSED 55050.7947337963 55419 55050.8162847222 2.4.12.26 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041408 Recent radio observations reveal blazar-like properties in some radio-loud narrow line Seyfert-1 AGNs. 1H0323+342, classified as this class of AGNs, shows prominent hard X-ray emission with a hard photon index. Since the spectrum in hard X-ray is reminiscent of blazar, its X-ray spectrum seems to have different components originated from disk and jet. Thanks to sensitive X-ray detectors extending to the hard X-ray band, Suzaku observation is expected to resolve a possible multi-component structure in the spectrum. Since beamed radiation from jet is highly variable, spectral temporal behavior is also vital information to distinguish the emission origin. As this source is located relatively nearby (z=0.061), the source is an excellent target to investigate the emission from disk and jet. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA MASAAKI NULL NULL USA 4 AO4 SUZAKU OBSERVATION OF 1H0323+342: A PECULIAR SEYFERT-1 --PROBING THE DISK AND JET CONNECTION IN AGN-- HXD Y 3C 332 244.4239 32.3632 52.6372471 45.34839384 292.5008 55051.0341782407 55052.4655092593 704038010 59833.9 60000 59833.9 59833.9 0 59833.9 2 2 0 2 1 0 0 46049.1 46049.1 123652 0 PROCESSED 55067.2342824074 55437 55067.2557986111 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041413 We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. EXTRAGALACTIC COMPACT SOURCES 7 C BAUMGARTNER WAYNE NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS XIS Y PKS 0326-288 52.1551 -28.6965 224.90475513 -55.39691379 250.3682 55226.8889699074 55228.3266087963 704039010 58023.7 60000 58023.8 58023.7 0 58023.7 3 2 0 2 1 0 0 49624.7 49624.7 124185.9 3 PROCESSED 55249.7407523148 55616 55249.7586805556 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041413 We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. EXTRAGALACTIC COMPACT SOURCES 7 C BAUMGARTNER WAYNE NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS XIS Y NGC985 38.6279 -8.738 180.72422437 -59.4803664 62.3866 55027.6174884259 55028.5925231482 704042010 31996.9 30000 31996.9 32006.3 0 32006.3 2 2 0 2 1 0 0 25724.1 25724.1 84237.9 1 PROCESSED 55040.2426736111 55406 55040.2752430556 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041414 We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. EXTRAGALACTIC COMPACT SOURCES 7 B TREISTER EZEQUIEL NULL NULL USA 4 AO4 THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN HXD Y IGRJ01528 28.2011 -3.4464 157.35013019 -62.14500791 77.3667 55007.0338078704 55008.1426388889 704043010 46915.9 40000 46915.9 47611.9 0 47624.8 3 2 0 2 1 0 0 42104.3 42104.3 95791.8 0 PROCESSED 55019.1754166667 55386 55019.1922337963 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041414 We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. EXTRAGALACTIC COMPACT SOURCES 7 A TREISTER EZEQUIEL NULL NULL USA 4 AO4 THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN XIS Y MRK1018 31.5471 -0.2351 159.73232745 -57.66458833 73.6945 55015.0121759259 55016.0939699074 704044010 43901.4 40000 43909.4 43901.4 0 43909.4 2 2 0 2 1 0 0 37688.4 37688.4 93457.8 5 PROCESSED 55027.0784606482 55395 55027.1070023148 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041414 We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. EXTRAGALACTIC COMPACT SOURCES 7 A TREISTER EZEQUIEL NULL NULL USA 4 AO4 THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN HXD Y MCG0208 43.0963 -8.5129 185.55840319 -55.88722126 57.4541 55016.0987037037 55017.2134722222 704045010 42911.5 40000 42943.5 42911.5 0 42919.5 2 2 0 2 1 0 0 36787.8 36787.8 96286 5 PROCESSED 55027.1008217593 55395 55027.1160532407 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041414 We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. EXTRAGALACTIC COMPACT SOURCES 7 A TREISTER EZEQUIEL NULL NULL USA 4 AO4 THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN XIS Y NGC1194 45.9522 -1.1044 179.17914291 -48.96176874 76.9913 55044.6911689815 55045.8141087963 704046010 50316.1 50000 50316.1 50596.1 0 50596.1 2 2 0 2 1 0 0 48426.8 48426.8 97003.8 1 PROCESSED 55061.5149768518 55427 55061.5275115741 2.4.12.26 2 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041414 We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. EXTRAGALACTIC COMPACT SOURCES 7 B TREISTER EZEQUIEL NULL NULL USA 4 AO4 THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN XIS Y NGC 4138 182.4434 43.7345 147.09151655 71.38668226 137.6226 55137.5331365741 55138.8849305556 704047010 60771.6 60000 60843.6 60771.6 0 60843.6 2 2 0 2 1 0 0 35872.4 35872.4 116781.8 2 PROCESSED 55151.1658912037 55517 55151.1923263889 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041415 The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 HXD Y NGC 3718 173.2341 53.1118 146.87581124 60.21394242 142.7392 55128.8497800926 55130.255775463 704048010 59888.2 60000 59920.2 59888.2 0 59920.2 2 2 0 2 1 0 0 52439.2 52439.2 121459.9 0 PROCESSED 55141.3074537037 55507 55141.3212384259 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041415 The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 4 AO4 SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 HXD Y SDSS J1352+4239 208.1832 42.6476 88.11360974 70.09649039 316.6443 54984.9959375 54985.7502199074 704050010 32074.5 30000 32082.5 32074.5 0 32082.5 2 2 0 2 1 0 0 29502.1 29502.1 65163.9 0 PROCESSED 54994.4134259259 55364 54994.4273032407 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041422 BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. EXTRAGALACTIC COMPACT SOURCES 7 A DAI XINYU NULL NULL USA 4 AO4 X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS XIS Y SDSS J1723+5553 260.8912 55.8942 83.89291292 34.34970174 8.0654 54986.3677777778 54986.8148032407 704051010 35936.8 30000 35944.8 35936.8 0 35952.8 1 1 0 1 1 0 0 29039.3 29039.3 38615.9 0 PROCESSED 54998.1671296296 55364 54998.1759722222 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041422 BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. EXTRAGALACTIC COMPACT SOURCES 7 A DAI XINYU NULL NULL USA 4 AO4 X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS XIS Y SDSS J0943+5417 145.8252 54.2751 161.23003018 46.41565232 274.2141 54975.5889236111 54976.3473611111 704052010 34226.4 30000 34226.4 34226.4 0 34226.4 2 2 0 2 1 0 0 32059.1 32059.1 65517.9 2 PROCESSED 54992.0635763889 55358 54992.6588888889 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041422 BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. EXTRAGALACTIC COMPACT SOURCES 7 A DAI XINYU NULL NULL USA 4 AO4 X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS XIS Y IC 2497 145.222 34.6799 190.267728 48.8163504 306.2341 54939.6906365741 54941.5550810185 704053010 76483.7 75000 76483.7 76483.7 0 76483.7 2 2 0 2 1 0 0 63948 63948 161047.8 2 PROCESSED 54952.1093981482 55318 54952.1320717593 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041432 The discovery of `Hanny's Voorwerp' near IC 2497 opens an unprecedented window into the time evolution of a single AGN on timescales up to 100,000 years. Based on its properties, the Voorwerp was illuminated by a luminous AGN ~100,000 years ago, but the AGN host galaxy - IC 2497 - does not seem to host a sufficiently luminous AGN. Thus, IC 2497 either hosts a highly obscured AGN only detectable in hard X-rays, or it has dropped in luminosity by a factor of 10-1000. We propose to observe IC 2497 with Suzaku for 75 ksec to determine the hard X-ray luminosity and spectrum to measure the amount of obscuration and the current intrinsic luminosity of its AGN. Only with hard X-ray observations can we break the degeneracy between obscuration and decrease in luminosity. EXTRAGALACTIC COMPACT SOURCES 7 A SCHAWINSKI KEVIN NULL NULL USA 4 AO4 HOW FAST CAN AN AGN SHUT DOWN? - SUZAKU OBSERVATION OF IC 2497 AND `HANNY'S VOORWERP' HXD Y MR 2251-178 343.5217 -17.5814 46.19628588 -61.32288878 63.4108 54958.1447222222 54961.4675231482 704055010 136924 130000 136932 136924 0 136939.9 2 2 0 2 1 0 0 112163.7 112163.7 287057.6 2 PROCESSED 54976.2703009259 55343 54976.3091782407 2.3.12.25 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042002 The bright, nearby (z=0.06398) QSO MR 2251-178 was the first AGN where a warm absorber was detected. There are now thought to be at least two warm absorber components in MR 2251-178; a low ionisation soft X-ray absorber and a putative high velocity (13000 km/s) high ionisation wind, which exhibits absorption lines in the iron K-shell band. We propose a 130 ks observation with Suzaku of MR 2251-178 with the primary goals; (i) to establish the nature of the high ionisation absorber, e.g. an accretion disk wind, through unprecedented high S/N observations in the iron K band with XIS; (ii) to determine the physical parameters of the soft X-ray warm absorber and (iii) to characterise the ionised reflection component and high-energy cut-off thanks to the high energy sensitivity of the HXD. EXTRAGALACTIC COMPACT SOURCES 7 A REEVES JAMES FUKAZAWA YASUSHI EUR 4 AO4 PROBING THE OUTFLOWING WIND IN MR 2251-178 XIS Y NGC4102 181.5322 52.6534 138.20676485 63.11040703 305.2196 54981.0678009259 54983.4203009259 704057010 105557.9 100000 105581.9 105557.9 0 105565.9 2 2 0 2 1 0 0 97280.2 97280.2 203213.9 2 PROCESSED 54994.4137037037 55363 54994.4413541667 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042014 The nature of Low Ionization Nuclear Emission-line Region (LINER) galaxies has been the subject of a strong controversy. The distinction between LINER nuclei and other families of Active Galactic Nuclei (AGN) can be due to different amounts and/or properties of the obscuring material. A high population of LINERs are Compton-thick candidates. However the Equivalent Width (EW) of the FeKa emission line are lower than those measured for Compton-thick AGN. We propose to use the unprecedented sensitivity of HXD and XIS on board Suzaku to study NGC4102, one of the brightest LINER in the 36-month Swift/BAT survey. NGC4102 is a Compton-thick LINER candidate with EW(FeKa)<500keV, it is therefore an ideal case to investigate the properties of absorption and the FeKa emission line. EXTRAGALACTIC COMPACT SOURCES 7 B GONZALEZ-MARTIN OMAIRA NULL NULL EUR 4 AO4 PROBING COMPTON-THICK OBSCURATION AND LOW EW(FEKA) OF LINERS: THE CASE OF NGC4102 HXD Y IRAS 04507+0358 73.3635 4.1233 194.58361833 -23.84576016 98.871 55075.0228356482 55078.1356481482 704058010 109052.4 100000 109052.4 109052.4 0 109052.4 2 2 0 2 1 0 0 84109.8 84109.8 268911.8 3 PROCESSED 55109.5111921296 55476 55109.5623842593 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042022 According to X-ray synthesis models, Compton-thick AGN (NH>1e24 cm-2) should represent 50% of the total absorbed AGN population. Despite their importance in the cosmological context, only a few of them have been found so far. We have selected a well-defined sample of 31 Compton-thick candidates on the basis on their FX/FIR and X-ray colors. Due to the heavy obscuration, data above 10 keV are fundamental to unveil these sources. We ask here deep Suzaku observations (100 ks on each source) for 2 sources of our sample for which data at energy >10keV are not available yet. These observations will allow to complete the physical characterization (NH and LX) of the bright tail (F(2-10 keV)>5e-12 cgs) of our sample and to add more information to test the prediction of the AGN synthesis model. EXTRAGALACTIC COMPACT SOURCES 7 B SEVERGNINI PAOLA NULL NULL EUR 4 AO4 SUZAKU OBSERVATIONS OF COMPTON-THICK CANDIDATES HXD Y IGR J22517+2218 342.9769 22.2871 89.68946946 -32.75751552 253.7359 55161.7610648148 55163.0086111111 704060010 52726.5 50000 52726.5 52726.5 0 52726.5 2 2 0 2 1 0 0 40116.4 40116.4 107777.9 0 PROCESSED 55179.2229166667 55545 55179.2471527778 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 042027 We propose to observe 4 high-z QSOs observed by INTEGRAL, two of which are newly discovered in hard X-rays. The broadband and the good energy resolution will allow to investigate the spectral behaviour at low energies, and in particular to constraint true absorption $vs$ continuum features scenario. Particularly intriguing is the possible presence of a bulk Compton motion component. A self consistent test of this model could be derived by measuring the peak energy of the Inverse Compton component in the SED, a requirement that further strenghtens the need of a broadband observation with Suzaku. Simultaneous optical, hard X and gamma-ray observations available through WEBT, INTEGRAL and AGILE will also improve the feasibility of the proposed program. EXTRAGALACTIC COMPACT SOURCES 7 B DE ROSA ALESSANDRA NULL NULL EUR 4 AO4 SUZAKU OBSERVATION A SAMPLE OF FOUR RADIO-LOUD/HIGH REDSHIFT QSOS OBSERVED BY INTEGRAL XIS Y NGC3516 166.8656 72.6213 133.14023939 42.38468378 135.8338 55132.2328125 55137.5272453704 704062010 251355.5 250000 251379.5 251371.5 0 251355.5 2 2 0 2 1 0 0 190837.2 190837.2 333010 5 PROCESSED 55152.2034259259 54922 55152.2729398148 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 4 AO4 A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN HXD Y NGC3783 174.7201 -37.7846 287.44066962 22.89477473 305.9228 55022.9100115741 55027.0016087963 704063010 209503.4 200000 209503.4 210311.4 0 210319.4 3 2 0 2 1 0 0 174040.4 174040.4 353453.5 2 PROCESSED 55040.5187152778 54922 55040.5612615741 2.4.12.26 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 046003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 4 AO4 A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN HXD Y 1H 0419-577 66.5658 -57.2343 267.01881665 -41.95465908 226.9739 55212.4834259259 55214.8224421296 704064010 122835.4 140000 123115.4 122835.4 0 123115.4 2 2 0 2 1 0 0 113439.2 113439.2 202066.8 4 PROCESSED 55228.1814236111 55594 55228.2152893518 2.4.12.27 1 Hea_01Apr2009_V6.6.2_Suzaku_23Mar2009_V12 041417 A 'hard excess' has been detected in 2007 Suzaku PIN data for the nearby quasar 1H 0419-577 relative to models fitting below 10 keV. The excess can be accounted for with Compton-thick partial-covering gas probably part of a clumpy disk wind originating inside of the BLR. The observed Fe Ka line luminosity is consistent with an origin in an equatorial wind. Blurred reflection models cannot satisfactorily fit the source and so 1H0419-577 provides a rare distinction between two observationally-similar classes of model. We propose two 140 ks follow-up Suzaku observations separated by months to probe the properties of the Compton-thick gas via variability measurements: this is an important new science area that can only be studied using the broad bandpass available from Suzaku. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 4 AO4 STUDYING THE COMPTON-THICK PARTIAL-COVERING ABSORPTION IN 1H 0419-577 HXD Y MRK 18 135.5092 60.0703 155.86471567 39.40052697 266.8203 55330.5025810185 55331.3772106482 705001010 37966.7 40000 37974.7 37974.7 0 37966.7 2 2 0 2 1 0 0 34667 34667 75553.9 1 PROCESSED 55403.058912037 55769 55403.0749768518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050003 We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 5 AO5 THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT HXD Y ARK 347 181.0952 20.2476 243.01628342 77.22827936 294.4295 55377.99625 55378.8668171296 705002010 38972.6 40000 38988.6 38972.6 0 38988.6 2 2 0 2 1 0 0 35987.6 35987.6 75209.9 0 PROCESSED 55404.2261689815 55772 55404.2387268518 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050003 We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 5 AO5 THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT HXD Y 1150+497 178.3624 49.5318 145.51949415 64.97605225 131.4133 55512.7136805556 55514.1042824074 705003010 105655.8 100000 105711.8 105655.8 0 105719.8 2 2 0 2 1 0 0 84643.8 84643.8 120128 1 PROCESSED 55524.2005671296 55892 55524.2197337963 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050007 A Suzaku observation of the iron line emitting blazar 1150+497 is proposed. The object is reported to exhibit a signature iron line. By measuring the equivalent width and line width, Suzaku will reveal the state of the accretion disc with the jet activity. It is notable that the blazar, aligning the jet with the line of sight, allow us to observe the jet and the accretion disc with a sufficient isochronism even with the violently variable sources. EXTRAGALACTIC COMPACT SOURCES 7 C SETA HIROMI NULL NULL JAP 5 AO5 SUZAKU OBSERVATION OF AN FE-LINE BLAZAR 1150+497 XIS Y MRK 78 115.67387 65.17708 151.07412774 29.78350067 -99 NULL NULL 705004010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050017 Monte Carlo simulation is one of the best tools to study the complex spectra of Compton-thick AGNs and to figure out the relation between their nuclear structures and X-ray spectra. We have simulated X-ray spectra of Compton-thick AGNs obscured by an accretion torus, and found that observed spectra of Compton thick objects, Mrk 3 and NGC 2273 are well reproduced by the simulated X-ray spectra. Furthermore, our simulation predicts that there are many obscured AGNs with a heavily absorbed reflection component. Their spectra are similar to that predicted from synthesis modeling of the Cosmic X-ray Background. We propose Suzaku observations of candidates of the Compton thick AGNs, Mrk 573 and Mrk 78. EXTRAGALACTIC COMPACT SOURCES 7 C AWAKI HISAMITSU NULL NULL JAP 5 AO5 SEARCH FOR COMPTON THICK AGNS WITH A HEAVILY ABSORBED REFLECTION COMPONENT HXD N PBC J0216.1+5124 34.0954 51.5104 136.13174863 -9.17115539 78.3815 55421.9728356482 55423.4168171296 705006010 72773.3 80000 72796.4 72773.3 0 72796.4 2 2 0 2 1 0 0 73558.2 73558.2 124725.8 3 PROCESSED 55435.279224537 55804 55435.2980092593 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050024 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5 BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y PBC J0839.7-1214 129.9392 -12.3029 237.21342575 17.37856511 291.8979 55324.6892824074 55326.4896990741 705007010 80564.3 80000 80564.3 80564.3 0 80564.3 2 2 0 2 1 0 0 70741.8 70741.8 155535.8 1 PROCESSED 55341.5420138889 55707 55341.5690856482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050024 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 5 AO5 BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND HXD Y ESO 428-G014 109.1256 -29.3248 241.87528565 -7.96864273 123.1273 55516.1372569445 55518.5508680556 705008010 82887.3 80000 82903.3 82887.3 0 82903.3 2 2 0 2 1 0 0 68451.8 68451.8 208501.6 2 PROCESSED 55530.2478703704 55898 55530.4256597222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050031 Non-Hidden Broad Line Region Seyfert 2 galaxies (NHBLR Sey2s) are classified as Seyfert 2 galaxies without broad Balmer lines even in the polarized light. One possible interpretation for the absence of broad lines is that NHBLR Sey2s are viewed from an extreme edge-on direction, so that the scattered light is obscured by the accretion torus. Hence observation of NHBLR Sey2s provides us the unique opportunity to investigate the densest region of the torus. We, therefore, propose 80 ksec observation of NHBLR Sey2 ESO 428-G014. High sensitivity throughout the 0.5-70 keV wide energy band of Suzaku allows us to strictly constrain the intrinsic X-ray luminosity and column density of the obscuring material. From our observation, we expect to derive more complete unified picture of AGNs. EXTRAGALACTIC COMPACT SOURCES 7 C HABA YOSHITO NULL NULL JAP 5 AO5 SUZAKU VIEW OF NON-HIDDEN BROAD LINE REGION SEYFERT 2 GALAXY ESO 428-G014 XIS Y IC 342 X2 56.516 68.1498 138.08335694 10.57829767 91.9969 55415.9786689815 55417.3765625 705009010 74379 80000 74379 74379 0 74379 2 2 0 2 1 0 0 64131.6 64131.6 120767.9 0 PROCESSED 55428.1371064815 55794 55428.1624537037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050041 The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection. EXTRAGALACTIC COMPACT SOURCES 7 A ISOBE NAOKI NULL NULL JAP 5 AO5 HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU XIS Y IC 342 X2 56.548 68.1243 138.10903546 10.56584534 237.0509 55640.3693981482 55641.8058101852 705009020 75446.7 80000 75470.7 75446.7 0 75478.7 2 2 0 2 1 0 0 74257.7 74257.7 124089.8 1 PROCESSED 55652.0001736111 56019 55652.0183680556 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050041 The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection. EXTRAGALACTIC COMPACT SOURCES 7 A ISOBE NAOKI NULL NULL JAP 5 AO5 HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU XIS Y EMS0071 16.6433 48.9425 125.49064727 -13.85403968 69.9406 55392.4123148148 55392.8855092593 705010010 23010.2 20000 23010.2 23010.2 0 23010.2 2 2 0 2 1 0 0 19568 19568 40881.9 0 PROCESSED 55411.2495138889 55779 55411.2637384259 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y EMS0857 198.1882 0.8497 314.828891 63.22804034 111.0249 55578.1935532407 55578.746087963 705011010 22070 20000 22078 22070 0 22085 1 1 0 1 1 0 0 15326.7 15326.7 47727.9 0 PROCESSED 55595.2268865741 55962 55595.4732986111 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y EMS1160 264.608 87.3047 120.03425165 27.94259409 59.9344 55312.9874537037 55313.4279513889 705012010 20279.6 20000 20279.6 20279.6 0 20279.6 2 2 0 2 1 0 0 19800.4 19800.4 38053.9 1 PROCESSED 55327.1454166667 55693 55327.1544791667 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y EMS1164 265.9438 -76.3446 317.07818058 -22.45515073 114.3984 55300.0111689815 55300.6980439815 705013010 42378.3 40000 42383.6 42378.3 0 42389 2 2 0 2 1 0 0 39048.7 39048.7 59343.9 1 PROCESSED 55309.1835763889 55675 55309.1947453704 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y EMS1274 285.5178 -51.1684 345.57919311 -22.40122796 103.8598 55299.2761921296 55300.0056944445 705014010 43925.3 40000 43925.3 43933.3 0 43933.3 2 2 0 2 1 0 0 34958.1 34958.1 63015.9 0 PROCESSED 55309.1975694444 55675 55309.2111458333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y EMS1395 310.8148 17.1786 61.89528011 -15.30299533 74.9546 55319.8076736111 55320.4342476852 705015010 23300.2 20000 23300.2 23300.2 0 23300.2 2 2 0 2 1 0 0 19494.4 19494.4 54129.9 0 PROCESSED 55330.188900463 55696 55330.2005208333 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y EMS1535 345.6918 44.7374 103.4061071 -13.97501662 63.3944 55373.2448611111 55374.0174768518 705016010 42395.5 40000 42403.5 42395.5 0 42403.5 1 1 0 1 1 0 0 42754.5 42754.5 66753.9 0 PROCESSED 55404.2109490741 55772 55404.2240625 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y 3C273 187.27792 2.05239 289.95088978 64.35997796 -99 NULL NULL 705017010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050052 We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5-TOO SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT XIS N 3C279 194.0465 -5.78931 305.10427142 57.06241024 -99 NULL NULL 705018010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050052 We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5-TOO SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT XIS N PKS1502+106 226.10408 10.49422 11.38195405 54.58061049 -99 NULL NULL 705019010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050052 We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5-TOO SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT XIS N PKS1510-089 228.21054 -9.09994 351.2892476 40.13876146 -99 NULL NULL 705020010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050052 We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5-TOO SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT XIS N 3C454.3 343.4951 16.1379 86.10833014 -38.194784 252.9263 55525.0494675926 55526.0141087963 705021010 41025.2 40000 41033.2 41033.2 0 41025.2 2 2 0 2 1 0 0 37141.2 37141.2 83327.8 0 PROCESSED 55550.1152199074 55916 55550.1355439815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050052 We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 5 AO5-TOO SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT XIS Y S5 0836+710 130.3515 70.895 143.54081046 34.42567625 -99 NULL NULL 705022010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050054 We propose intensive Suzaku observations of powerful gamma-ray blazar S5 0836+710 with 50ksec exposure. We stress that the sources will be monitored simultaneously by Fermi (GeV), Swift XRT/UVOT (UV to X-ray). We will obtain the broadband spectra from 10^9 Hz to 10^25 Hz. The proposed Suzaku observation will allow us to investigate EXTRAGALACTIC COMPACT SOURCES 7 C SATO RIE NULL NULL JAP 5 AO5 SUZAKU OBSERVATIONS OF BRIGHT GAMMA-RAY BLAZAR: S50836+710 HXD N LEDA 84274 220.5853 66.0952 106.75984756 47.40039166 359.2838 55331.3858333333 55332.0542824074 705023010 49465 50000 49465 49465 0 49465 2 2 0 2 1 0 0 40838.5 40838.5 57751.9 1 PROCESSED 55403.1108796296 55769 55403.1228125 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050074 We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy. EXTRAGALACTIC COMPACT SOURCES 7 B OYABU SHINKI NULL NULL JAP 5 AO5 SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI XIS Y IRAS 01250+2832 21.9819 28.787 132.5132824 -33.40495941 250.843 55571.3211805556 55572.5926388889 705024010 57582.9 50000 57582.9 57582.9 0 57582.9 2 2 0 2 1 0 0 54808.2 54808.2 109829.9 1 PROCESSED 55595.2069675926 55962 55595.2272569444 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050074 We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy. EXTRAGALACTIC COMPACT SOURCES 7 B OYABU SHINKI NULL NULL JAP 5 AO5 SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI XIS Y MRK 509 311.0469 -10.7401 35.95684044 -29.86794514 252.3716 55521.595625 55523.8155092593 705025010 102120.5 100000 102128.5 102128.5 0 102120.5 2 2 0 2 1 0 0 92062.5 92062.5 191769.7 0 PROCESSED 55550.2282407407 55916 55550.2628356482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050113 We propose the observation of one of the typical Seyferts I Mrk 509 for 100 ksec to understand how a vry hard component component that varies independently of power-law is created and how the physical structure near SMBH in Seyferts is. The hard component has been found by carrying out timing analysis of hard X-ray band to explain the extremely broad iron line feature of several Seyferts. Taking this component into account, we succeeded to explain the data of MCG 6-30-15 without the extremely broad iron line, though the origin of this component has not been identified yet. Because Mrk 509 has strong flux and large amplitude of hard X-ray variation, we found it is the most suitable object to verify this component and to get alternative interpretation to the extremely broad iron line. EXTRAGALACTIC COMPACT SOURCES 7 C NODA HIROFUMI NULL NULL JAP 5 AO5 VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509 XIS Y EMS0992 230.2572 -3.8213 358.15856297 42.46037658 113.2867 55593.7858564815 55594.1841898148 705026010 18979 20000 18979 18979 0 18979 3 2 0 2 1 0 0 14832 14832 34393.9 0 PROCESSED 55607.0347106482 55973 55607.0454976852 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050126 Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. EXTRAGALACTIC COMPACT SOURCES 7 C TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS1341 301.2467 70.0571 102.85714193 19.4440121 233.7732 55527.303275463 55527.7619675926 705027010 23066.8 20000 23066.8 23066.8 0 23066.8 1 1 0 1 1 0 0 21505.5 21505.5 39623.9 0 PROCESSED 55537.0081597222 55903 55537.0214814815 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050126 Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. EXTRAGALACTIC COMPACT SOURCES 7 C TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS1388 309.878 -56.3562 341.17879119 -37.12820094 256.6037 55497.456400463 55498.1383912037 705028010 21533.6 20000 21541.6 21541.6 0 21533.6 2 2 0 2 1 0 0 18373.5 18373.5 58909.9 0 PROCESSED 55508.975462963 55875 55508.9886342593 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050126 Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. EXTRAGALACTIC COMPACT SOURCES 7 C TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS0873 200.796 29.7234 55.1881509 82.55574598 136.0743 55527.7704976852 55528.2800231482 705029010 22784.9 20000 22784.9 22784.9 0 22784.9 1 1 0 1 1 0 0 20810.6 20810.6 44007.9 2 PROCESSED 55536.9722685185 55903 55536.9832523148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 050126 Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. EXTRAGALACTIC COMPACT SOURCES 7 C TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y EMS1360 272.619 17.725 44.60977416 16.83010742 -99 NULL NULL 705030010 -99 20000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 050126 Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. EXTRAGALACTIC COMPACT SOURCES 7 C TANAKA YASUYUKI NULL NULL JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES XIS N NGC 1365 53.3909 -36.1409 237.95774893 -54.60665436 30.5416 55374.0284143518 55377.9834606482 705031010 151613.4 450000 151629.4 151613.4 0 151621.4 2 2 0 2 1 0 0 123242.2 123242.2 341657.7 2 PROCESSED 55434.2082523148 55287 55434.2469444445 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051112 We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. EXTRAGALACTIC COMPACT SOURCES 7 A BRENNEMAN LAURA NULL NULL USA 5 AO5 A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS XIS Y NGC 1365 53.3976 -36.1412 237.95777124 -54.60123537 60.7695 55392.8956597222 55399.3676273148 705031020 302175.3 450000 302175.3 302183.3 0 302183.3 2 2 0 2 1 0 0 251061.2 251061.2 425533.9 2 PROCESSED 55413.7427083333 55287 55413.8216435185 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051112 We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. EXTRAGALACTIC COMPACT SOURCES 7 A BRENNEMAN LAURA NULL NULL USA 5 AO5 A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS XIS Y CEN A S LOBE NO. 1 200.8664 -45.1602 308.83796576 17.34395301 288.0039 55418.6612962963 55419.7758101852 705032010 75165.4 80000 75165.4 75165.4 0 75165.4 2 2 0 2 1 0 0 64272.8 64272.8 96281.8 0 PROCESSED 55428.1346759259 55803 55428.1537152778 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051401 We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). EXTRAGALACTIC COMPACT SOURCES 7 B MADEJSKI GRZEGORZ NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A XIS Y CEN A S LOBE NO. 2 200.3949 -45.1401 308.49497877 17.40582221 289.0008 55419.7766087963 55420.9641087963 705033010 81387.8 80000 81395.8 81387.8 0 81403.8 2 2 0 2 1 0 0 68108.5 68108.5 102585.8 0 PROCESSED 55445.2491203704 55812 55445.267662037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051401 We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). EXTRAGALACTIC COMPACT SOURCES 7 B MADEJSKI GRZEGORZ NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A XIS Y CEN A S LOBE NO. 3 205.7514 -45.1409 312.39292182 16.78143613 279.0007 55420.9668981482 55421.3452777778 705034010 20057.5 20000 20081.5 20073.5 0 20057.5 3 2 0 2 1 0 0 18943.6 18943.6 32687.9 1 PROCESSED 55435.15875 55803 55435.169537037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051401 We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). EXTRAGALACTIC COMPACT SOURCES 7 B MADEJSKI GRZEGORZ NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A XIS Y CEN A S LOBE NO. 4 196.751 -45.1436 305.81117883 17.64110832 288.0039 55421.3479282407 55421.67375 705035010 20642 20000 20642 20650 0 20658 1 1 0 1 1 0 0 18964.3 18964.3 28143.9 0 PROCESSED 55435.1489814815 55803 55435.1577314815 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051401 We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). EXTRAGALACTIC COMPACT SOURCES 7 B MADEJSKI GRZEGORZ NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A XIS Y 1RXS J111706.3+20141 169.2749 20.2432 225.56577108 67.37465885 120.2309 55510.3081944444 55511.1543402778 705036010 34212.5 32000 34212.5 34212.5 0 34212.5 2 2 0 2 1 0 0 31536.6 31536.6 73097.9 0 PROCESSED 55537.0802777778 55903 55537.0979050926 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051402 High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. EXTRAGALACTIC COMPACT SOURCES 7 C MASSARO FRANCESCO NULL NULL USA 5 AO5 X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS XIS Y 1RXS J044127.8+15045 70.36542 15.08169 183.04271359 -20.05970185 -99 NULL NULL 705037010 -99 32000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 051402 High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. EXTRAGALACTIC COMPACT SOURCES 7 C MASSARO FRANCESCO NULL NULL USA 5 AO5 X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS HXD N 1RXS J032613.6+02252 51.5615 2.4213 180.7494445 -42.4285339 253.9336 55596.8403356482 55597.6203125 705038010 32197.1 32000 32197.1 32197.1 0 32197.1 2 2 0 2 1 0 0 22644.1 22644.1 67387.9 1 PROCESSED 55614.1712731482 55983 55614.1886342593 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051402 High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. EXTRAGALACTIC COMPACT SOURCES 7 C MASSARO FRANCESCO NULL NULL USA 5 AO5 X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS XIS Y NGC 6251 248.2903 82.5391 115.75265542 31.17774629 182.5432 55532.2390625 55534.0341898148 705039010 87070.6 85000 87070.6 87070.6 0 87070.6 2 2 0 2 1 0 0 75807.4 75807.4 155087.9 1 PROCESSED 55565.3467476852 55931 55565.375162037 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051411 We propose an 85-ks Suzaku observation of NGC 6251, the brightest example of a low-excitation radio galaxy (LERG). We have previously suggested that LERGs violate conventional AGN unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. However, Suzaku observations at low and high energies are needed to test this model directly. We will use the XIS and HXD to search for the signatures of accretion-related X-ray emission: (1) the 6.4 keV Fe Ka line, (2) heavily absorbed X-ray emission, and (3) the >10 keV Compton reflection bump. These results will have important implications for models of accretion and feedback in radio-loud AGN. EXTRAGALACTIC COMPACT SOURCES 7 C EVANS DANIEL NULL NULL USA 5 AO5 A DIRECT TEST OF THE NUCLEAR X-RAY DICHOTOMY IN RADIO-LOUD AGN XIS Y 3C111 64.5838 38.0364 161.66578558 -8.81556542 79.7358 55441.1593055556 55442.8995138889 705040010 80683 80000 80691 80683 0 80691 2 2 0 2 1 0 0 73370.7 73370.7 150307.9 1 PROCESSED 55456.1927199074 55822 55456.2202430556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051412 Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. EXTRAGALACTIC COMPACT SOURCES 7 A SAMBRUNA RITA NULL NULL USA 5 AO5 PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU XIS Y 3C111 64.5838 38.0341 161.66743119 -8.81719194 77.8463 55448.0268865741 55449.7585416667 705040020 79419.8 80000 79419.8 79419.8 0 79419.8 2 2 0 2 1 0 0 71809 71809 149605.8 0 PROCESSED 55461.2832060185 55827 55461.3122106482 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051412 Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. EXTRAGALACTIC COMPACT SOURCES 7 A SAMBRUNA RITA NULL NULL USA 5 AO5 PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU XIS Y 3C111 64.5838 38.0329 161.66828978 -8.81804056 76.1726 55453.9599768518 55455.7432986111 705040030 80365.9 80000 80381.9 80365.9 0 80381.9 2 2 0 2 1 0 0 70953.3 70953.3 154063.9 2 PROCESSED 55469.3410185185 55835 55469.3718287037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051412 Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. EXTRAGALACTIC COMPACT SOURCES 7 A SAMBRUNA RITA NULL NULL USA 5 AO5 PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU XIS Y PDS 456 262.0809 -14.2537 10.4015562 11.17111116 96.1694 55636.625462963 55639.3564930556 705041010 125527.2 130000 125535.2 125527.2 0 125532.7 2 2 0 2 1 0 0 100875 100875 235927.6 2 PROCESSED 55677.2758680556 56050 55677.3183564815 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051421 PDS 456 is the most luminous nearby AGN and a recent Suzaku observation revealed a powerful ionized outflow moving at 0.25c with kinetic output matching the quasar bolometric luminosity. Above 10 keV the HXD appears to show a factor 3 rise in flux over the XIS, implying that a high column density absorber (>10^24 cm^-2) is located close to the X-ray source in order to partially covers its emission. We propose to study the remarkable X-ray absorption towards PDS 456 through two further 130 ks Suzaku observations. This will:-i) confirm the nature of the hard excess, ii) determine whether spectral variability can be explained by variable partial covering and iii) enable us to measure the imprint of the ionized outflow at Fe K with unprecedented accuracy. EXTRAGALACTIC COMPACT SOURCES 7 B TURNER TRACEY NULL NULL USA 5 AO5 THE COMPTON-THICK OUTFLOW IN THE TYPE I QSO PDS 456 XIS Y CBS 126 153.2712 35.8701 188.30426979 55.38335717 124.145 55487.3144907407 55489.5529861111 705042010 101542 100000 101566 101542 0 101566 2 2 0 2 1 0 0 90743.8 90743.8 193389.7 2 PROCESSED 55498.2908449074 55867 55498.3270949074 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051432 We propose to carry out a 100 ks Suzaku observation of Broad Line Seyfert 1 (BLS1) galaxy CBS 126. This source exhibits many properties which are thought to be typical of a Narrow Line Seyfert 1 (NLS1), such as a large soft X-ray excess and strong spectral variability, but unusual for a BLS1. Taking advantage of Suzaku's unique broad band X-ray energy window, our main goal is to clarify the nature of the unusual, variable, optically polarized spectrum of CBS 126. These interesting spectral features cover a wide energy range where Suzaku is ideal. With these proposed studies we will gain better understanding of accretion-powered AGN in general. EXTRAGALACTIC COMPACT SOURCES 7 B TSURUTA SACHIKO NULL NULL USA 5 AO5 SPECTRAL AND TEMPORAL STUDIES OF THE SEYFERT 1 GALAXY CBS 126 XIS Y MKN 590 33.6446 -0.7698 163.50990373 -56.94179664 250.4206 55584.0937615741 55585.6252083333 705043010 61554.7 150000 61586.7 61554.7 0 61570.7 2 2 0 2 1 0 0 55159.9 55159.9 132275.8 0 PROCESSED 55599.1698611111 55965 55599.1867824074 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051433 We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. EXTRAGALACTIC COMPACT SOURCES 7 C RIVERS ELIZABETH NULL NULL USA 5 AO5 QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 XIS Y MKN 590 33.6477 -0.7713 163.51612886 -56.94122484 251.1273 55587.0949652778 55588.2146990741 705043020 40913.9 150000 40921.9 40921.9 0 40913.9 2 2 0 2 1 0 0 37869.9 37869.9 96733.9 1 PROCESSED 55621.1939699074 55988 55621.2137731482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051433 We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. EXTRAGALACTIC COMPACT SOURCES 7 C RIVERS ELIZABETH NULL NULL USA 5 AO5 QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 XIS Y NGC 526A 20.9794 -35.0729 263.77547728 -79.45131683 257.0195 55578.7592939815 55580.6404050926 705044010 72934.6 70000 72934.6 72934.6 0 72934.6 2 2 0 2 1 0 0 63137.2 63137.2 162497.7 2 PROCESSED 55595.3555208333 55961 55595.4905671296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051434 The Compton-thin NELG NGC 526a has large hard X-ray variability and likely an abnormally flat photon index, Gamma near 1.6. We request two observations of 70 ks each, spaced six months apart, to accurately constrain Compton reflection and obtain geometrical constraints on the accreting material to test Seyfert unification schemes, as well as constrain coronal power law parameters. Importantly, we will track long-term spectral variability to constrain the location and nature of the reflecting material. We also will resolve the moderately broad Fe K alpha line, which may indicate the presence of a truncated accretion disk, and thus constrain the amount of reflection off an accretion disk versus that from a torus. EXTRAGALACTIC COMPACT SOURCES 7 C MARKOWITZ ALEX NULL NULL USA 5 AO5 COMPTON REFLECTION AND LONG-TERM SPECTRAL VARIABILITY IN THE SEYFERT AGN NGC 526A XIS Y IRAS 12072-0444 182.4393 -5.0116 283.97337665 56.31820605 111.9489 55534.0444328704 55535.5169328704 705045010 61933.9 60000 61941.9 61941.9 0 61933.9 2 2 0 2 1 0 0 28159.6 28159.6 127206 0 PROCESSED 55544.2668171296 55910 55544.3011226852 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051441 We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. EXTRAGALACTIC COMPACT SOURCES 7 C RISALITI GUIDO NULL NULL USA 5 AO5 BURIED QUASAR 2S INSIDE ULIRGS XIS Y IRAS 00397-1312 10.5707 -12.9503 113.89016485 -75.66108211 246.4295 55558.1361342593 55560.2501388889 705046010 83792.8 90000 83792.8 83792.8 0 83792.8 2 2 0 2 1 0 0 71931.4 71931.4 182631.7 1 PROCESSED 55670.328587963 56040 55670.3615046296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051441 We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. EXTRAGALACTIC COMPACT SOURCES 7 C RISALITI GUIDO NULL NULL USA 5 AO5 BURIED QUASAR 2S INSIDE ULIRGS XIS Y NGC 4945 196.3459 -49.5284 305.256234 13.28040137 283.285 55381.636087963 55382.6765856482 705047010 39073.7 40000 39081.7 39081.7 0 39073.7 1 1 0 1 1 0 0 34075.1 34075.1 89871.9 1 PROCESSED 55404.2545833333 55770 55404.2681134259 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051442 We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. EXTRAGALACTIC COMPACT SOURCES 7 B RISALITI GUIDO NULL NULL USA 5 AO5 HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 HXD Y NGC 4945 196.3415 -49.5274 305.25336122 13.28155854 286.7821 55386.9936226852 55388.2626388889 705047020 44151.7 40000 44151.7 44159.7 0 44151.7 2 2 0 2 1 0 0 40161.2 40161.2 109434 0 PROCESSED 55411.2137847222 55777 55411.4916898148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051442 We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. EXTRAGALACTIC COMPACT SOURCES 7 B RISALITI GUIDO NULL NULL USA 5 AO5 HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 HXD Y NGC 4945 196.3265 -49.5207 305.24375345 13.28878787 296.6587 55403.0670717593 55404.1745717593 705047030 40326.6 40000 40342.6 40326.6 0 40342.6 2 2 0 2 1 0 0 34618.2 34618.2 95635.8 0 PROCESSED 55414.064537037 55780 55414.0832407407 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051442 We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. EXTRAGALACTIC COMPACT SOURCES 7 B RISALITI GUIDO NULL NULL USA 5 AO5 HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 HXD Y NGC 4945 196.2918 -49.5144 305.2209968 13.29631795 319.7988 55438.8990277778 55439.9896990741 705047040 39385.9 40000 39385.9 39385.9 0 39385.9 2 2 0 2 1 0 0 35782.3 35782.3 94223.9 0 PROCESSED 55449.2384953704 55815 55449.2596296296 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051442 We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. EXTRAGALACTIC COMPACT SOURCES 7 B RISALITI GUIDO NULL NULL USA 5 AO5 HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 HXD Y NGC 4945 196.3636 -49.4659 305.27160994 13.34216317 120.2557 55590.0873842593 55591.1182175926 705047050 46107.6 40000 46107.6 46107.6 0 46107.6 2 2 0 2 1 0 0 54090.7 54090.7 89051.8 0 PROCESSED 55602.208912037 55969 55602.2238194445 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051442 We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. EXTRAGALACTIC COMPACT SOURCES 7 B RISALITI GUIDO NULL NULL USA 5 AO5 HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 XIS Y ESP 39607 11.5922 -40.0968 307.24150307 -76.98900447 243.1952 55549.7680208333 55551.3175810185 705048010 60668.7 60000 60692.7 60668.7 0 60684.7 2 2 0 2 1 0 0 48955.5 48955.5 133839.9 3 PROCESSED 55593.2059259259 55960 55593.2278472222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051443 We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. EXTRAGALACTIC COMPACT SOURCES 7 C BAUMGARTNER WAYNE NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS XIS Y SWIFTJ2344.6-424322 356.1059 -42.7624 339.65324523 -69.27134863 225.0657 55505.2812731482 55506.5570601852 705049010 61741.6 60000 61741.6 61741.6 0 61741.6 2 2 0 2 1 0 0 50394.1 50394.1 110211.8 1 PROCESSED 55518.2908912037 55885 55518.3162847222 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051443 We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. EXTRAGALACTIC COMPACT SOURCES 7 C BAUMGARTNER WAYNE NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS XIS Y 3C 433 320.9422 25.055 74.46917661 -17.70913692 252.1178 55506.5663310185 55508.0953472222 705050010 62500.9 60000 62540 62500.9 0 62540 2 2 0 2 1 0 0 44427.1 44427.1 132069.8 0 PROCESSED 55524.1249305556 55890 55524.1485416667 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051443 We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. EXTRAGALACTIC COMPACT SOURCES 7 C BAUMGARTNER WAYNE NULL NULL USA 5 AO5 SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS XIS Y NGC 4258 184.7518 47.3153 138.28789039 68.83430148 139.1798 55511.1601388889 55512.7112615741 705051010 103833.2 100000 103833.2 103841.2 0 103837 2 2 0 2 1 0 0 86225.7 86225.7 133968.8 1 PROCESSED 55537.1528587963 55903 55537.1754398148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 051451 We request a 100 ksec observation of the Low Luminosity AGN NGC 4258. This observation is meant to complement our existing 100 ksec Suzaku observation (Reynolds et al. 2009), and our 320 ksec Chandra-HETG observation (Murphy et al., in prep.). The goal is to further characterize the observed variability of the Fe Kalpha line and any associated changes in the continuum and/or absorption of NGC 4258. Given the unique constraints that we have on the mass, distance and accretion flow geometry in NGC 4258, as well as its role as a bridge between the most quiescent nuclei and powerful AGN, further Suzaku studies of NGC 4258 are clearly warranted. EXTRAGALACTIC COMPACT SOURCES 7 C NOWAK MICHAEL NULL NULL USA 5 AO5 HUNTING FOR THE VARIABLE IRON LINE IN NGC 4258 XIS Y MCG-03-58-007 342.3795 -19.2152 42.20057234 -60.96689333 68.5139 55350.7016203704 55352.8940046296 705052010 99087.3 100000 99087.3 99087.3 0 99087.3 2 2 0 2 1 0 0 81420 81420 189406 1 PROCESSED 55365.5047916667 55734 55365.563912037 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052011 Despite their relevance, less than two dozens of confirmed Compton-thick (CT) AGN have been found so far. We have recently selected a well defined sample of CT AGN candidates using FX/Fir ratios and X-ray colors. Due to their heavy obscuration, good statistics at 6.4 keV and data above 10 keV are needed to assess the real nature of these sources. We propose deep Suzaku observations (100 and 150 ks) for two sources for which data above 10 keV are not available and the quality of XMM data is poor. This request is a continuation of an approved AO4 proposal. These observations will allow us to possibly unveil two more examples of CT AGN, provide a physical characterization of the relatively bright tail of our sample, and estimate the efficiency of our method in selecting CT AGN. EXTRAGALACTIC COMPACT SOURCES 7 A SEVERGNINI PAOLA NULL NULL EUR 5 AO5 SUZAKU OBSERVATIONS OF TWO COMPTON-THICK CANDIDATES HXD Y NGC 3147 154.2433 73.3869 136.29780832 39.47682975 262.9224 55340.8248611111 55343.2925231482 705054010 150047.6 150000 150047.6 150055.6 0 150055.6 2 2 0 2 1 0 0 132913.6 132913.6 213181.8 2 PROCESSED 55393.4344212963 55765 55393.4710648148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052013 NGC3147 is the best candidate to be a true Seyfert 2, i.e., with no BLR. We propose a 150 ks observation with Suzaku to study the Fe line profile which in the short XMM-Newton observation shows some structure. If the iron line will turn out to be originated from the accretion disc, the lack of the BLR cannot be attributed to the lack of ionizing photons; if originated from the torus, this would put constraints on models assuming a common origin for the torus and the BLR; if the presence of an ionized iron line is confirmed, a BLR might exist but so highly ionized to be invisible at optical/UV wavelengths. An important added value of this observation is to confirm NGC3147 as a true Seyfert 2 by ruling out a Compton-thick nature, which only Suzaku can do thanks to its hard X-ray coverage. EXTRAGALACTIC COMPACT SOURCES 7 B MATT GIORGIO NULL NULL EUR 5 AO5 SUZAKU OBSERVATION OF THE BEST ``TRUE SEYFERT 2'' GALAXY CANDIDATE, NGC 3147 XIS Y IGR J19378-0617 294.4023 -6.2869 32.53385066 -13.11752642 260.9167 55485.0705324074 55487.3016087963 705055010 77801.4 80000 77817.4 77801.4 0 77817.4 2 2 0 2 1 0 0 70571.2 70571.2 192743.9 1 PROCESSED 55498.2109837963 55867 55498.2386805556 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052014 We propose to observe with Suzaku three Narrow Line Seyfert 1 galaxies detected by INTEGRAL/IBIS and/or Swift/BAT with a flux in excess of 1.5e-11 cgs in the 15-50keV band (corresponding to the HXD/PIN band). The proposed observations will provide rare high quality spectra of NLS1s in the 0.5-50keV band. The good quality data above 10keV will dramatically help us removing the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM-Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources. EXTRAGALACTIC COMPACT SOURCES 7 A MINIUTTI GIOVANNI NULL NULL EUR 5 AO5 BROADBAND X-RAY PROPERTIES OF HARD-X-RAY-BRIGHT NLS1 GALAXIES HXD Y 4U 1344-60 206.8966 -60.619 309.76861534 1.50528265 97.6008 55572.7924189815 55575.4751273148 705058010 93877.3 100000 93901.3 93893.3 0 93877.3 2 2 0 2 1 0 0 79561.7 79561.7 231753.7 3 PROCESSED 55607.3672569444 55975 55607.6933333333 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052018 We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. EXTRAGALACTIC COMPACT SOURCES 7 C SVOBODA JIRI NULL NULL EUR 5 AO5 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE XIS Y CENTAURUS B 206.7018 -60.4061 309.72060452 1.73379394 97.6796 55572.6060763889 55572.7919444444 705059010 8761.1 10000 8769.1 8769.1 0 8761.1 1 1 0 1 1 0 0 6452.6 6452.6 16055.9 0 PROCESSED 55595.2007175926 55962 55595.2069675926 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052018 We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. EXTRAGALACTIC COMPACT SOURCES 7 C SVOBODA JIRI NULL NULL EUR 5 AO5 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE XIS Y S5 0014+813 4.28529 81.58558 121.61133863 18.8019055 -99 NULL NULL 705060010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 052019 We propose to perform SUZAKU observations of the extreme hard-X-ray blazars S5 0014+813 and GB6 0805+614, detected in the Swift-BAT survey. Both objects have z>3 and are among the most powerful known, with very massive central black hole and accretion luminosities near the Eddington limit. Simultaneous soft and hard X-ray and MeV-GeV observations are a powerful tool to study the bulk emission of the jet of these objects. Combined optical-UV emission will provide the related information of the thermal emission of the disk. The SUZAKU data, together with the simultaneous public LAT data and a series of short Swift observations, will allow us to gather important insight into the structure of the emission regions and the physical processes producing both the thermal and non-thermal radiation. EXTRAGALACTIC COMPACT SOURCES 7 C TAGLIAFERRI GIANPIERO NULL NULL EUR 5 AO5 THE BLAZARS WITH THE MOST POWERFUL JETS AND THE MOST MASSIVE BLACK HOLE: TESTING THE BULK OF THEIR EMISSION WITH SUZAKU HXD N MRK 205 185.2459 75.2485 125.52269394 41.72619699 309.3435 55338.764849537 55340.8203125 705062010 100960.5 126000 100968.5 100960.5 0 100968.5 2 2 0 2 1 0 0 91952.5 91952.5 177577.8 0 PROCESSED 55355.2064467593 55723 55355.4313773148 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 052026 Mrk 205 (z=0.071) is a ``bare'' radio-quiet quasar, showing a peculiar continuum and FeK complex. From our analysis of past XMM-Newton observations, it shows a prominent and variable soft excess down to a two-day timescale. In 2000, an unusual FeK profile was found with an unresolved narrow line at 6.4keV and a broadened line centered at 6.7keV; while in 2006 a broad line has been observed near 6.4keV with a visible energy shift to 6.5keV occurring when the source flux increased. Our aims are to: (i) determine the FeK origin from its profile, and its possible variability on sub-orbital time-scales, (ii) to obtain an unprecedented simultaneous measurement of the Compton hump which is critical for modelling the true FeK profile (iii) and hence to infer a global picture of this object. EXTRAGALACTIC COMPACT SOURCES 7 B PORQUET DELPHINE NULL NULL EUR 5 AO5 PROBING THE ORIGIN OF THE FEK COMPLEX IN THE ``BARE'' NUCLEUS OF MRK205. HXD Y FAIRALL 9 20.848 -58.7784 295.14856402 -57.86436534 32.7271 55335.1255671296 55338.764837963 705063010 229296.3 250000 229302 229302 0 229296.3 2 2 0 2 1 0 0 174941.2 174941.2 288656 1 PROCESSED 55434.3783101852 55287 55434.4437615741 2.5.16.28 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 056003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 5 AO5 A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN HXD Y 1FGL J1311.7-3429 197.9423 -34.512 307.68226276 28.17214982 298.263 55774.7002314815 55776.7362847222 706001010 82477.1 80000 82477.1 82477.1 0 82477.1 2 2 0 2 1 0 0 70373.7 70373.7 175863.8 2 PROCESSED 55851.268275463 56219 55851.4595601852 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060003 We propose Suzaku observations of "unusual" Fermi-LAT sources 1FGL J1311.7 and 1FGL J2339.7, which are extremely bright in gamma-ray (> 30 sigma detection), but are as-yet unidentified even after two-year accumulation of Fermi-LAT data. Previous Suzaku observation revealed a highly variable X-ray source at the position of 1FGL J1311.7, but both spectral and temporal features do not resemble that of blazars or the gamma-ray pulsars. Meanwhile, an X-ray counterpart of 1FGL J2339.7 shows extremely hard spectrum with its photon index 1.1, which seems to connect smoothly with a bump feature around 2GeV. We will characterize variability and spectral properties of these peculiar X-ray counterparts and firmly understand the nature/origin of "new-type" GeV gamma-ray sources. EXTRAGALACTIC COMPACT SOURCES 7 B KATAOKA JUN NULL NULL JAP 6 AO6 SUZAKU OBSERVATIONS OF "NEW-TYPE'' GAMMA-RAY SOURCES DETECTED WITH FERMI-LAT XIS Y NGC6251_LOBE 246.4248 82.6439 116.00587189 31.32598662 26.9674 55666.2760069444 55667.0258564815 706003010 38077.9 40000 38077.9 38077.9 0 38077.9 2 2 0 2 1 0 0 37527.6 37527.6 64784 0 PROCESSED 55690.977962963 56058 55690.9897685185 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060004 We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 XIS Y NGC6251_LOBE_BGD1 247.6537 82.9256 116.18672095 31.0445068 26.9624 55667.0269328704 55667.4328125 706004010 18822 20000 18835.7 18822 0 18835.6 3 2 0 2 1 0 0 18957.2 18957.2 35065.9 1 PROCESSED 55691.0799305556 56058 55691.0888194444 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060004 We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 XIS Y NGC6251_LOBE_BGD2 245.2973 82.3586 115.82251183 31.60630628 26.9772 55667.4343981482 55667.8230902778 706005010 12010.3 20000 12018.3 12010.3 0 12026.3 1 1 0 1 1 0 0 17585.1 17585.1 33575.9 0 PROCESSED 55690.9723263889 56058 55690.9834490741 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060004 We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 XIS Y NGC6251_LOBE_BGD2 245.3877 82.3337 115.79036875 31.61025625 299.99 55789.4176967593 55789.6225 706005020 11178 10000 11178 11178 0 11178 1 1 0 1 1 0 0 9788 9788 17687.9 0 PROCESSED 55805.1809722222 56173 55805.1871527778 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060004 We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. EXTRAGALACTIC COMPACT SOURCES 7 A KATAOKA JUN NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 XIS Y 1ES 1927+654 291.8157 65.5862 97.0030083 20.97400385 83.4311 55667.8280092593 55669.2425115741 706006010 71888.9 100000 71912.9 71888.9 0 71912.9 2 2 0 2 1 0 0 79664.7 79664.7 122191.9 0 PROCESSED 55691.253912037 56059 55691.2683912037 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060008 1ES 1927+654, an X-ray unabsorbed optically classified type-2 AGN, challenges the standard unified model. What is known about its X-ray characteristics suggest it can provide tremendous insight. It is extremely bright and will render close to 20 ct/s in the combined XIS providing sufficient data to unambiguously detect features in the Fe~K region, distinguish absorption and reflection models, and study its rapid variability. Even in the most conservative estimates a PIN detection is expected. It is persistently variable on short time scales and in combination with the long duration of Suzaku observations, the proposed observationswill yield fruitful variability studies. It has never been observed by Suzaku thus guaranteeing significant opportunity for discovery. EXTRAGALACTIC COMPACT SOURCES 7 B GALLO LUIGI NULL NULL JAP 6 AO6 REVEALING THE NATURE OF AN X-RAY ABSORBED SEYFERT 2 XIS Y HESS J1943+213 295.9916 21.301 57.76229591 -1.30331963 246.7107 55875.6293055556 55876.6015393518 706007010 38881.5 40000 38881.5 38889.5 0 38889.5 2 2 0 2 1 0 0 35313 35313 83972 1 PROCESSED 55890.4825462963 56256 55890.6970833333 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060028 A new point-like source HESS J1943+213 has been detected at TeV energies at the position coinciding with the unidentified hard X-ray objects IGR J19443+2117. All the available observational constraints favor an identification of HESS J1943+213 as a BL Lac at redshift z>0.14. If correct, this would be the first time an AGN is discovered serendipitously from TeV observations in the Galactic Plane. It would be also the most extreme BL Lac known, with the persistent synchrotron continuum extending up to the observed energies >100 keV. A good quality broad X-ray spectrum is needed to confirm the blazar association and the extreme character of the peculiar object HESS J1943+213. Here we argue that a relatively moderate Suzaku exposure of 40 ksec will enable us to obtain such a spectrum. EXTRAGALACTIC COMPACT SOURCES 7 C STAWARZ LUKASZ NULL NULL JAP 6 AO6 PECULIAR UNIDENTIFIED TEV SOURCE HESS J1943+213 IN THE GALACTIC PLANE: EXTREME BLAZAR OR SOMETHING ELSE? XIS Y SWIFT J0709.4-3559 107.3109 -36.0226 247.327711 -12.25710974 260.0142 55653.0945601852 55655.0640393518 706008010 81173.9 80000 81173.9 81173.9 0 81173.9 2 2 0 2 1 0 0 61462.1 61462.1 170123.9 2 PROCESSED 55670.2214699074 56037 55670.2451967593 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060030 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6 BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND XIS Y SWIFT J1310.9-5553 197.6868 -55.8722 305.6577855 6.89731776 290.4478 55761.4489467593 55762.6432523148 706009010 82785 80000 82793 82785 0 82785 2 2 0 2 1 0 0 67508.1 67508.1 103177.9 1 PROCESSED 55845.2296527778 56213 55845.247662037 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060030 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 6 AO6 BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND XIS Y 2MASX J15115979-2119 227.9997 -21.3083 341.57056512 30.81939061 105.6253 55979.0551388889 55980.937650463 706010010 83816.2 80000 83816.2 83816.2 0 83816.2 2 2 0 2 1 0 0 82256.8 82256.8 162635.9 1 PROCESSED 55995.1388888889 56361 55995.1640393518 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060032 We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 6 AO6 ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S XIS Y WKK 4438 223.82254 -51.57083 321.71542855 6.72677341 -99 NULL NULL 706011010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060032 We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 6 AO6 ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S XIS Y IC 4518A 224.42158 -43.13211 326.11379055 13.98506276 -99 NULL NULL 706012010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060040 We propose to observe the Compton-thin AGN IC 4518A with a very small L_X/L_IR ratio, which has often been employed as an indicator of the presence of a Compton-thick AGN. Our aim is to examine the recent argument that L_X/L_IR is not a good measure of absorption column densities and that this ratio is more dependent on the covering fraction of absorber and intrinsic spectral shape. We measure the spectral slope, covering fraction, and NH, and compare them with the prediction of Monte-Carlo simulations to test the validity of L_X/L_IR as a measure of Compton thickness. EXTRAGALACTIC COMPACT SOURCES 7 C HIRATA YOSHITAKA NULL NULL JAP 6 AO6 BROAD-BAND SPECTRA OF THE COMPTON-THIN AGN IC 4518A WITH A SMALL L_X/L_IR: TESTING VALIDITY OF A COMPTON-THICK INDICATOR XIS Y 3C78 47.1071 4.1138 174.85308943 -44.51284685 84.4195 55793.5846990741 55795.7502430556 706013010 97012.2 100000 97012.2 97012.2 0 97012.2 3 2 0 2 1 0 0 85907.5 85907.5 187087.8 0 PROCESSED 55806.3682407407 56176 55806.3891435185 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060046 We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others. EXTRAGALACTIC COMPACT SOURCES 7 B FUKAZAWA YASUSHI NULL NULL JAP 6 AO6 ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 XIS Y PKS0625-354 96.7724 -35.4904 243.45420005 -19.97253333 121.4596 55868.6502199074 55871.6231597222 706014010 100719.8 100000 100727.8 100727.8 0 100719.8 2 2 0 2 1 0 0 86434.2 86434.2 256813.8 4 PROCESSED 55881.2463310185 56250 55881.2887731482 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060046 We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others. EXTRAGALACTIC COMPACT SOURCES 7 B FUKAZAWA YASUSHI NULL NULL JAP 6 AO6 ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 XIS Y 3C 98 59.723 10.4395 179.82925767 -31.05249617 81.003 55812.5811342593 55815.280787037 706015010 101144 100000 101144 101144 0 101144 2 2 0 2 1 0 0 89838.9 89838.9 233214 3 PROCESSED 55848.3131712963 56218 55851.4528356482 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060055 Whether radio-loud and radio-quiet AGN may be unified under one model is still open to debate. The most important limitation in such work is that jet beaming swamps nuclear emission, so we must study powerful radio sources which are not affected by this bias. These are the Narrow Line Radio Galaxies (NLRGs). Heavy obscuration means that their primary emission is visible only above 10 keV. 3C 98 is an important member of the NLRG class because its hard band power dominates the full radio to X-ray core luminosity. We propose a 100 ks observation of this source with Suzaku to detect the core continuum emission and reflection above 10 keV. 3C~98 is one of few NLRGs for which we can expect to model (rather than just detect) the hard X-ray flux, and hence use it for testing unification schemes. EXTRAGALACTIC COMPACT SOURCES 7 B GANDHI POSHAK NULL NULL JAP 6 AO6 HARD X-RAY EMISSION AND REFLECTION IN RADIO GALAXIES: 3C 98 XIS Y I ZW 1 13.39167 12.69333 123.74259367 -50.17506794 -99 NULL NULL 706016010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060069 Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. EXTRAGALACTIC COMPACT SOURCES 7 C SAMESHIMA HIROAKI NULL NULL JAP 6 AO6 X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION XIS Y PG 1626+554 247.0224 55.3701 84.50112094 42.16849703 200.5289 55876.6090046296 55877.9341550926 706017010 60848.8 60000 60848.8 60848.8 0 60848.8 2 2 0 2 1 0 0 56132.8 56132.8 114463.9 2 PROCESSED 55890.4949074074 56256 55890.6981828704 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060069 Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. EXTRAGALACTIC COMPACT SOURCES 7 C SAMESHIMA HIROAKI NULL NULL JAP 6 AO6 X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION XIS Y PG 1322+659 200.9787 65.7065 117.62442893 51.08576313 141.5827 55892.4154050926 55894.0862268518 706018010 81686.9 80000 81710.9 81686.9 0 81710.9 2 2 0 2 1 0 0 78916.8 78916.8 144343.9 2 PROCESSED 55907.1744328704 56274 55907.1929282407 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060069 Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. EXTRAGALACTIC COMPACT SOURCES 7 C SAMESHIMA HIROAKI NULL NULL JAP 6 AO6 X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION XIS Y NGC 5252 204.56625 4.5425 331.29811657 64.80324027 -99 NULL NULL 706022010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060074 The Eddington ratio (L/LEdd) is the most fundamental observable describing accretion activity. There are claims that the X-ray spectral shape (Gamma) may be used as a proxy of L/LEdd. But the Gamma-L/LEdd correlation also shows some hard spectrum sources as being clear outliers, so the validity of such a correlation needs confirmation. We propose to study 3 outliers to understand the origin of their hard spectral indices. The targets are amongst the bright outlier population, and hence will be detectable above 10 keV with Suzaku. This will enable us to search for signatures distinguishing between various physical scenarios, including intrinsically low-luminosity AGN or heavy obscuration. EXTRAGALACTIC COMPACT SOURCES 7 C HAGINO KOUICHI NULL NULL JAP 6 AO6 ELUCIDATING THE NATURE OF AGNS HAVING UNUSUALLY HARD ENERGY SPECTRA XIS N NGC 4939 196.06 -10.33972 308.09696948 52.40359351 -99 NULL NULL 706023010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 060074 The Eddington ratio (L/LEdd) is the most fundamental observable describing accretion activity. There are claims that the X-ray spectral shape (Gamma) may be used as a proxy of L/LEdd. But the Gamma-L/LEdd correlation also shows some hard spectrum sources as being clear outliers, so the validity of such a correlation needs confirmation. We propose to study 3 outliers to understand the origin of their hard spectral indices. The targets are amongst the bright outlier population, and hence will be detectable above 10 keV with Suzaku. This will enable us to search for signatures distinguishing between various physical scenarios, including intrinsically low-luminosity AGN or heavy obscuration. EXTRAGALACTIC COMPACT SOURCES 7 C HAGINO KOUICHI NULL NULL JAP 6 AO6 ELUCIDATING THE NATURE OF AGNS HAVING UNUSUALLY HARD ENERGY SPECTRA XIS N 1FGL J0103.1+4840 15.7305 48.657 124.88749892 -14.17113818 69.2705 55753.0127430556 55755.0002199074 706025010 84362.2 80000 84362.2 84362.2 0 84362.2 2 2 0 2 1 0 0 79727 79727 171695.7 2 PROCESSED 55778.3520486111 56148 55778.4339814815 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060084 In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher. EXTRAGALACTIC COMPACT SOURCES 7 B MAEDA KOTO NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE XIS Y 1FGL J1946.7-5404 296.6052 -54.0506 343.89458124 -29.55670998 268.6577 55865.7799074074 55866.783599537 706026010 42395.9 40000 42395.9 42398.8 0 42398.8 2 2 0 2 1 0 0 54883.3 54883.3 86707.9 0 PROCESSED 55879.1746064815 56246 55879.1861574074 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060084 In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher. EXTRAGALACTIC COMPACT SOURCES 7 B MAEDA KOTO NULL NULL JAP 6 AO6 SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE XIS Y RX J1633+4718 248.3303 47.3072 73.53738657 42.62611906 329.4078 55743.8204050926 55744.8460069444 706027010 39991.6 40000 39991.6 39991.6 0 39991.6 2 2 0 2 1 0 0 39653.1 39653.1 88605.9 1 PROCESSED 55775.2881365741 56144 55775.3057407407 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060089 RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA KIYOSHI NULL NULL JAP 6 AO6 X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 XIS Y RX J1633+4718 248.3342 47.2989 73.52584527 42.62417772 308.6809 55760.5047916667 55761.4376388889 706027020 37510 40000 37510 37510 0 37510 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 55783.6229513889 56152 55830.7262268518 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060089 RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA KIYOSHI NULL NULL JAP 6 AO6 X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 XIS Y RX J1633+4718 248.3661 47.3315 73.56753068 42.5999019 136.9343 55939.8747337963 55940.8307407407 706027030 44127.1 40000 44127.1 44127.1 0 44127.1 2 2 0 2 1 0 0 38957.8 38957.8 82592 0 PROCESSED 55960.2121296296 56331 55960.228587963 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060089 RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA KIYOSHI NULL NULL JAP 6 AO6 X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 XIS Y RX J1633+4718 248.3647 47.3332 73.56993988 42.60070523 133.9355 55962.6778240741 55963.7502430556 706027040 45483.4 40000 45483.4 45483.4 0 45483.4 2 2 0 2 1 0 0 40311.3 40311.3 92645.9 0 PROCESSED 55978.4985300926 56345 55978.5479282407 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060089 RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA KIYOSHI NULL NULL JAP 6 AO6 X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 XIS Y 4C+74.26 310.7114 75.111 108.98584774 19.50187948 247.6342 55888.5409027778 55890.613275463 706028010 101412.5 100000 101412.5 101412.5 0 101412.5 2 2 0 2 1 0 0 117882.7 117882.7 179029.7 2 PROCESSED 55901.2195486111 56269 55901.2441203704 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 060101 We propose the 120 ks observation of Broad Line Radio Galaxy 4C+74.26. The purpose is to estimate the angular momentum of the central super massive black hole from the broadness of Fe-K line. We study the spectral changes on spectra in details on the Fe-K lines and reflection hump in HXD-PIN band. We try to study the correlation between the radio intensity and black hole spins. EXTRAGALACTIC COMPACT SOURCES 7 C NODA HIROFUMI NULL NULL JAP 6 AO6 STUSY OF BROAD IRON LINE OF 4C+74.26 TO ESTIMATE THE SPIN OF CENTRAL SUPER MASSIVE BLACK HOLE XIS Y MRK 841 226.0091 10.4587 11.24319757 54.63999984 112.9994 55931.8646180556 55937.1896990741 706029010 244351.8 350000 244351.8 244351.8 0 244359.8 2 2 0 2 1 0 0 229726 229726 419686 4 PROCESSED 55946.4579166667 55652 55946.5082407407 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061119 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 6 AO6-LP A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN XIS Y MRK 841 226.0057 10.444 11.21871304 54.63485497 108.0015 55944.7625347222 55947.3599305556 706029020 110289 350000 110291.5 110289 0 110291.5 2 2 0 2 1 0 0 92218.2 92218.2 224404 1 PROCESSED 55985.2857523148 55652 55985.3097337963 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061119 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 6 AO6-LP A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN XIS Y SMC X-1 19.2829 -73.4465 300.41108523 -43.55576838 356.8796 55658.8646759259 55659.2447106482 706030010 18466.2 18000 18466.2 18550 0 18544.8 1 1 0 1 1 0 0 15557.7 15557.7 32823.9 0 PROCESSED 55673.2237847222 56040 55673.2343055556 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2476 -73.446 300.42473809 -43.55764171 6.4299 55669.2561805556 55669.705775463 706030020 17276.9 18000 17276.9 17284.9 0 17484.4 2 2 0 1 1 0 0 17664.6 17664.6 38815.9 0 PROCESSED 55691.1419328704 56058 55691.1543171296 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2337 -73.4445 300.42986971 -43.55966827 9.1005 55673.6490625 55674.1112037037 706030030 15652.6 18000 15652.6 15652.6 0 15871 2 2 0 1 1 0 0 21261.4 21261.4 39919.9 1 PROCESSED 55692.2873032407 56067 55692.2968634259 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2724 -73.4484 300.41553375 -43.55429702 25.8573 55691.0197337963 55691.4064814815 706030040 17905.4 18000 17921.4 17921.4 0 17905.4 1 1 0 1 1 0 0 16814.3 16814.3 33407.9 0 PROCESSED 55701.1453819445 56068 55701.1543981482 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2828 -73.4495 300.41169288 -43.55280074 39.2778 55706.0851851852 55706.6745833333 706030050 17846.3 18000 17846.3 18182.3 0 18100.1 2 2 0 1 1 0 0 16682.9 16682.9 50913.9 0 PROCESSED 55725.1511111111 56092 55725.1651736111 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2661 -73.446 300.41753301 -43.55692043 64.0051 55740.5953819444 55741.0960069444 706030060 18668.2 18000 18712.9 18704.9 0 18668.2 2 2 0 1 1 0 0 20676.4 20676.4 43247.9 0 PROCESSED 55775.1589467593 56163 55775.167974537 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2772 -73.44 300.41207357 -43.56242986 167.9636 55825.1720949074 55825.6536805556 706030070 18123.9 18000 18277.2 18285.2 0 18123.9 2 2 0 1 1 0 0 18368.7 18368.7 41595.9 0 PROCESSED 55848.2999884259 56218 55851.4509027778 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2675 -73.4407 300.41598527 -43.56211574 204.2035 55875.0768055556 55875.6182291667 706030080 19859.8 18000 19888.1 19896.1 0 19859.8 2 2 0 1 1 0 0 19250.8 19250.8 46772 0 PROCESSED 55890.479212963 56260 55890.6941203704 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2766 -73.4376 300.41185267 -43.56483062 244.987 55907.8985069444 55908.2709722222 706030090 17305.5 18000 17407.9 17407.9 0 17305.5 1 1 0 1 1 0 0 18413 18413 32171.9 0 PROCESSED 55920.9659837963 56289 55920.9743981482 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N SMC X-1 19.2681 -73.4483 300.41718915 -43.55456404 342.3682 56005.2598611111 56005.8452546296 706030100 18582.1 18000 18626.3 18634.3 0 18582.1 2 2 0 1 1 0 0 20306.1 20306.1 50571.9 0 PROCESSED 56022.1914467593 88068 56022.2021296296 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061236 We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. EXTRAGALACTIC COMPACT SOURCES 7 A NEILSEN JOSEPH NULL NULL USA 6 AO6 THE WANDERING WARP OF SMC X-1 XIS N III ZW 2 2.6244 10.9839 106.97577765 -50.61513425 67.4163 55726.9877893518 55728.9792708333 706031010 81466 80000 81466 81466 0 81466 2 2 0 2 1 0 0 74362.9 74362.9 172039.7 3 PROCESSED 55748.9019560185 56127 55757.7040046296 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061411 Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA MASAAKI NULL NULL USA 6 AO6 SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG XIS Y NGC 6814 295.6733 -10.3371 29.34034439 -16.02176478 260.0004 55867.6992013889 55868.637662037 706032010 42120 40000 42143.5 42136 0 42120 2 2 0 2 1 0 0 40091.8 40091.8 81069.8 1 PROCESSED 55881.0596643518 56248 55881.0746527778 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061411 Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. EXTRAGALACTIC COMPACT SOURCES 7 A HAYASHIDA MASAAKI NULL NULL USA 6 AO6 SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG XIS Y ESO 323-G077 196.6073 -40.4236 306.0162391 22.35835315 295.8925 55762.647337963 55763.4168287037 706033010 44122.2 40000 44122.2 44122.2 0 44122.2 2 2 0 2 1 0 0 40925.8 40925.8 66481.9 0 PROCESSED 55845.2284490741 56212 55845.2395949074 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061411 Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. EXTRAGALACTIC COMPACT SOURCES 7 B HAYASHIDA MASAAKI NULL NULL USA 6 AO6 SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG XIS Y ESO 511-G030 214.84333 -26.64472 326.22830066 32.21831908 -99 NULL NULL 706034010 -99 270000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 061413 The study of 'bare' Seyfert AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K line component and lack of any intrinsic warm absorption, it is also one of the brightest 'bare' Seyferts featured in the Swift 58 month hard X-ray BAT catalog as yet unobserved by Suzaku. We propose a 270ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the spin of the central black hole. In addition to this, the inclusion of HXD data will allow us to measure the Compton reflection hump, while the excellent XIS spectral resolution at soft X-rays will allow the origin of the soft excess to be determined. EXTRAGALACTIC COMPACT SOURCES 7 C REEVES JAMES NULL NULL USA 6 AO6 MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 XIS N ZW229-15 286.3333 42.4706 73.09172558 15.5517204 34.6696 55715.0128356482 55719.6251736111 706035010 167083.8 165000 168676.6 167083.8 0 168684.6 2 2 0 2 1 0 0 218183.2 218183.2 398435.7 2 PROCESSED 55748.9090740741 56127 55757.7055671296 2.6.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061414 The optical emission from AGN is though to be a combination of direct radiation from an accretion disk and reprocessed x-ray emission. Separating these components requires simultaneous high-precision x-ray/optical monitoring, which has heretofore not been achieved. We propose to gather this necessary data via simultaneous optical and x-ray monitoring of the Sy 1 galaxy Zw 229-15. Kepler is monitoring Zw 229-15 every 30 minutes with unprecedented 99% duty cycle and 0.1% repeatability. The key missing data is an appropriate x-ray campaign. We propose a 64-orbit (165 ks) Suzaku long-look combined with a series of 48 Swift visits to probe lags of 0.1-10 days. This will be the first experiment sensitive to such short lags and thus will critically test the present disc/reprocessing paradigm EXTRAGALACTIC COMPACT SOURCES 7 B MUSHOTZKY RICHARD NULL NULL USA 6 AO6 SIMULTANEOUS SUZAKU/SWIFT/ KEPLER MONITORING OF ZW 229-15 XIS Y B3 0309+411 48.2809 41.3324 149.59257755 -14.09014879 253.0016 55976.5100462963 55979.0410532407 706036010 104624.5 100000 104624.5 104629.6 0 104624.5 2 2 0 2 1 0 0 95453 95453 218671.9 2 PROCESSED 55992.2083101852 56360 55992.2317824074 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062007 We propose to observe B3 0309+411, an X--ray bright FRII BLRG detected by INTEGRAL for 100 ks. BRLGs have been poorly studied in X-rays and usually show weak reprocessing spectral features with respect to their radio-quiet counterparts. B3 0309+411 has been already followed-up with XMM-Newton and, the XMM-Newton and INTEGRAL data suggests that the source could 1) be strongly reflection-dominated; 2) exhibit extreme flux/spectral variability; 3) be severely affected by absorption. The Suzaku observation will unveil the puzzling spectral shape of this peculiar BLRG, allowing to determine with accuracy the reflection properties which would have a large impact on our understanding of the disk/jet contribution in BLRG. EXTRAGALACTIC COMPACT SOURCES 7 B PANESSA FRANCESCA NULL NULL EUR 6 AO6 B3 0309+411: A REFLECTION--DOMINATED BROAD LINE RADIO GALAXY? XIS Y MRK 231 193.9205 56.8603 121.76268106 60.25831511 352.6128 55678.6054282407 55682.3543402778 706037010 197511.3 200000 197511.3 197511.3 0 197511.3 2 2 0 2 1 0 0 191743.4 191743.4 323875.6 2 PROCESSED 55697.3845023148 56065 55697.4231597222 2.5.16.29 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062008 We propose the first Suzaku observation of the nearest low-ionization BAL quasar/ULIRG, i.e. MRK 231, for which we have recently reported the most clear-cut evidence for AGN-driven feedback onto the host galaxy cold molecular gas component. Our target exhibits an hard X-ray (> 15 keV) excess in a previous BeppoSAX/PDS spectrum, suggesting the presence of a heavily obscured quasar at the heart of this peculiar system. By exploiting the Suzaku unique broad-band spectral coverage, we aim at deriving the column density of the nuclear absorber and, in turn, the intrinsic luminosity of the quasar with unprecedented accuracy. EXTRAGALACTIC COMPACT SOURCES 7 A PICONCELLI ENRICO NULL NULL EUR 6 AO6 BROAD-BAND X-RAY SPECTROSCOPY OF THE NEAREST BAL QUASAR/ULIRG MARKARIAN 231 HXD Y IRAS 09104+4109 138.3378 40.9513 180.99146588 43.55010524 90.0004 55883.9878356482 55885.7675694444 706038010 81327.6 80000 81335.6 81327.6 0 81335.6 2 2 0 2 1 0 0 76588.3 76588.3 153730 2 PROCESSED 55895.1875694444 56264 55895.209849537 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062009 We propose to observe IRAS 09104+4109 for 80 ks with Suzaku in order to confirm the ~3 sigma BeppoSAX PDS detection of the source and increase the detection significance with the HXD/PIN to 10 sigma in the 10--80 keV band, allowing the detailed spectral shape to be determined. IRAS 09104+4109 is a hyperluminous Type 2 quasar embedded in a central cluster galaxy at redshift 0.442. It is likely to be the hard-X-ray-brightest such object observed with Suzaku and could well be the prototype Compton-thick Type 2 quasar. The Suzaku observation, especially above 10 keV will most likely reveal one of the most luminous Compton--thick Type 2 QSO to date. EXTRAGALACTIC COMPACT SOURCES 7 C CHIANG CHIA-YING NULL NULL EUR 6 AO6 THE TYPE 2 HYPERLUMINOUS QUASAR IRAS 09104+4109 XIS Y IGR J16024-6107 240.45125 -61.14861 323.93711937 -6.30129608 -99 NULL NULL 706039010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 062023 We ask 100 ks exposure on the Sey 2 IGR J16024-6107. The analysis of non-simultaneous XMM and Integral data revealed a moderate obscuration in X-rays, two narrow iron K lines and a huge value of the Reflection fraction. The high value of R could be due to possible flux variation between the XMM and Integral observations or to a real presence of a (non-uniform) Compton thick gas. The main goal of our proposal is to firmly measure the Compton reflection without any ambiguity with respect to variability. This study will allow us to investigate the physical/geometrical properties of the regions around the SMBH. The proposed programme will be supported by simultaneous optical observations. EXTRAGALACTIC COMPACT SOURCES 7 C DE ROSA ALESSANDRA NULL NULL EUR 6 AO6 ABSORPTION AND REFLECTION PROPERTIES OF THE HARD X-RAY SELECTED SEYFERT 2 AGN IGR J16024-6107 XIS N NGC6240 253.24583 2.40056 20.72891692 27.2903482 -99 NULL NULL 706040010 -99 150000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 062025 We propose to observe the galaxy NGC6240. It is a template of Ultraluminous Infrared Galaxies (ULIRGs), and it hosts both a powerful starburst and a Compton-thick AGN. It is often used as a template for luminous obscured class-II QSOs, and as a basis for the modeling of the Cosmic X-ray Background. Despite its importance, the spectral parameters above 10 keV are not yet known, so that even the absorption-corrected luminosity is uncertain. By observing with the XIS and HXD/PIN instrumets, we will be able to determine the slope of the Compton-thick component, the column density of the absorber, the reflection efficiency, the relative luminosities of the AGN and of the starburst. EXTRAGALACTIC COMPACT SOURCES 7 C RANALLI PIERO NULL NULL EUR 6 AO6 THE POWERFUL STARBURST AND THE COMPTON-THICK AGN IN NGC 6240 HXD N MRK 478 220.4959 35.3708 59.0913373 65.0766343 294.6097 55756.9652777778 55758.8334837963 706041010 85323.6 80000 85331.6 85339.6 0 85323.6 3 2 0 2 1 0 0 77636.6 77636.6 161389.7 1 PROCESSED 55783.6922800926 56151 55783.7198842593 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 062028 The NLS1 galaxy Mrk 478 has exceptionally unusual properties. It shows up to a factor of five variability while keeping its spectral shape constant. Previous short XMM-Newton observations show that it is probably reflection-dominated, where light-bending effects are at their extreme. This is the only known object that shows such high variability while remaining in a reflection-dominated state. All other known objects show reflection-dominated spectra only when in a faint state, making their study very difficult. This object is reflection-dominated yet bright enough to study with relatively short exposures.Here we propose to observe this object for 80 ks. The goal is to detect the reflection hump using Suzaku capabilities above 10 keV and probe light-bending around this black hole. EXTRAGALACTIC COMPACT SOURCES 7 A ZOGHBI ABDERAHMEN NULL NULL EUR 6 AO6 PROBING EXTREME RELATIVISITC LIGHT-BENDING IN MRK 478 HXD Y 3C120 68.2984 5.3496 190.37864439 -27.39774516 260.9996 55966.4234143518 55970.8752083333 706042010 183001.5 300000 183025.5 183001.5 0 183025.5 3 2 0 2 1 0 0 158030.6 158030.6 384595.7 3 PROCESSED 55992.3790277778 55652 55992.4178819444 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 6 AO6-KP A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN XIS Y 3C120 68.2996 5.3511 190.37800916 -27.39591229 261.0003 55971.7483564815 55974.8819907407 706042020 118068.9 120000 118068.9 118068.9 0 118068.9 2 2 0 2 1 0 0 103536.5 103536.5 270735.9 2 PROCESSED 55992.2839467593 55652 55992.3150694444 2.7.16.31 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 066003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A REYNOLDS CHRISTOPHER NULL NULL USA 6 AO6-KP A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN XIS Y 0528+134 82.7323 13.541 191.35839601 -11.00951452 89.1633 55832.6802314815 55833.0119444444 706043010 14789.2 10000 14789.2 14789.2 0 14789.2 2 2 0 2 1 0 0 15865.9 15865.9 28635.9 0 PROCESSED 55875.5396180556 56225 55875.6223958333 2.7.16.30 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061601 We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. EXTRAGALACTIC COMPACT SOURCES 7 S JORSTAD SVETLANA NULL NULL USA 6 AO6 EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM XIS Y 1622-297 246.5282 -29.8629 348.81494865 13.309894 287.0011 55828.8879166667 55829.1800810185 706044010 8778.1 10000 8778.1 8778.1 0 8778.1 2 2 0 2 1 0 0 8751.3 8751.3 25198 0 PROCESSED 55868.9273263889 56236 55868.9351851852 2.7.16.30 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061601 We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. EXTRAGALACTIC COMPACT SOURCES 7 S JORSTAD SVETLANA NULL NULL USA 6 AO6 EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM XIS Y 4C38.41 248.824 38.1186 61.06470824 42.32788618 255.0463 55829.1891666667 55829.4148032407 706045010 8923.9 10000 8931.9 8931.9 0 8923.9 1 1 0 1 1 0 0 9535.3 9535.3 19471.9 0 PROCESSED 55875.5343402778 56225 55875.6235185185 2.7.16.30 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061601 We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. EXTRAGALACTIC COMPACT SOURCES 7 S JORSTAD SVETLANA NULL NULL USA 6 AO6 EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM XIS Y 1730-130 263.2641 -13.0933 12.02258907 10.80244107 271.1606 55829.6599537037 55830.0946643518 706046010 11085.8 10000 11093.8 11093.8 0 11085.8 1 1 0 1 1 0 0 9881.1 9881.1 37535.9 1 PROCESSED 55875.5372337963 56225 55875.6203703704 2.7.16.30 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061601 We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. EXTRAGALACTIC COMPACT SOURCES 7 S JORSTAD SVETLANA NULL NULL USA 6 AO6 EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM XIS Y OT+081 267.8906 9.6366 34.9082961 17.63584745 268.2827 55830.0996759259 55830.3911921296 706047010 10774 10000 10774 10774 0 10774 1 1 0 1 1 0 0 11036 11036 25151.9 1 PROCESSED 55875.5357638889 56225 55875.6247569444 2.7.16.30 2 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 061601 We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. EXTRAGALACTIC COMPACT SOURCES 7 S JORSTAD SVETLANA NULL NULL USA 6 AO6 EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM XIS Y NGC 4941 196.05471 -5.55161 308.80584418 57.1743004 -99 NULL NULL 707001010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070003 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7 BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND XIS N NGC 1566 65.00167 -54.93778 264.31008938 -43.39331862 -99 NULL NULL 707002010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070003 The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. EXTRAGALACTIC COMPACT SOURCES 7 A UEDA YOSHIHIRO NULL NULL JAP 7 AO7 BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND XIS Y NGC 7603 349.73604 0.24389 80.06765348 -54.73980568 -99 NULL NULL 707003010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070010 X-ray spectra from Seyfert galaxies often consist of various emission components such as from an accretion disk and dusty torus. Because of this complexity, interpretation of reprocessed feature (Fe lines and reflection continuum) in X-ray spectra is often ambiguous. We selected a Seyfert 1 with very weak mid infrared emission from the putative torus relative to X-rays from an accretin disk bu using AKARI IR and XMM X-ray catalogs. We will measure a ``pure'' accretion disk spectrum without contamination of reprocessed emission from the torus, and castrain extent of an accretion disk, which is expected to depend on an Eddington ratio, from the reprocessed X-ray emission. EXTRAGALACTIC COMPACT SOURCES 7 B TERASHIMA YUICHI NULL NULL JAP 7 AO7 PURE ACCRETION DISK SPECTRUM OF THE SEYFERT 1 NGC 7603 XIS N 3C 227 146.93833 7.42222 228.58278161 42.28622509 -99 NULL NULL 707004010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070012 Radio galaxies are a key class to understand the origin and effects of AGN feedback to the surroundings. However, the fundamental question, how the structure of the nucleus is different between AGNs with and without jets, is not resolved yet. A key parameter to understand the accretion flow is the Eddington ratio. BLRGs of 4C 50.55 and 3C 120 are rare objects having high Eddington ratio (L_bol/L_Edd~0.4) compared with Seyferts and typical BLRGs (< 0.1). Though the accretion disks in many BLRGs are known to be truncated and/or inner parts covered by corona, unified picture of accretion flows over a wide range of accretion rate is far from established. Therefore we propose observing a BLRG of 3C 227, which has the highest Eddington ratio in the hard X-ray luminous BLRGs. EXTRAGALACTIC COMPACT SOURCES 7 C TAZAKI FUMIE NULL NULL JAP 7 AO7 STUDY OF NUCLEAR STRUCTURE OF BLRGS WITH HIGH ACCRETION RATE XIS N 3C 236 WEST LOBE 151.3326 35.0063 189.89255573 53.835807 -99 NULL NULL 707005010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070014 Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe. EXTRAGALACTIC COMPACT SOURCES 7 A ISOBE NAOKI NULL NULL JAP 7 AO7 INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 XIS Y 3C 236 BACKGROUND 151.1525 34.7488 190.33084647 53.69085038 -99 NULL NULL 707006010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070014 Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe. EXTRAGALACTIC COMPACT SOURCES 7 A ISOBE NAOKI NULL NULL JAP 7 AO7 INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 XIS Y 2FGL J0923.5+1508 140.989 15.088 215.95959912 40.48625478 -99 NULL NULL 707007010 -99 90000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070024 We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe. EXTRAGALACTIC COMPACT SOURCES 7 B TAKAHASHI YOSUKE NULL NULL JAP 7 AO7 SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE XIS Y 2FGL J1502.1+5548 225.621 55.868 92.72383945 52.88040322 -99 NULL NULL 707008010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070024 We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe. EXTRAGALACTIC COMPACT SOURCES 7 B TAKAHASHI YOSUKE NULL NULL JAP 7 AO7 SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE XIS Y 2FGL J0022.2-1853 5.5385 -18.89281 82.14223288 -79.36517807 -99 NULL NULL 707009010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070034 We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). EXTRAGALACTIC COMPACT SOURCES 7 B KATAOKA JUN NULL NULL JAP 7 AO7 FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY XIS N 2FGL J0037.8+1238 9.46271 12.63911 117.76120183 -50.09617873 -99 NULL NULL 707010010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070034 We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). EXTRAGALACTIC COMPACT SOURCES 7 B KATAOKA JUN NULL NULL JAP 7 AO7 FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY XIS N 2FGL J0157.2-5259 29.2405 -53.03333 282.19776069 -61.37740665 -99 NULL NULL 707011010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070034 We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). EXTRAGALACTIC COMPACT SOURCES 7 B KATAOKA JUN NULL NULL JAP 7 AO7 FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY XIS N NGC 3431 162.8125 -17.00806 266.03426935 37.10769462 -99 NULL NULL 707012010 -99 70000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070067 The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature. EXTRAGALACTIC COMPACT SOURCES 7 A GANDHI POSHAK NULL NULL JAP 7 AO7 WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? XIS N ESO 565-G019 143.68125 -21.92778 253.86823335 21.67993675 -99 NULL NULL 707013010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070067 The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature. EXTRAGALACTIC COMPACT SOURCES 7 A GANDHI POSHAK NULL NULL JAP 7 AO7 WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? XIS Y RXJ0134-4258 23.57046 -42.97397 276.936266 -71.92573671 -99 NULL NULL 707014010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070081 RXJ0134.2-4258 was detected in the ROSAT all sky observation (RASS), later identified as a radio loud (RL) narrow line Seyfert 1 galaxy. During the RASS, the soft X-ray spectrum of this source was steep. Following observations with ROSAT, ASCA, Swift, and XMM-Newton (XMM) showed flatter spectra. The XMM spectra are fitted with a power law with an cut-off (EC) at 4 keV, where a blackbody (BB) component was not evident. Either type of spectrum is not common for Seyferts. We consider this peculiarity is related to the RL nature of this object, originated in the jet. We will observe this source with Suzaku, which has higher energy resolution than XMM, to reveal the long term variability of this source. Particular interests go to the EC energy, bb component, and the iron K emission line. EXTRAGALACTIC COMPACT SOURCES 7 C TAKAHASHI HIROAKI NULL NULL JAP 7 AO7 X-RAY EMISSION FROM THE BRIGHTEST RADIO LOUD NARROW LINE SEYFERT 1 RXJ0134.2-4258 XIS N 1H0323+342 51.171 34.179 155.72667322 -18.75710691 -99 NULL NULL 707015010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070088 We propose to observe a narrow-line radio-loud gamma-ray emitting Seyfert 1 galaxy 1H0323+342, which is the X-ray brightest among a new class of GeV gamma-ray emitting AGNs, first detected by Fermi/LAT. Based on accurate and high-sensitive measurement of X-ray spectra with Suzaku, we study the presence of Fe-K lines and energy-dependence of time variability, in order to constrain the origin of X-ray emission of this object. This leads to understanding the SED of this object and constraining the jet power. EXTRAGALACTIC COMPACT SOURCES 7 C FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 STUDY OF X-RAY SPECTRAL VARIABILITY OF A NARROW-LINE RADIO-LOUD GAMAM-RAY EMITTING SEYFERT 1 GALAXY 1H0323+342 XIS N E1821+643 275.4885 64.34339 94.00249285 27.41700178 -99 NULL NULL 707016010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070089 Central engines of AGN are considered to be generally in Multi-Zone Comptonization (MZC) condition (e.g., Noda et al. 2011a,b). To verify this thing on a high-luminosiy AGN, we suggest to observe Radio-Quiet Quasar E1821+643 By Suzaku. Utilizing a time variability of each Comptonization component, we will resolve spectral variable components, and study whether the central engine of E1821+643 is in MZC condition or not. EXTRAGALACTIC COMPACT SOURCES 7 C NODA HIROUMI NULL NULL JAP 7 AO7 SUZAKU STUDY OF MULTI-ZONE COMPTONIZATION PICTURE ON THE CENTRAL ENGINE OF RADIO-QUIET QUASAR E1821+643 XIS N NGC1365 53.402 -36.138 237.95193057 -54.59785619 -99 NULL NULL 707017010 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070095 NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } EXTRAGALACTIC COMPACT SOURCES 7 B FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 XIS N NGC1365 53.402 -36.138 237.95193057 -54.59785619 -99 NULL NULL 707017020 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070095 NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } EXTRAGALACTIC COMPACT SOURCES 7 B FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 XIS N NGC1365 53.402 -36.138 237.95193057 -54.59785619 -99 NULL NULL 707017030 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070095 NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } EXTRAGALACTIC COMPACT SOURCES 7 B FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 XIS N NGC1365 53.402 -36.138 237.95193057 -54.59785619 -99 NULL NULL 707017040 -99 30000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070095 NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } EXTRAGALACTIC COMPACT SOURCES 7 B FUKAZAWA YASUSHI NULL NULL JAP 7 AO7 MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 XIS N SWIFT J164449.3+1573 251.20792 57.58333 86.7113491 39.4412737 -99 NULL NULL 707018010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 070096 We propose a 80 ks observation of a tidal disruption event Swift J164449.3+1573451 one year after its onset. In this event, a star was presumably disrupted by a strong tidal force of a massive black hole at the center of a galaxy at z=0.35, releasing a relativistic jet that emitted intense X-rays. In this proposal, we attempt to detect the non-thermal emission from the relativistic jet and the fluorescent Fe K line from its surrounding material. With these results we study the driving mechanism of the jet and to test the tidal disruption model. EXTRAGALACTIC COMPACT SOURCES 7 B USUI RYUICHI NULL NULL JAP 7 AO7 ONE YEAR AFTER THE TIDAL DISRUPTION OF SWIFT J164449.3+1573451 XIS Y HOLMBERG IX X-1 149.4435 69.0486 141.95726659 41.07139178 311.5635 56030.7575810185 56034.6807175926 707019010 182527.4 500000 182527.4 182527.4 0 182527.4 2 2 0 2 1 0 0 208623.6 208623.6 338933.9 3 PROCESSED 56044.4331365741 56018 56044.4614699074 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 071251 Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. EXTRAGALACTIC COMPACT SOURCES 7 A MILLER JON NULL NULL USA 7 AO7 A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE XIS Y SNR 1987A 83.86667 -69.26975 279.7034345 -31.93709283 -99 NULL NULL 707020010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071331 Despite extensive observations of supernova remnant (SNR) 1987A with Chandra and XMM-Newton, the origin of the hard band (3-10 keV) X-ray emission is elusive (thermal vs nonthermal). A straightforward way to discriminate the thermal and nonthermal origins of the hard X-rays is to detect Fe K lines. The Suzaku XIS provides a uniquely efficient opportunity for a sensitive search for the Fe K lines, which is an excellent complement to the existing Chandra and XMM-Newton studies of SNR 1987A. Thus, we propose an 80 ks Suzaku observation of SNR 1987A. EXTRAGALACTIC COMPACT SOURCES 7 C PARK SANGWOOK NULL NULL USA 7 AO7 X-RAY EMISSION FROM SUPERNOVA REMNANT 1987A XIS N AO 0235+164 39.6625 16.61611 156.77127117 -39.10963825 -99 NULL NULL 707021010 -99 40000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071402 We request observations of the variable blazar AO 0235+164, to be conducted simultaneously with Fermi and optical and radio telescopes, towards a multi-band campaign. This object has complex X-ray spectrum due to absorption by an intervening galaxy, and Suzaku will be essential in unraveling the effects and composition of that absorber, and for the first time, provide a robust measurement of the underlying blazar X-ray continuum, which, together with the Swift UVOT spectrum, will allow to verify the signature of the bulk-Compton component, due to cold electrons propagating in the relativistic jet. At the highest priority, we request 40 ks for a precise spectral measurement; at a lower priority, we wish to monitor the source for the total of 5 days, with the request of additional 160 ks. EXTRAGALACTIC COMPACT SOURCES 7 B MADEJSKI GRZEGORZ NULL NULL USA 7 AO7 SUZAKU OBSERVATIONS OF THE GAMMA-RAY BLAZAR AO 0235+164 XIS N NGC 4593 189.91417 -5.34417 297.48271593 57.40287587 -99 NULL NULL 707022010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071412 We request a 120 ks observation of the X-ray bright Seyfert NGC 4593, previous X-ray observations of which support the presence of a truncated radiatively-efficient disk. A 2007 Suzaku observation happened to catch the source in a low flux state, hinting at structural changes to, or poor illumination in, the inner disk. A second observation at a normal flux level will enable us to resolve the Fe line and test for relativistic broadening in the Fe K profile with proper statistics. Only a new observation using the broadband coverage of Suzaku can deconvolve the broadband emitting/absorbing components, quantify the long-term behavior of the Compton reflection hump, and constrain if/how the disk structure and/or illumination of the disk responds to the continuum X-ray flux level. EXTRAGALACTIC COMPACT SOURCES 7 C MARKOWITZ ALEX NULL NULL USA 7 AO7 TRACKING THE BEHAVIOR OF THE TRUNCATED ACCRETION DISK IN NGC 4593 XIS N ESO 511-G030 214.84333 -26.64472 326.22830066 32.21831908 -99 NULL NULL 707023010 -99 270000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071413 The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. EXTRAGALACTIC COMPACT SOURCES 7 A REEVES JAMES NULL NULL USA 7 AO7 MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 XIS N NGC 4151 182.63575 39.40572 155.0773325 75.06317443 -99 NULL NULL 707024010 -99 150000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071417 We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. EXTRAGALACTIC COMPACT SOURCES 7 A BRENNEMAN LAURA NULL NULL USA 7 AO7 SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A XIS N IC 4329A 207.33025 -30.30944 317.49624781 30.92002733 -99 NULL NULL 707025010 -99 120000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071417 We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. EXTRAGALACTIC COMPACT SOURCES 7 A BRENNEMAN LAURA NULL NULL USA 7 AO7 SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A XIS N PG 1404+226 211.59117 22.39617 21.47671404 72.36521032 -99 NULL NULL 707026010 -99 80000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071419 We propose a 80 ks observation of a NLS galaxy, PG1404+226, with Suzaku/XIS to investigate the physical conditions of extreme absorbers known as the ultra-fast-outflows (UFOs; v/c~0.1-0.2) of variable resonant absorption features from many ions (e.g. Ne IX, Ne X, Mg XII and S XVI) in the soft X-ray band (~0.5-3.5 keV), and we propose the first Suzaku observation of this object to (i) independently confirm/refute the previous claims of the presence of these UFOs including a potential detection of Fe K-shell absorbers, (ii) examine their variabilities and compare the outflow properties at low and high XIS-flux states, (iii) compare its outflow rate and kinetic power with those in other AGN UFOs, and (iv) utilize a high-quality Suzaku data to improve our MHD disk-wind model. EXTRAGALACTIC COMPACT SOURCES 7 C FUKUMURA KEIGO NULL NULL USA 7 AO7 PROBING THE ULTRA-FAST-OUTFLOWS OF PG1404+226 WITH SUZAKU XIS N MCG-03-34-64 200.60192 -16.72858 313.53985024 45.50432017 -99 NULL NULL 707027010 -99 150000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 071423 Analysis of Suzaku observations selected from the BAT 58-month catalog has shown extreme hard X-ray excesses to exist in ~70% of type 1 AGN, and these can be modeled by partial-covering of Compton-thick gas. This new result shows the importance of broad X-ray coverage, currently available only with Suzaku. The most extreme of the sample sources, MCG-03-34-64 and NGC 1194, show significant spectral and flux variability above 10 keV, likely attributable to changes in the Compton-thick absorber. We request new observations of MCG-03-34-64 (150 ks) and NGC 1194 (200 ks) to study the X-ray reprocessor in these extreme systems, confirm the high-energy spectral variability and constrain the nature and location of the Compton-thick absorber. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 THE CASE FOR VARIATIONS IN COMPTON-THICK ABSORPTION: MCG-03-34-64 AND NGC 1194 XIS N NGC 5252 204.56625 4.5425 331.29811657 64.80324027 -99 NULL NULL 707028010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071424 A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM XIS N IRAS 05078+1626 77.68958 16.49861 186.1137271 -13.49938095 -99 NULL NULL 707029010 -99 45000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071424 A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM XIS N NGC 931 37.06025 31.3115 146.11404172 -27.1659872 -99 NULL NULL 707030010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071424 A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM XIS N ESO 141-G55 290.30888 -58.67036 338.18334805 -26.71120848 -99 NULL NULL 707031010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071424 A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM XIS N UGC 03142 70.94496 28.97178 172.0887829 -10.99643268 -99 NULL NULL 707032010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071424 A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM XIS N 2MASX J11454045-1827 176.41858 -18.45417 281.85431509 41.71026419 -99 NULL NULL 707033010 -99 50000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071424 A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. EXTRAGALACTIC COMPACT SOURCES 7 C TURNER TRACEY NULL NULL USA 7 AO7 INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM XIS N NGC 2110 88.0475 -7.45611 212.92624903 -16.54517825 -99 NULL NULL 707034010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071426 We request two 100 ks EXTRAGALACTIC COMPACT SOURCES 7 B RIVERS ELIZABETH NULL NULL USA 7 AO7 TRACKING THE PARTIAL COVERING ABSORBERS IN NGC 2110: CONSTRAINTS FOR CLUMPY ABSORBER MODELS XIS N PDS 456 262.0825 -14.26556 10.39214013 11.1635133 -99 NULL NULL 707035010 -99 450000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 56018 NULL NULL NULL NULL 071431 PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. EXTRAGALACTIC COMPACT SOURCES 7 B REEVES JAMES NULL NULL USA 7 AO7 VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 XIS N IRAS 00182-7112 5.14458 -70.92417 306.5521554 -45.98654983 -99 NULL NULL 707036010 -99 90000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071441 We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. EXTRAGALACTIC COMPACT SOURCES 7 B NARDINI EMANUELE NULL NULL USA 7 AO7 THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS XIS Y IRAS 12127-1412 183.82875 -14.49583 289.9419292 47.46276581 -99 NULL NULL 707037010 -99 60000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 071441 We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. EXTRAGALACTIC COMPACT SOURCES 7 B NARDINI EMANUELE NULL NULL USA 7 AO7 THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS XIS N WISE J1819+4532 274.9137 45.5584 73.38480627 24.31157427 77.6532 56020.3333333333 56021.0070833333 707038010 30881.9 30000 30881.9 30881.9 0 30881.9 2 2 0 2 1 0 0 27564 27564 58203.9 0 PROCESSED 56033.2282291667 88068 56033.2380787037 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 071443 We request a 30-ks observation of WISE J1819+4532, an extreme WISE-selected AGN at z=2.031. This source stands out even amongst the rare WISE-selected sources we have been targeting: at mid-IR wavelengths, WISE J1819+4532 is ~10x brighter than similarly selected WISE sources, and more than 50x brighter than extreme Spitzer-selected sources. Assuming the local mid-IR to hard X-ray correlations, the implied intrinsic hard X-ray luminosity is L(2-10)~3e46 erg/s. WISE J1819+4532 is optically faint and the optical spectrum shows a typical obscured AGN with narrow emission lines. However, the object is infrared bright and the near-IR spectrum shows broad H-alpha emission. This implies that WISE J1819+4532 is a rare example of a an extremely luminous, semi-obscured AGN. EXTRAGALACTIC COMPACT SOURCES 7 A STERN DANIEL NULL NULL USA 7 AO7 WISE J1819+4532: AN OBSCURED, HYPERLUMINOUS ULIRG/AGN AT Z~2 XIS Y RE J1034+396 158.66083 39.64111 180.27825596 59.06464008 -99 NULL NULL 707039010 -99 100000 -99 -99 -99 -99 NULL NULL NULL NULL NULL -99 -99 -99 -99 -99 NULL NOTPROCESSED NULL 88068 NULL NULL NULL NULL 072005 Understanding the nature of the emission from the extreme active galaxy, RE J1034+396 can help us to unravel the properties of accretion as the Eddington limit is reached. A fleeting glimpse of the unique quasi-periodic oscillation (QPO) in this source has shown a complex timing behaviour with the emission below ~2 keV apparently crucial to its presence. Thus by understanding the origin and properties of the soft emission we can probe the physical mechanism of signals that cannot be resolved in stellar mass X-ray binaries but must be associated with the regions closest to the black hole. A new observation with Suzaku will allow a much deeper analysis of the soft emission and will shed light on how its changing properties can trigger such unique behaviour as the QPO. EXTRAGALACTIC COMPACT SOURCES 7 C MIDDLETON MATTHEW NULL NULL EUR 7 AO7 REVEALING THE NATURE OF RE J1034+396 AND THE EXTREME SOFT EXCESS XIS N PKS 0548-322 87.6707 -32.2739 237.56869078 -26.144265 287.028 56023.6105555556 56026.3891435185 707040010 102656.7 100000 102656.7 102656.7 0 102656.7 2 2 0 2 1 0 0 91523.7 91523.7 240055.8 3 PROCESSED 56044.2871527778 88068 56044.314525463 2.7.16.32 1 Hea_24Mar2010_V6.9_Suzaku_24Mar2010_V16 072006 We propose Suzaku observations of the two brightest extreme BL Lac objects, PKS 0548-322 and RGB J0710+591 (100 ksec each), whose synchrotron bump peaks in the medium-hard X-ray band. The requested observations, never performed by Suzaku on this two sources, will permit to measure their continuum in the 0.6-70 keV range, fully exploiting the unique capabilities of the Suzaku satellite. With its wide energy coverage and good response, Suzaku will allow us to determine with unprecedented precision the spectral properties of the sources in the hard, medium and soft X-ray ranges, allowing us to measure the physical properties of the emitting relativistic electrons and, complemented by data at other frequencies, to infer the physical conditions in the emitting region. EXTRAGALACTIC COMPACT SOURCES 7 A TAVECCHIO FABRIZIO NULL NULL EUR 7 AO7 REVEALING THE HIGH-ENERGY SYNCHROTRON PEAK OF EXTREME BL LACS WITH SUZAKU XIS Y A1413 178.8303 23.6485 225.18767075 76.86550896 123.0348 53689.8362847222 53692.5939699074 800001010 107867.2 100000 107867.2 108003.2 107947.2 107910.3 2 2 2 2 1 0 0 102431.5 102431.5 238239.7 7 PROCESSED 54331.5152662037 54247 54038.1136689815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001010 No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement. EXTRAGALACTIC DIFFUSE SOURCES 8 A HENRY J. NULL NULL JAP 0 SWG CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS XIS N FORNAX CLUSTER NORTH 54.7022 -35.2276 236.33819165 -53.57399329 245.0013 53740.3046990741 53740.493275463 800002010 7763.5 80000 7763.5 7763.5 7763.5 7763.5 1 1 1 1 1 0 0 8270.8 8270.8 16271.9 0 PROCESSED 54320.570462963 54247 54039.6718518518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001018 The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 0 SWG MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER NULL N FORNAX CLUSTER NORTH 54.7043 -35.2293 236.34100564 -53.57224957 244.9996 53741.5137847222 53742.3336111111 800002020 37192.1 80000 37192.1 37216.1 37208.1 37200.1 2 2 2 2 1 0 0 39287.4 39287.4 70815.9 1 PROCESSED 54324.8078240741 54247 54039.8151041667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001018 The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 0 SWG MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER XIS N FORNAX CLUSTER NORTH 54.7043 -35.2294 236.34117402 -53.57224789 244.9993 53749.1506134259 53750.3265509259 800002030 45575 80000 45583 45579 45575 45587 2 2 2 2 1 0 0 42571.3 42571.3 101600 1 PROCESSED 54325.0726851852 54247 54039.9702777778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001018 The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 0 SWG MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER XIS N A1060 159.1744 -27.531 269.60056717 26.48279097 103.6438 53696.6258796296 53697.7211111111 800003010 39139 40000 39139 39147 39155 39155 2 2 2 2 1 0 0 34602.4 34602.4 94625.9 1 PROCESSED 54327.710162037 54247 54037.8583449074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001021 A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. EXTRAGALACTIC DIFFUSE SOURCES 8 A OHASHI TAKAYA NULL NULL JAP 0 SWG OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 XIS N A1060 OFFSET 159.5124 -27.532 269.88117164 26.64663217 96.4857 53694.9817708333 53696.6231365741 800004010 52402.5 60000 52402.5 53202.5 52418.5 52538.5 2 2 2 2 1 0 0 46203.9 46203.9 141801.8 1 PROCESSED 54329.6246875 54247 54038.1216666667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001021 A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. EXTRAGALACTIC DIFFUSE SOURCES 8 A OHASHI TAKAYA NULL NULL JAP 0 SWG OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 XIS N ABELL2811 10.4703 -28.5552 358.34166022 -87.45073592 232.1065 53702.1678240741 53702.8814699074 800005010 30654.6 25000 30662.6 30682.6 30654.6 30665.9 2 2 2 2 1 0 0 28325.4 28325.4 61656 0 PROCESSED 54324.189224537 54247 54038.5109722222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001025 We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. EXTRAGALACTIC DIFFUSE SOURCES 8 A TAMURA TAKAYUKI NULL NULL JAP 0 SWG THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM XIS N ABELL2811-OFF 10.1781 -28.7333 358.19144602 -87.13859798 232.6526 53702.8821296296 53703.731412037 800006010 33949.4 25000 33957.4 33965.4 33949.4 33949.8 2 2 2 2 1 0 0 30905.6 30905.6 73365.9 1 PROCESSED 54324.9009259259 54247 54038.6719560185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001025 We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. EXTRAGALACTIC DIFFUSE SOURCES 8 A TAMURA TAKAYUKI NULL NULL JAP 0 SWG THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM XIS N ABELL2804 9.8968 -28.9096 357.98440451 -86.83577265 234.7036 53706.3688078704 53707.166875 800007010 31612.9 25000 31612.9 31612.9 31612.9 31612.9 2 2 2 2 1 0 0 26914.5 26914.5 68950 2 PROCESSED 54405.4656828704 54247 54038.8727893518 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001025 We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. EXTRAGALACTIC DIFFUSE SOURCES 8 A TAMURA TAKAYUKI NULL NULL JAP 0 SWG THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM XIS N ABELL2801 9.6433 -29.1188 357.12193154 -86.53506096 232.0377 53701.3547106482 53702.1668865741 800008010 34890 25000 34890 34890 34890 34890 2 2 2 2 1 0 0 30163.6 30163.6 70163.9 1 PROCESSED 54320.765474537 54247 54038.3717361111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001025 We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. EXTRAGALACTIC DIFFUSE SOURCES 8 A TAMURA TAKAYUKI NULL NULL JAP 0 SWG THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM XIS N NGC720 28.2529 -13.7362 173.01572713 -70.35499124 242.5294 53734.3673611111 53739.5627546296 800009010 177192.9 100000 177192.9 177192.9 177192.9 177192.9 2 2 2 2 1 0 0 9662.1 9662.1 47540.8 0 PROCESSED 54329.5290162037 54247 54039.6651736111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001031 We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 0 SWG OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720 XIS N A426 49.9554 41.5039 150.58326426 -13.26576669 260.2176 53767.568900463 53768.5294560185 800010010 50398.6 50000 50406.6 50406.6 50398.6 50406.6 2 2 2 2 1 0 0 54436.4 54436.4 82975.8 0 PROCESSED 54405.6660532407 54247 54041.0862152778 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001036 A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas. EXTRAGALACTIC DIFFUSE SOURCES 8 A FABIAN ANDREW NULL NULL JAP 0 SWG THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER XIS N A3376 WEST RELIC 90.0415 -39.9946 246.43569548 -26.38071178 132.0018 53681.5938078704 53684.7883912037 800011010 126996.9 150000 126996.9 127180.9 127076.9 127028.9 2 2 2 2 1 0 0 112911.3 112911.3 230939.7 3 PROCESSED 54331.359375 54247 54037.6050231482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001039 We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO NULL NULL JAP 0 SWG SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 XIS N A3376 WEST RELIC 90.0363 -39.9917 246.43145562 -26.38385089 126.3601 54034.3950231482 54035.9176388889 800011020 62264.8 60000 62264.8 62264.8 62264.8 62264.8 2 2 2 2 1 0 0 55562.9 55562.9 131537.8 2 PROCESSED 54327.8698263889 54694 54090.2671643518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001039 We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO NULL NULL JAP 0 SWG SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 HXD Y ABELL 1795 207.2241 26.601 33.84733119 77.1817764 130.8638 53714.5034259259 53714.7752199074 800012010 13098.2 120000 13106.2 13098.2 13106.2 13106.2 1 1 1 1 1 0 0 10375.9 10375.9 23463.9 1 PROCESSED 54320.6911111111 54247 54038.7903703704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001056 We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. EXTRAGALACTIC DIFFUSE SOURCES 8 A BAUTZ MARK NULL NULL JAP 0 SWG TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 XIS N ABELL 1795 Near North 207.2221 26.7993 34.737463 77.20142043 130.7334 53714.7756481482 53715.3203587963 800012020 24410.6 25000 24426.6 24410.6 24442.6 24434.6 1 1 1 1 1 0 0 25179.8 25179.8 47055.9 2 PROCESSED 54320.8942476852 54247 54038.8804166667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001056 We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. EXTRAGALACTIC DIFFUSE SOURCES 8 A BAUTZ MARK NULL NULL JAP 0 SWG TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 XIS N ABELL 1795 Far North 207.223 26.9995 35.63943573 77.21561208 130.4264 53715.3208796296 53715.9730092593 800012030 30640.6 30000 30648.6 30640.6 30663.9 30656.6 2 2 2 2 1 0 0 27883.3 27883.3 56337.9 1 PROCESSED 54322.7007060185 54247 54039.1003703704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001056 We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. EXTRAGALACTIC DIFFUSE SOURCES 8 A BAUTZ MARK NULL NULL JAP 0 SWG TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 XIS N ABELL 1795 Near South 207.2228 26.4007 32.94964182 77.16185549 129.833 53715.9739467593 53716.5355787037 800012040 26074 25000 26098 26091.9 26074 26086 2 2 2 2 1 0 0 25798.6 25798.6 48522 1 PROCESSED 54327.0841203704 54247 54039.0706018518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001056 We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. EXTRAGALACTIC DIFFUSE SOURCES 8 A BAUTZ MARK NULL NULL JAP 0 SWG TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 XIS N ABELL 1795 Far South 207.2227 26.2001 32.0541753 77.13779505 129.4115 53716.5361921296 53717.4168865741 800012050 40120.6 30000 40136.6 40152.6 40120.6 40136.6 2 2 2 2 1 0 0 39437.3 39437.3 76081.9 1 PROCESSED 54324.2863773148 54247 54039.1460069445 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001056 We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. EXTRAGALACTIC DIFFUSE SOURCES 8 A BAUTZ MARK NULL NULL JAP 0 SWG TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 XIS N HCG62 193.274 -9.2022 303.62256693 53.66732525 113.6407 53755.3883333333 53758.5002199074 800013020 114848.8 100000 114856.8 114848.8 114848.8 114856.8 2 2 2 2 1 0 0 98783.6 98783.6 268849.8 4 PROCESSED 54331.1539583333 54247 54040.4546064815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001057 We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity. EXTRAGALACTIC DIFFUSE SOURCES 8 A OTA NAOMI NULL NULL JAP 0 SWG MEASURING HARD TAILS AND METAL DISTRIBUTIONS IN THE GALAXY GROUP HCG62 XIS N CENTAURUS CLUSTER 192.2012 -41.3132 302.40029759 21.55583076 106.2442 53731.2579050926 53732.1808333333 800014010 36519.2 30000 36519.2 36546.4 36546.4 36522.4 2 2 2 2 1 0 0 32149.8 32149.8 79739.9 0 PROCESSED 54326.8240509259 54247 54039.373900463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001070 A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 0 SWG OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER XIS N CENCL OFFSET1 192.2015 -41.4461 302.40210867 21.42294125 106.2765 53732.1811689815 53733.2502199074 800015010 44880.2 40000 44896.2 44904.2 44880.2 44919.6 2 2 2 2 1 0 0 37226.7 37226.7 92347.8 2 PROCESSED 54405.4815740741 54247 54039.5403472222 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001070 A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 0 SWG OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER XIS N CENCL OFFSET2 192.2009 -41.1804 302.39848339 21.68862024 106.52 53733.2507407407 53734.3543865741 800016010 43277.3 40000 43285.3 43285.3 43277.3 43293.3 2 2 2 2 1 0 0 35253.1 35253.1 95332 1 PROCESSED 54405.5282523148 54247 54039.6041203704 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001070 A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 0 SWG OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER XIS N NGC4388 186.4461 12.6674 279.11809751 74.34084148 119.622 53728.3779976852 53731.250162037 800017010 123634.1 100000 123924.9 125814.3 123634.1 124152.3 2 2 2 2 1 0 0 111820.9 111820.9 248128 3 PROCESSED 54331.4335416667 54247 54039.5984375 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001077 Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum. EXTRAGALACTIC DIFFUSE SOURCES 8 A TSURU TAKESHI NULL NULL JAP 0 SWG VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388 XIS N NGC 4636 190.7243 2.7556 297.77503713 65.54179663 112.2967 53710.1073726852 53711.9446643518 800018010 79201 80000 79201 79201 79201 79201 2 2 2 2 1 0 0 75777.1 75777.1 158727.8 2 PROCESSED 54330.4164930556 54247 54038.9551388889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001083 We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS. EXTRAGALACTIC DIFFUSE SOURCES 8 A FIGUEROA-FELICIANO ENECTALI NULL NULL JAP 0 SWG OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636 XIS N A 2218 CENTER 249.0052 66.205 97.72589248 38.11630228 233.3294 53669.4904050926 53670.1905555556 800019010 31935.4 35000 31943.4 31943.4 31935.4 31943.4 2 2 2 2 1 0 0 28937.1 28937.1 60487.9 1 PROCESSED 54327.1030555556 54247 54036.9596990741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001096 To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. EXTRAGALACTIC DIFFUSE SOURCES 8 A OHASHI TAKAYA NULL NULL JAP 0 SWG SEARCH FOR OXYGEN LINES FROM WARM IGM NULL N A 2218 OFFSETB 249.9091 65.2119 96.37864193 38.09205953 233.3309 53670.1916319444 53670.4620833333 800020010 14921.5 15000 14937.5 14933.5 14921.5 14941.5 2 2 2 2 1 0 0 14193.1 14193.1 23356.1 0 PROCESSED 54323.0796527778 54247 54036.8343981482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001096 To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. EXTRAGALACTIC DIFFUSE SOURCES 8 A OHASHI TAKAYA NULL NULL JAP 0 SWG SEARCH FOR OXYGEN LINES FROM WARM IGM NULL N NGC 2403 114.2007 65.5918 150.58117971 29.1798975 310.3004 53810.5896875 53811.5884143518 800021010 72368.7 70000 72376.7 72368.7 72376.7 72376.7 2 2 2 2 1 0 0 59359.1 59359.1 86277.9 0 PROCESSED 54323.8741087963 54247 54042.0667708333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 001101 We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission. EXTRAGALACTIC DIFFUSE SOURCES 8 A MAKISHIMA KAZUO NULL NULL JAP 0 SWG A PROPOSAL FOR A 70 KSEC SUZAKU OBSERVATION OF THE NORMAL SPIRAL GALAXY NGC 2403 XIS N A2104W 234.9146 -3.2969 2.73337641 39.30878407 117.9077 54121.3401388889 54121.8960532407 801001010 19926.9 20000 19926.9 19926.9 0 19926.9 1 1 0 1 1 0 0 17200.1 17200.1 48007.9 2 PROCESSED 54323.2674537037 54735 54137.0936805556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010012 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 1 AO1 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y A2104N 235.0318 -3.1802 2.94593816 39.29281704 117.689 54119.2779166667 54119.7522337963 801002010 18842.4 20000 18842.4 18842.4 0 18842.4 2 2 0 2 1 0 0 13644.8 13644.8 40977.9 1 PROCESSED 54322.5292708333 54735 54133.3893518518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010012 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 1 AO1 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y A2104E 235.1486 -3.297 2.9252225 39.1285511 117.6908 54118.1261226852 54118.6850231482 801003010 22784.7 20000 22784.7 22784.7 0 22784.7 2 2 0 2 1 0 0 17735.2 17735.2 48287.9 1 PROCESSED 54322.7539814815 54735 54132.8631365741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010012 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 1 AO1 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y A2104S 235.0317 -3.4139 2.71321412 39.14413145 117.9978 54120.3324884259 54120.8266087963 801004010 17323.4 20000 17323.4 17323.4 0 17323.4 2 2 0 2 1 0 0 13829.1 13829.1 42681.9 1 PROCESSED 54320.9102314815 54750 54137.3891898148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010012 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 1 AO1 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y RX J1347.5-1145 206.856 -11.8093 323.97916756 48.76108187 292.056 53916.7756597222 53918.7600115741 801013010 69661.1 75000 69661.1 69661.1 69661.1 69661.1 2 2 2 2 1 0 0 60982 60982 171375.9 0 PROCESSED 54327.6398263889 54394 53926.4810300926 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010014 We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 B OTA NAOMI NULL NULL JAP 1 AO1 BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 HXD N RX J1347.5-1145 206.8558 -11.8095 323.97878779 48.76095676 291.7151 53931.2858333333 53933.2551388889 801013020 79110.5 75000 79126.5 79110.5 79126.5 79134.5 2 2 2 2 1 0 0 69567 69567 170109.8 2 PROCESSED 54326.8262847222 54394 53942.463587963 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010014 We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 B OTA NAOMI NULL NULL JAP 1 AO1 BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 HXD N FORNAX A WEST LOBE 50.4184 -37.1645 240.1258488 -56.89722719 219.7525 54092.8700462963 54095.6113888889 801014010 93309.3 100000 93309.3 93309.3 0 93309.3 2 2 0 2 1 0 0 96371.6 96371.6 236835.8 5 PROCESSED 54330.0930902778 54735 54111.6821875 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010029 We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. EXTRAGALACTIC DIFFUSE SOURCES 8 C TASHIRO MAKOTO NULL NULL JAP 1 AO1 RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A HXD Y FORNAX A HOST GALAXY 50.6684 -37.2029 240.15407206 -56.69497357 218.3809 54091.6179976852 54092.8689699074 801015010 48721.7 50000 48721.7 48721.7 0 48721.7 2 2 0 2 1 0 0 48398.7 48398.7 108083.9 1 PROCESSED 54324.8278472222 54735 54132.9200347222 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010029 We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. EXTRAGALACTIC DIFFUSE SOURCES 8 C TASHIRO MAKOTO NULL NULL JAP 1 AO1 RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A XIS Y PKS 2356-61 359.7661 -60.908 314.02525269 -55.07790138 249.6445 54075.7140740741 54078.21625 801016010 100837.2 100000 100845.2 100837.2 0 100853.2 2 2 0 2 1 0 0 92125.5 92125.5 216157.9 3 PROCESSED 54710.8232291667 54456 54088.6546759259 2.2.8.20 3 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 010059 We propose a 100 ksec Suzaku observation of the radio galaxy PKS 2356-61. PKS 2356-61 is reported to reside in a group of galaxies, and a sign of a diffuse X-ray emission with a possibly high temperature surrounding PKS 2356-61 was suggested with ASCA. Our objective is the determination of the origin of the diffuse emission to evaluate AGN heating of the intragroup gas by PKS 2356-61. EXTRAGALACTIC DIFFUSE SOURCES 8 C HONG SOOJING NULL NULL JAP 1 AO1 HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61 XIS N NGC 507 20.9105 33.2598 130.6367604 -29.12969375 54.0771 53944.6189351852 53946.5544444444 801017010 79501.3 80000 79525.3 79501.3 79525.3 79525.3 2 2 2 2 1 0 0 80286.7 80286.7 167170 2 PROCESSED 54327.4814351852 54394 53955.7736689815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010061 We propose to observe luminous elliptical galaxies NGC 507 and NGC 499 for 80 and 100 ksec, respectively, to study abundance distribution of Fe and O. The good energy resolution and low background of the XIS instrument is crucial for this study, and we can perform the first reliable measurement of O distribution around elliptical galaxies. Comparison of O and Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. Comparison of NGC 507 and NGC 499 will show us how much metal production process differ with galaxy size. EXTRAGALACTIC DIFFUSE SOURCES 8 B SATO KOSUKE NULL NULL JAP 1 AO1 CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499 XIS N NGC 4631 190.5387 32.5478 142.74124336 84.2191655 139.0678 54067.1412615741 54068.9133217593 801019010 81076.1 80000 81084.1 81076.1 0 81084.1 2 2 0 2 1 0 0 74435.8 74435.8 153070 0 PROCESSED 54328.2123958333 54735 54088.6914699074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010062 We propose to observe a edge-on nearby starburst galaxy, NGC 4631 for an exposure time of 80 ksec. This observation will give us a ``template'' of ejecta from type II SNe with less than 30% accuracy of abandance of alpha elemements. EXTRAGALACTIC DIFFUSE SOURCES 8 C YAMASAKI NORIKO NULL NULL JAP 1 AO1 OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS XIS Y A399/401 FILAMENT 44.7475 13.2485 164.45015039 -39.12843885 74.1756 53966.1736921296 53969.4641666667 801020010 151060.1 150000 151060.1 151068.1 151068.1 151068.1 2 2 2 2 1 0 0 142203.6 142203.6 284273.8 5 PROCESSED 54330.7779513889 54526 54021.1056944444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010063 Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUJITA YUTAKA NULL NULL JAP 1 AO1 THE DETECTION OF WHIM IN THE A399/401 FILAMENT XIS N OPHIUCHUS CLUSTER 0 258.0174 -23.3865 0.50702706 9.33401192 88.8366 54183.0313078704 54183.5648726852 801021010 16641.1 15000 16641.1 16641.1 0 16641.1 2 2 0 2 1 0 0 13520.9 13520.9 46095.9 0 PROCESSED 54323.3271527778 54736 54209.5175462963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010065 The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUJITA YUTAKA NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER XIS Y OPHIUCHUS CLUSTER 1 258.2981 -23.3868 0.65649186 9.12279372 88.7031 54180.6159953704 54181.1398611111 801022010 24067 15000 24075 24067 0 24075 2 2 0 2 1 0 0 21821.3 21821.3 45254 1 PROCESSED 54323.2977083333 54736 54186.192650463 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010065 The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUJITA YUTAKA NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER XIS Y OPHIUCHUS CLUSTER 2 257.7375 -23.3864 0.3572282 9.54416529 94.9391 54181.1423726852 54181.825162037 801023010 24678.2 15000 24702.2 24694.2 0 24678.2 2 2 0 2 1 0 0 21278.1 21278.1 58987.9 1 PROCESSED 54323.3876388889 54736 54209.5433217593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010065 The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUJITA YUTAKA NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER XIS Y OPHIUCHUS CLUSTER 5 258.0184 -23.1077 0.73892155 9.49336651 88.7652 54181.8276736111 54182.4890277778 801026010 24255.7 15000 24255.7 24255.7 0 24255.7 2 2 0 2 1 0 0 19227.1 19227.1 57135.9 0 PROCESSED 54322.6967361111 54736 54186.2070949074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010065 The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUJITA YUTAKA NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER XIS Y OPHIUCHUS CLUSTER 8 258.0175 -23.6665 0.2749393 9.17298979 88.8988 54182.4897337963 54183.0308333333 801029010 23738.9 15000 23746.9 23738.9 0 23746.9 2 2 0 2 1 0 0 21678 21678 46746 0 PROCESSED 54323.2328587963 54736 54209.5725231482 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010065 The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUJITA YUTAKA NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER XIS Y OPHIUCHUS CLUSTER BG 257.0147 -25.0612 358.58755189 9.10838139 89.7146 54183.5662268518 54183.9169444444 801030010 15298.3 15000 15306.3 15306.3 0 15298.3 2 2 0 2 1 0 0 14635.1 14635.1 30296 0 PROCESSED 54320.6879050926 54736 54209.5187384259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010065 The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUJITA YUTAKA NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER XIS Y 3EGJ1234 1318_1 188.0173 -13.3363 295.70141073 49.26333697 109.7313 54081.3723032407 54081.9273032407 801031010 19409.8 20000 19417.8 19417.8 0 19409.8 2 2 0 2 1 0 0 18722.8 18722.8 47949.9 1 PROCESSED 54322.609537037 54735 54094.2359722222 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010068 We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. EXTRAGALACTIC DIFFUSE SOURCES 8 C TOTANI TOMONORI NULL NULL JAP 1 AO1 CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION HXD Y 3EGJ1234 1318_2 188.017 -13.0869 295.65674578 49.51103665 109.9322 54081.9277777778 54082.7766087963 801032010 30942.7 30000 30966.7 30958.7 0 30942.7 2 2 0 2 1 0 0 26083 26083 73333.9 1 PROCESSED 54322.8767476852 54735 54094.2665740741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010068 We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. EXTRAGALACTIC DIFFUSE SOURCES 8 C TOTANI TOMONORI NULL NULL JAP 1 AO1 CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION HXD Y AWM7 43.631 41.5933 146.34082925 -15.61629549 90.4997 53954.2348842593 53954.71625 801035010 18985.8 20000 18985.8 18985.8 18985.8 18985.8 2 2 2 2 1 0 0 17554.2 17554.2 41588 0 PROCESSED 54323.1701157407 54422 54020.7471759259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010076 The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. EXTRAGALACTIC DIFFUSE SOURCES 8 B OHASHI TAKAYA NULL NULL JAP 1 AO1 SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 XIS N AWM7 EAST OFFSET 44.0318 41.5949 146.61375919 -15.47239178 90.4995 53952.2676967593 53953.2398611111 801036010 38536.1 40000 38536.1 38536.1 38536.1 38536.1 1 1 1 1 1 0 0 37541 37541 83959.9 0 PROCESSED 54322.6825462963 54394 54020.7498726852 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010076 The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. EXTRAGALACTIC DIFFUSE SOURCES 8 B OHASHI TAKAYA NULL NULL JAP 1 AO1 SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 XIS N AWM7 WEST OFFSET 43.2295 41.594 146.06522235 -15.7568529 90.4999 53953.2407060185 53954.2343171296 801037010 39817.7 40000 39849.7 39817.7 39849.7 39849.7 2 2 2 2 1 0 0 38108.9 38108.9 85835.9 1 PROCESSED 54326.9776851852 54394 54020.7562384259 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010076 The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. EXTRAGALACTIC DIFFUSE SOURCES 8 B OHASHI TAKAYA NULL NULL JAP 1 AO1 SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 XIS N M87 CENTER 187.7366 12.4456 283.82387862 74.55209055 120.529 54068.9187037037 54071.1266666667 801038010 98183.1 100000 98183.1 98183.1 0 98183.1 1 1 0 1 1 0 0 88250.3 88250.3 190730.8 2 PROCESSED 54330.6221064815 54735 54090.4156134259 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010084 The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. EXTRAGALACTIC DIFFUSE SOURCES 8 C MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU HXD Y M87 50' SE 188.2678 11.8367 286.30035277 74.11241529 119.899 54071.127650463 54072.312037037 801039010 53637.4 50000 53637.4 53658.1 0 53645.4 2 2 0 2 1 0 0 46139.4 46139.4 102309 1 PROCESSED 54324.1604282407 54735 54088.5776736111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010084 The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. EXTRAGALACTIC DIFFUSE SOURCES 8 C MATSUMOTO HIRONORI NULL NULL JAP 1 AO1 NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU XIS Y A2319CENTER 290.3341 43.878 75.63759851 13.45022652 251.6652 54035.9326041667 54038.1466898148 801040010 99533.2 100000 99549.2 99541.2 99533.2 99549.2 2 2 2 2 1 0 0 93954.8 93954.8 191268 2 PROCESSED 54328.7315740741 54735 54063.5741666667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010085 We propose the observations of the A2319 cluster with the Suzaku HXD and XIS to investigate particle acceleration processes in the intracluster medium(ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will detect non-thermal hard X-ray with HXD, and determine the velocity difference between the two subclusters with XIS. With these results, we will determine dynamical status of the ICM and get implications on the particle acceleration processes. We will compare the results with theoretical models, numerical simulations, and radio and optical observations to get an overall picture of particle acceleration in clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 B TAKIZAWA MOTOKAZU NULL NULL JAP 1 AO1 PARTICLE ACCELERATION IN THE A2319 CLUSTER HXD Y A85 10.4739 -9.4292 115.23010576 -72.15810594 248.2856 54105.4020023148 54108.0557175926 801041010 99201.2 100000 99201.2 99201.2 0 99201.2 2 2 0 2 1 0 0 84813.9 84813.9 229242.1 2 PROCESSED 54329.8971643518 54735 54132.9388773148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010088 We propose observations of A2199 and A85 clusters of galaxies with an each exposure time of 100 ks, in order to search for excess hard X-ray emission, to constrain the spectral shape, and to discuss the origin of the hard X-ray emission. Both are listed as the clusters which are detected non-thermal emission signal with 2 sigma confidence level by Beppo SAX PDS detector. In addition, these two clusters only have features of brighter X-ray flux, good size, relatively cool ICM temperature, and including no bright member AGNs. Therefore they are suitable target samples for our observational purpose about estimation photon index and flux for the excess hard X-ray emission with high significance wherever possible. EXTRAGALACTIC DIFFUSE SOURCES 8 C SHIBATA RYO NULL NULL JAP 1 AO1 SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS HXD Y M31 10.6944 41.2627 121.18191229 -21.57961988 231.6592 54115.6775578704 54117.4572222222 801043010 99872.3 100000 99872.3 99872.3 0 99872.3 2 2 0 2 1 0 0 103912.4 103912.4 153723.8 1 PROCESSED 54328.2985069444 54744 54132.9457291667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010089 We propose the 100 ks Suzaku observation of the central region of Andromeda Nebula (M31). Our gaol is to detect 3 components (cool, hot and hard) of galactic diffuse X-ray emission (GDXE) with the XIS and HXD. This detection shows the existance of the GDXE hot and hard component in the extragalactic normal spiral galaxy, for the first time. EXTRAGALACTIC DIFFUSE SOURCES 8 C TAKAHASHI HIROMITSU NULL NULL JAP 1 AO1 DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA XIS Y COMA CLUSTER OFFSET 194.6939 27.9466 60.06105128 88.1791818 318.0815 53885.0996412037 53886.8384722222 801044010 79172 80000 79172 79172 79172 79172 2 2 2 2 1 0 0 75228.2 75228.2 150204.9 2 PROCESSED 54405.8277199074 54394 53926.7587384259 2.1.6.15 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010091 In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 1 AO1 THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER XIS N NGC 5044 198.8504 -16.3899 311.2339251 46.09520433 290.0016 53918.7631712963 53919.3600115741 801046010 19746.6 20000 19746.6 19746.6 19746.6 19746.6 2 2 2 2 1 0 0 17971.6 17971.6 51562 1 PROCESSED 54322.6661226852 54394 53930.6133217593 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010092 We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 1 AO1 THE METAL DISTRIBUTION OF THE NGC 5044 GROUP XIS N NGC 5044 OFFSET1 198.8505 -16.143 311.28196707 46.33985641 290.0004 53919.3604398148 53920.9599305556 801047010 54620.4 60000 54620.4 54620.4 54620.4 54620.4 2 2 2 2 1 0 0 45803.3 45803.3 138189.9 1 PROCESSED 54327.7891550926 54394 53942.4615740741 2.0.6.13 5 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010092 We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 1 AO1 THE METAL DISTRIBUTION OF THE NGC 5044 GROUP XIS N NGC 5044 OFFSET2 199.1117 -16.388 311.59229028 46.06278821 290.7836 53920.9609143518 53922.7598842593 801048010 62451 60000 62451 62451 62451 62451 2 2 2 2 1 0 0 57110.2 57110.2 155314.9 2 PROCESSED 54328.0385648148 54422 54034.2926736111 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010092 We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 1 AO1 THE METAL DISTRIBUTION OF THE NGC 5044 GROUP XIS N PERSEUS CL OFFSET 49.6445 42.068 150.06631202 -12.92163855 65.996 53980.0800925926 53980.7668287037 801049010 29243.8 30000 29255.9 29247.9 29251.8 29243.8 2 2 2 2 1 0 0 25672.9 25672.9 59329.9 1 PROCESSED 54322.7651041667 54526 54021.3135416667 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010097 We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 1 AO1 MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER HXD N PERSEUS CL OFFSET 49.2788 41.3719 150.2212005 -13.65398882 65.9966 53980.7676273148 53981.4543287037 801049020 32464.6 30000 32480.6 32464.6 32496.6 32488.6 1 1 1 1 1 0 0 28291.2 28291.2 59319.9 1 PROCESSED 54323.3007986111 54526 54021.2712731482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010097 We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 1 AO1 MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER HXD N PERSEUS CL OFFSET 50.2242 41.1004 150.98569591 -13.49005998 65.9967 53981.4552662037 53982.1418287037 801049030 32839.6 30000 32855.6 32847.6 32839.6 32863.6 1 1 1 1 1 0 0 31031.3 31031.3 59288 0 PROCESSED 54323.2247569444 54526 54020.8372106482 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010097 We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 1 AO1 MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER HXD N PERSEUS CL OFFSET 50.5735 41.8053 150.80595618 -12.75877318 65.9956 53982.1426736111 53982.4377893518 801049040 10420.6 30000 10420.6 10420.6 10420.6 10420.6 2 2 2 2 1 0 0 7540.2 7540.2 25467.9 1 PROCESSED 54320.656875 54526 54021.0033680556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010097 We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. EXTRAGALACTIC DIFFUSE SOURCES 8 A FUKAZAWA YASUSHI NULL NULL JAP 1 AO1 MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER HXD N Z348 16.7077 1.0407 131.03941429 -61.58850223 247.9196 54110.9286689815 54111.5259722222 801050010 22647.7 23000 22647.7 22647.7 0 22647.7 2 2 0 2 1 0 0 21340.3 21340.3 51589 1 PROCESSED 54322.6440277778 54735 54133.0321643518 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010098 We propose to carry out the Suzaku/XIS observations of 4 massive clusters at low redshifts (z <0.3). Combining the X-ray data with the existing Subaru datasets that allow us to directly reconstruct the mass distribution from the gravitational lensing measurements, we will investigate the physical relations between the mass and gas distributions to understand the nature of cluster in a quantitative way. EXTRAGALACTIC DIFFUSE SOURCES 8 C FUTAMASE TOSHIFUMI NULL NULL JAP 1 AO1 THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS XIS Y NGC3923 177.7599 -28.8047 287.27787622 32.22445477 293.1988 53899.8430671296 53902.7293287037 801054010 115820 120000 115828 115820 115828 115828 2 2 2 2 1 0 0 107731.3 107731.3 249352.8 3 PROCESSED 54330.6253472222 54394 53927.2880902778 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010100 We propose to observe an isolated elliptical galaxy NGC3923, to meaasure a dark matter distribution. The large effective area and stable low background of XIS enable us to measure a faint extended X-ray emission such as the periphery of elliptical galaxies more accurately than ever. Since X-ray bright elliptical galaxies have been found to be surrounded by group-scale emission, X-ray faint elliptical galaxies are the best to investigate the dark matter associated with the galaxy itself. The dark matter around galaxies is a key to resolve the problem of why X-ray bright and faint elliptical galaxies exist. The oxygen abundance distribution is also useful to probe the above issue. EXTRAGALACTIC DIFFUSE SOURCES 8 B FUKAZAWA YASUSHI NULL NULL JAP 1 AO1 ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923 XIS N A2142 239.5312 27.2879 44.29837206 48.74478569 138.1624 54104.1546990741 54105.3891666667 801055010 51452.5 60000 51460.5 51452.5 0 51460.5 2 2 0 2 1 0 0 49209.8 49209.8 106632 1 PROCESSED 54324.8951041667 54735 54111.417037037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010106 We propose to reveal the formation and evolution of dense core with cold fronts with SUZAKU/XIS. Our strategy of observation is based on the results of Chandra, ROSAT and weak lensing analysis. A2142 is a galaxy cluster which has contact discontinuities, "cold fronts", between cold-dense cores and hot-thin surrounding gas. We have carried out "weak lensing analysis" and derived mass map in A2142. We measure the bulk velocity via Fe-K line in the central region. We derive the merger velocity by observing the temperatures of the heating and non-heating which are expected by our observational results. It leads to understand the formation and evolution of dense core with cold fronts, since the merger and core velocities are closely related to the evolution of dense cores with cold fronts. EXTRAGALACTIC DIFFUSE SOURCES 8 C OKABE NOBUHIRO NULL NULL JAP 1 AO1 REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142 XIS Y ABELL 2199 CENTER 247.1922 39.484 62.84241749 43.66620611 252.3681 54009.2972222222 54009.8967361111 801056010 24928.2 25000 25479.9 24928.2 25479.9 25479.9 2 2 2 2 1 0 0 20519 20519 51793.9 1 PROCESSED 54322.5504398148 54735 54021.2246990741 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010138 Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. EXTRAGALACTIC DIFFUSE SOURCES 8 B KAWAHARADA MADOKA NULL NULL JAP 1 AO1 PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES HXD Y ABELL 2199 OFFSET 1 247.0269 39.6504 63.06766091 43.79825488 251.7923 54009.8973958333 54010.4467476852 801057010 24631.5 25000 24631.5 24631.5 24631.5 24631.5 2 2 2 2 1 0 0 25534.3 25534.3 47454 0 PROCESSED 54322.6262962963 54735 54021.2449189815 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010138 Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. EXTRAGALACTIC DIFFUSE SOURCES 8 B KAWAHARADA MADOKA NULL NULL JAP 1 AO1 PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES HXD Y ABELL 2199 OFFSET 2 247.3619 39.6495 63.07626508 43.54039287 251.2564 54011.5284722222 54012.1578587963 801058010 22707.2 25000 22723.2 22707.2 22723.2 22723.2 2 2 2 2 1 0 0 20704 20704 54360 0 PROCESSED 54323.3556018518 54735 54024.6719907407 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010138 Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. EXTRAGALACTIC DIFFUSE SOURCES 8 B KAWAHARADA MADOKA NULL NULL JAP 1 AO1 PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES HXD Y ABELL 2199 OFFSET 3 247.3596 39.3165 62.61707687 43.53145251 252.4737 54012.1589351852 54012.6786921296 801059010 25246.7 25000 25246.7 25246.7 25246.7 25246.7 1 1 1 1 1 0 0 20505 20505 44887.9 1 PROCESSED 54323.1807407407 54735 54025.4730092593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010138 Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. EXTRAGALACTIC DIFFUSE SOURCES 8 B KAWAHARADA MADOKA NULL NULL JAP 1 AO1 PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES HXD Y ABELL 2199 OFFSET 4 247.0296 39.3161 62.60481799 43.78660639 250.4756 54012.6800462963 54013.3044444444 801060010 24454.6 25000 24470.6 24462.6 24454.6 24477.5 2 2 2 2 1 0 0 25811 25811 53939.9 0 PROCESSED 54322.6147106482 54735 54024.6738888889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010138 Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. EXTRAGALACTIC DIFFUSE SOURCES 8 B KAWAHARADA MADOKA NULL NULL JAP 1 AO1 PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES HXD Y A2256 256.0138 78.7112 111.08264828 31.72462704 207.9671 54049.8560069445 54052.0834722222 801061010 95511.1 100000 95511.1 95511.1 0 95511.1 2 2 0 2 1 0 0 103578.9 103578.9 192441.8 4 PROCESSED 54405.8233333333 54456 54089.4338425926 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010139 A2256 is a nearby (z=0.058) rich cluster with strong X-ray emission. The cluster has variety of indications of a on-going merger; two peaks separated by 3.5 arcmin are clearly visible near the center of X-ray emission, gas temperature map show sub structure and a cold front etc. The velocity distribution of member galaxies also exhibits two or three sub groups in this cluster. We measure the bulk motion of the hot gas using Suzaku XIS, in particular, about 2000km/s velocity difference between the main-cluster and the sub-cluster is the target. We also aim to search for hard X-ray emission claimed by previous missions with Suzaku HXD. EXTRAGALACTIC DIFFUSE SOURCES 8 C HAYASHIDA KIYOSHI NULL NULL JAP 1 AO1 BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256 XIS N A1674 195.9676 67.5471 121.10331631 49.53698634 114.9985 54085.1434837963 54087.0426388889 801062010 68413.8 100000 68421.8 68421.8 0 68413.8 2 2 0 2 1 0 0 109013.1 109013.1 164064 2 PROCESSED 54327.4057060185 54750 54094.6003935185 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 010156 A1674 is a nearby (z=0.106) richness class 3 clsuter with Abell galaxy count of 165, while its X-ray luminsity is as low as 6e43erg/s. We have observed this cluster with ASCA and XMM-Newton, and found iregular extended X-ray emission. The X-ray spectrum can be fitted with a thin thermal model of kT ~ 3keV, but the metal abundance is 0.07 with upper limit of 0.2. We assume this cluster may be a cluster under construction. Utilizing the low background level and high sensitivity of Suzaku XIS, we aim to obtain accurate X-ray spectrum of this cluster to constrain the metal abndance of each species. We also examine possible contribution of diffuse non-thermal emission in cluster scale. EXTRAGALACTIC DIFFUSE SOURCES 8 C HAYASHIDA KIYOSHI NULL NULL JAP 1 AO1 METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674 XIS Y M101 210.8841 54.3679 101.97854462 59.72940376 150.2959 54062.5790625 54064.7182175926 801063010 98852.2 100000 98876.2 98852.2 0 98876.2 2 2 0 2 1 0 0 89612.5 89612.5 184802 2 PROCESSED 54405.84125 54455 54088.707650463 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011402 We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk. EXTRAGALACTIC DIFFUSE SOURCES 8 C KUNTZ K. NULL NULL USA 1 AO1 SOFT DIFFUSE X-RAY EMISSION FROM M101 XIS N NGC 4472 187.4441 8.005 286.9163593 70.20028227 117.8054 54072.8427893518 54075.7014699074 801064010 121035.8 120000 121035.8 121035.8 0 121035.8 2 2 0 2 1 0 0 103446.4 103446.4 246954.8 6 PROCESSED 54330.7686226852 54702 54089.1857523148 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011403 We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. EXTRAGALACTIC DIFFUSE SOURCES 8 B LOEWENSTEIN MICHAEL NULL NULL USA 1 AO1 INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU XIS Y NGC 4649 190.9148 11.557 295.86493189 74.32191724 113.3108 54098.4203703704 54104.1473263889 801065010 224030.4 120000 224030.4 224030.4 0 224030.4 2 2 0 2 1 0 0 26304.2 26304.2 69289.8 1 PROCESSED 54328.9267708333 54743 54132.9809027778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011403 We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. EXTRAGALACTIC DIFFUSE SOURCES 8 B LOEWENSTEIN MICHAEL NULL NULL USA 1 AO1 INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU XIS Y UGC03957 115.2433 55.429 162.22286538 28.93195726 271.243 53841.9927314815 53842.2828587963 801072010 10771.4 12000 10779.4 10779.4 10787.4 10771.4 1 1 1 1 1 0 0 9642 9642 25007.9 0 PROCESSED 54320.5244791667 54401 53906.7753240741 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A2572B 349.6066 18.7294 94.21850787 -38.90117923 59.1565 53922.7742939815 53923.3002199074 801073010 24059.5 21000 24075.5 24059.5 24067.5 24075.5 2 2 2 2 1 0 0 21495.1 21495.1 45397.9 1 PROCESSED 54322.5244675926 54401 53930.6043055556 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N Z8852 347.6318 7.5789 84.17423864 -47.55525942 260.3346 54065.5867013889 54066.1543287037 801074010 14852.6 15000 14852.6 14852.6 0 14852.6 2 2 0 2 1 0 0 13983.4 13983.4 49037.9 0 PROCESSED 54322.5510069444 54695 54088.6000694444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y IIZW108 318.5228 2.5728 53.56011975 -29.86052353 77.7227 53864.5319791667 53864.7883680556 801075010 11605.2 11000 11605.2 11605.2 11605.2 11605.2 2 2 2 2 1 0 0 9632 9632 22149.9 1 PROCESSED 54320.6820601852 54401 53913.9958564815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A2665 357.7161 6.1352 96.94047732 -53.65177278 245.9817 54078.2252893518 54078.562037037 801076010 13944 15000 13944 13944 0 13944 2 2 0 2 1 0 0 11607.3 11607.3 29087.9 0 PROCESSED 54320.483912037 54695 54089.271412037 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y A1831 209.8007 27.9693 40.05378223 74.96810077 288.1207 53937.1181828704 53937.5106481482 801077010 18079.6 18000 18079.6 18079.6 18079.6 18079.6 2 2 2 2 1 0 0 17089.1 17089.1 33897.9 1 PROCESSED 54320.8105324074 54401 53943.553599537 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A1800 207.3618 28.0973 40.59651819 77.12066844 302.3644 53936.635625 53937.1140509259 801078010 20043.7 17000 20047.3 20055.3 20055.3 20043.7 2 2 2 2 1 0 0 19000.3 19000.3 41331.9 0 PROCESSED 54320.9156481482 54401 53943.5299652778 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N Z8276 266.0474 32.9693 57.88393681 27.65216461 308.1365 53961.1406134259 53961.4723958333 801079010 14937.4 14000 14937.4 14937.4 14937.4 14937.4 1 1 1 1 1 0 0 15462 15462 28658 0 PROCESSED 54323.2745601852 54391 54018.6023842593 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A2495 342.5777 10.9124 81.20126485 -41.9387619 237.1467 54061.4694097222 54062.0787037037 801080010 18031.3 18000 18031.3 18367.3 0 18119.3 2 2 0 2 1 0 0 16389.1 16389.1 52633.9 3 PROCESSED 54322.5562847222 54695 54088.9563194444 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y A2495 342.5662 10.9218 81.19678392 -41.92445268 65.1354 54260.5857523148 54261.1668287037 801080020 25780.6 18000 25780.6 25780.6 0 25780.6 2 2 0 2 1 0 0 20976.2 20976.2 50195.9 2 PROCESSED 54323.2277893518 54695 54270.430625 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y A2061 230.3095 30.6453 48.13899774 57.1713197 293.2901 53943.6955092593 53943.9946643518 801081010 13888.7 14000 13904.7 13904.7 13888.7 13896.7 1 1 1 1 1 0 0 11844.3 11844.3 25839.9 0 PROCESSED 54323.2505324074 54401 53955.6442939815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A2249 257.46 34.4851 57.64541352 34.94797305 129.9858 54114.5939467593 54115.1252777778 801082010 22815.6 15000 22815.6 22823.6 0 22823.6 1 1 0 1 1 0 0 19763.7 19763.7 45903.9 1 PROCESSED 54320.8101157407 54695 54133.0295833333 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y Z235 10.9622 24.4059 120.72614401 -38.43334342 59.0539 53944.0060185185 53944.6148032407 801083010 20033.5 20000 20041.5 20041.5 20041.5 20033.5 2 2 2 2 1 0 0 19526.3 19526.3 52589.9 1 PROCESSED 54320.7510416667 54401 53955.6800925926 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A272 28.7603 33.9026 137.73606223 -27.1341127 64.9465 53943.0449537037 53943.6842476852 801084010 22245.5 21000 22253.5 22253.5 22245.5 22253.5 2 2 2 2 1 0 0 24603.5 24603.5 55231.9 0 PROCESSED 54323.3001851852 54401 53955.6516782407 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N A566 106.0915 63.2647 152.76309519 25.45548296 285.637 54178.3128587963 54178.8029976852 801085010 22271.1 20000 22271.1 22271.1 0 22271.1 2 2 0 2 1 0 0 22152.3 22152.3 42339.9 0 PROCESSED 54320.8916782407 54695 54185.9799305556 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B SCHARF CALEB NULL NULL USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y RXJ 0658 104.704 -55.933 266.02429497 -21.20357002 164.9362 54095.6181597222 54098.4099421296 801089010 101384.5 100000 101384.5 101384.5 0 101384.5 2 2 0 2 1 0 0 84384 84384 241138.9 2 PROCESSED 54330.9327662037 54702 54111.5842013889 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 011448 We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 C PETROSIAN VAHE NULL NULL USA 1 AO1 HARD X-RAY EMISSION FROM CLUSTER RXJ0658 HXD Y SN 1987A 83.9013 -69.2655 279.69660922 -31.92548266 330.0004 53894.6930555556 53895.6683449074 801090010 39646.4 40000 39646.4 39646.4 39646.4 39646.4 2 2 2 2 1 0 0 39251.9 39251.9 84239.9 0 PROCESSED 54322.9615740741 54400 53928.1346527778 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012006 In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar. EXTRAGALACTIC DIFFUSE SOURCES 8 B HASINGER G NTHER NULL NULL EUR 1 AO1 SN 1987A - A RUSTY REMNANT? XIS N ABELL 2204 248.0963 5.6404 21.10023438 33.35451369 261.3606 53995.3098958333 53996.5098958333 801091010 49111.3 55000 49111.3 49111.3 49111.3 49111.3 2 2 2 2 1 0 0 51937.2 51937.2 103643.9 1 PROCESSED 54322.9746643518 54526 54020.8840277778 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012018 Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii. EXTRAGALACTIC DIFFUSE SOURCES 8 B REIPRICH THOMAS NULL NULL EUR 1 AO1 A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS SPE N SERSIC 159-03 348.4959 -42.7314 348.33340728 -64.81387916 47.3295 53851.5323611111 53853.2668055556 801093010 67784.3 70000 67800.3 67800.3 67784.3 67792.3 2 2 2 2 1 0 0 41583.3 41583.3 149827.8 2 PROCESSED 54328.1256134259 54400 53907.8625231482 2.0.6.13 4 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 012045 We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku. EXTRAGALACTIC DIFFUSE SOURCES 8 A KAASTRA JELLE NULL NULL EUR 1 AO1 O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN? XIS N A3667_NW_RELIC 302.5617 -56.3599 341.42703548 -33.08195751 74.7123 53858.7409837963 53861.2933449074 801094010 94394.6 95000 94402.6 94394.6 94394.6 94402.6 3 3 3 3 1 0 0 56250.6 56250.6 220489 4 PROCESSED 54330.5487731482 54394 53913.7574189815 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013080 We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO SARAZIN CRAIG JUS 1 AO1 SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 HXD N A3667_NW_17OFF 302.8177 -56.56 341.18808838 -33.22347241 74.1682 53861.293912037 53861.7356944444 801095010 17258.6 20000 17282.6 17274.6 17266.6 17258.6 1 1 1 1 1 0 0 14255.5 14255.5 38151.9 1 PROCESSED 54320.7734953704 54735 53913.7593518518 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013080 We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO SARAZIN CRAIG JUS 1 AO1 SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 HXD N A3667_NW_17OFF 302.869 -56.6666 341.06051648 -33.2513141 258.9342 54038.8325578704 54039.0106944444 801095020 11963.4 10000 11979.4 11979.4 11963.4 11971.4 1 1 1 1 1 0 0 8724 8724 15383.9 0 PROCESSED 54320.5234027778 54735 54056.1858796296 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013080 We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO SARAZIN CRAIG JUS 1 AO1 SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 HXD Y A3667_CENTER 303.141 -56.7974 340.90266514 -33.39955413 74.263 53861.7363078704 53862.3843055556 801096010 20880.5 20000 20888.5 20888.5 20896.5 20880.5 1 1 1 1 1 0 0 8425 8425 55943.9 1 PROCESSED 54320.9182407407 54394 53913.7840509259 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 013080 We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO SARAZIN CRAIG JUS 1 AO1 SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 HXD N COMA RADIO HALO 194.9267 27.9061 56.39742233 88.00849705 295.2687 53886.8435300926 53890.7439699074 801097010 178657.2 180000 178689.2 178657.2 178713.2 178689.2 2 2 2 2 1 0 0 167450.6 167450.6 336975.8 7 PROCESSED 54331.6390972222 54401 53926.6760416667 2.0.6.13 3 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 014446 We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment. EXTRAGALACTIC DIFFUSE SOURCES 8 A SARAZIN CRAIG MATSUSHITA KYOKO USJ 1 AO1 NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER HXD N ABELL 262 CENTER 28.1922 36.1591 136.56609466 -25.08359968 69.9979 54329.1761921296 54330.0446643518 802001010 37164.5 36000 37164.5 37164.5 0 37164.5 2 2 0 2 1 0 0 34130.4 34130.4 75029.9 1 PROCESSED 54404.9359259259 54730 54350.5576851852 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020004 We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks. EXTRAGALACTIC DIFFUSE SOURCES 8 A MATSUSHITA KYOKO NULL NULL JAP 2 AO2 O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 XIS Y 3EGJ1234 1318_3 188.2697 -13.5708 296.11455637 49.05777767 113.9119 54445.0609375 54445.8543171296 802004010 1602 30000 1602 29779.4 0 29779.4 1 2 0 2 1 0 0 26304.8 26304.8 68519.8 0 PROCESSED 54629.2788310185 54999 54633.6933217593 2.2.8.20 2 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 020007 We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. EXTRAGALACTIC DIFFUSE SOURCES 8 C TOTANI TOMONORI NULL NULL JAP 2 AO2 CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION HXD Y 3EGJ1234 1318_4 188.5214 -13.4715 296.47032219 49.18242085 113.9125 54445.8547453704 54446.4655555556 802005010 20139.2 20000 0 20139.2 0 20155.2 0 2 0 2 1 0 0 20006.4 20006.4 52771.9 0 PROCESSED 54628.4840740741 55000 54633.6925347222 2.2.8.20 2 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 020007 We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. EXTRAGALACTIC DIFFUSE SOURCES 8 C TOTANI TOMONORI NULL NULL JAP 2 AO2 CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION HXD Y CEN45 192.5119 -41.3865 302.65166747 21.4844922 104.7288 54458.1467939815 54459.2294444444 802008010 58222.6 53000 58222.6 58236.5 0 58230.6 2 2 0 2 1 0 0 64517.1 64517.1 93521.8 2 PROCESSED 54486.1793402778 54854 54486.1941087963 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020011 We propose to obtain high-quality X-ray spectra of the subcluster region in the Centaurus cluster, Cen45, aiming at the first reliable detection of a supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that Cen45 is indeed in the process of merging and has a high velocity relative to the main cluster. Utilizing the high-sensitivity Suzaku/XIS spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be accurately measured from the Doppler shift of iron-K lines. With our proposed 40ks observation, we can put a strong constraint on the gas motion in the subcluster region. This will also have great impacts on our understanding of dynamical state of clusters and their evolution. EXTRAGALACTIC DIFFUSE SOURCES 8 B OTA NAOMI NULL NULL JAP 2 AO2 MEASURING GAS MOTIONS OF THE INFALLING SUBCLUSTER CEN45 XIS Y A963N 154.2645 39.1732 182.34163859 55.82043448 108.9136 54428.4751041667 54429.0522453704 802010010 29131.8 25000 29131.8 29141.3 0 29135.8 2 2 0 2 1 0 0 27884.3 27884.3 49838.1 0 PROCESSED 54434.2128703704 54804 54434.2199305556 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020018 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 2 AO2 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y A963E 154.4148 39.0556 182.51717965 55.95361494 109.3314 54427.8082060185 54428.4745833333 802011010 29082.5 25000 29082.5 29082.5 0 29082.5 2 2 0 2 1 0 0 24469.9 24469.9 57567.9 0 PROCESSED 54434.176724537 54804 54434.1859837963 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020018 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 2 AO2 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y A963S 154.2641 38.9388 182.75442962 55.85527134 107.1093 54432.4435300926 54432.9584953704 802012010 27717.2 25000 27725.2 27725.2 0 27717.2 2 2 0 2 1 0 0 25654.6 25654.6 44492 1 PROCESSED 54440.964212963 54811 54440.9716319444 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020018 We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. EXTRAGALACTIC DIFFUSE SOURCES 8 C HATTORI MAKOTO NULL NULL JAP 2 AO2 TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS XIS Y FORNAX CLUSTER N30' 54.7324 -34.9521 235.87381769 -53.55297023 245 54479.2031134259 54480.3542708333 802021010 55810.7 53000 55810.7 55810.7 0 55810.7 2 2 0 2 1 0 0 58344.1 58344.1 99443.8 2 PROCESSED 54490.3524884259 54864 54490.3658680556 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020038 To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings. EXTRAGALACTIC DIFFUSE SOURCES 8 C MATSUSHITA KYOKO NULL NULL JAP 2 AO2 DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES XIS Y NGC 4636 NORTH 190.6832 3.0555 297.61641621 65.83736523 111.9967 54441.2091087963 54443.0530555556 802022010 71429.4 67000 0 71429.4 0 71429.4 0 2 0 2 1 0 0 61781 61781 159310.1 3 PROCESSED 54629.3525347222 55000 54633.6943402778 2.2.8.20 2 Hea_15Apr2008_V6.4.1_Suzaku_15Apr2008_V8.0 020038 To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings. EXTRAGALACTIC DIFFUSE SOURCES 8 C MATSUSHITA KYOKO NULL NULL JAP 2 AO2 DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES XIS Y A1060_OFFSET 159.8425 -27.5312 270.15539037 26.80693828 96.4852 54425.0245486111 54427.7988888889 802028010 103799.3 100000 103799.3 103799.3 0 103799.3 2 2 0 2 1 0 0 89111.9 89111.9 239679.7 2 PROCESSED 54434.2202777778 54804 54434.2515509259 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020060 We propose to observe a 30' offset region of the cluster of galaxies Abell 1060 for 100 ksec to study the temperature and abundance profiles. The central region within ~0.3 times the virial radius, or 380 kpc, has been already observed as one of the SWG targets, and the temperature decrease and differnt profiles of metal abundances are clealy observed (Sato et al. 2006). This observation will reveal the temperature and abundance profiles to half the virial radius. Comparison of the abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the outer cluster region. EXTRAGALACTIC DIFFUSE SOURCES 8 C SATO KOSUKE NULL NULL JAP 2 AO2 TEMPERATURE AND ABUNDANCE PROFILES IN THE OUTER REGION OF THE NON-CD CLUSTER A1060 XIS Y A2142 OFFSET1 239.3897 27.3899 44.41448178 48.88746657 283.7323 54316.0523726852 54317.0211226852 802030010 37622.7 30000 37630.7 37622.7 0 37630.7 2 2 0 2 1 0 0 29667.7 29667.7 83687.9 1 PROCESSED 54404.9619560185 54723 54347.3816087963 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020076 We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 B OHASHI TAKAYA NULL NULL JAP 2 AO2 WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 XIS Y A2142 OFFSET2 239.2185 27.5666 44.63617571 49.06945571 260.7114 54358.4806597222 54360.0627893518 802031010 57718.7 50000 57718.7 57718.7 0 57718.7 1 1 0 1 1 0 0 52597.6 52597.6 136631.8 1 PROCESSED 54404.9724652778 54751 54371.4005208333 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020076 We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 B OHASHI TAKAYA NULL NULL JAP 2 AO2 WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 XIS Y A2142 OFFSET3 239.0356 27.7434 44.85726257 49.26078026 283.7312 54341.8454166667 54342.3960532407 802032010 23789.9 20000 23789.9 23789.9 0 23789.9 2 2 0 2 1 0 0 14242.5 14242.5 47569.9 0 PROCESSED 54404.9598842593 54724 54356.294849537 2.1.6.15 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020076 We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. EXTRAGALACTIC DIFFUSE SOURCES 8 B OHASHI TAKAYA NULL NULL JAP 2 AO2 WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 XIS Y ABELL 2744 3.5397 -30.3446 9.24871336 -81.22170813 53.4742 54239.5874652778 54243.7709953704 802033010 153233.2 150000 153241.2 153241.2 0 153233.2 2 2 0 2 1 0 0 133863.1 133863.1 361439.8 2 PROCESSED 54331.511099537 54745 54248.6974074074 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020077 We propose a 150 ks Suzaku observation of Abell 2744 aiming at non-thermal hard X-ray detection. It has a red-shift of 0.3, a radio-halo flux of 57 mJy at 1.4 GHz and ICM temperature of 9 keV. Our strategy here is to observe a luminous merging cluster hosting a bright radio halo, whilst avoiding the thermal ICM emission to overwhelm the 10-40 keV band, in which the HXD has the best sensitivity. The key is to look for relatively high red-shift cluster. Since the CMB density increases as (1+z)^4, the inverse Compton emission relative to the radio flux increases typically as (1+z)^2, while the thermal ICM emission is red-shifted. We believe this is one of the best method to utilize the Suzaku power for cluster hard X-ray survey. EXTRAGALACTIC DIFFUSE SOURCES 8 A NAKAZAWA KAZUHIRO NULL NULL JAP 2 AO2 HARD X-RAY VIEW OF A DISTANT RADIO-HALO CLUSTER ABELL2744 HXD Y MS 1512.4+3647 228.6059 36.6198 59.43888584 58.40149096 128.9265 54463.6508449074 54469.6946527778 802034010 268889.8 200000 268945.8 268889.8 0 268945.8 2 2 0 2 1 0 0 47480.3 47480.3 102801.9 2 PROCESSED 54542.2343981482 54909 54542.2596296296 2.2.7.18 2 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020086 Evolution of the amount of metals depends on history of super novae activities and metal tranport from inter-stellar space into the ICM. We observe a distant cluster, MS 1512+3647 (z=0.372), and determine the abundance ratio of alpha particles which are created by type II supernovae to iron by type Ia. This reveals the evolution of branch ratio of metals in a galaxy between stars and the ICM which has been unresolved observationally. EXTRAGALACTIC DIFFUSE SOURCES 8 B KAWAHARADA MADOKA NULL NULL JAP 2 AO2 EVOLUTION STUDY ON AMOUNT OF METALS IN THE ICM USING A DISTANT CLUSTER XIS Y ANTLIA CLUSTER 157.5092 -35.3277 272.94647188 19.18131972 90.0004 54423.2458796296 54425.0211111111 802035010 65952.8 60000 65960.8 65960.8 0 65952.8 2 2 0 2 1 0 0 58106.4 58106.4 153363.8 2 PROCESSED 54433.3706712963 54801 54433.3905092593 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020101 Suzaku observation of the non-cD cluster Abell 1060 shows that temperature of intra-cluster medium (ICM) increases toward the center. This phenomenon is exact opposite of that of giant cD clusters, in which temperature of the ICM decreases toward the center. To explain this observation, we have proposed that galaxies moving through the ICM interact magnetohydrodynamically with the ICM. This scenario implies that the galaxies have lost some part of their kinetic energies, while the ICM received the released energies. As a result, the ICM have been efficiently heated near the center in which galaxy number density is high. To strengthen our scenario, we propose to observation and study temperature map of the Antlia cluster which is another non-cD, relaxed, and nearby (z=0.0087) cluster. EXTRAGALACTIC DIFFUSE SOURCES 8 C KITAGUCHI TAKAO NULL NULL JAP 2 AO2 SUZAKU OBSERVATION OF NON-CD ANTLIA CLUSTER XIS Y FORNAX_GALACTIC_1 48.2958 -37.68 241.51144521 -58.49700193 45.4419 54279.8103240741 54280.3335532407 802037010 20417.5 20000 20417.5 20417.5 0 20417.5 1 1 0 1 1 0 0 16191.2 16191.2 45184 0 PROCESSED 54322.4253587963 54695 54322.4346064815 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020119 We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. EXTRAGALACTIC DIFFUSE SOURCES 8 B TAKEI YOH NULL NULL JAP 2 AO2 DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES XIS Y A2052_GALACTIC_1 225.6293 8.2927 7.81905694 53.73503279 292.5625 54295.7150810185 54296.5765509259 802038010 33733.4 30000 33733.4 33733.4 0 33733.4 1 1 0 1 1 0 0 30527.2 30527.2 74423.9 1 PROCESSED 54339.2890162037 54709 54339.4114583333 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020119 We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. EXTRAGALACTIC DIFFUSE SOURCES 8 B TAKEI YOH NULL NULL JAP 2 AO2 DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES XIS Y NGC4636_GALACTIC_1 192.513 5.4558 301.99802564 68.32503562 300.0459 54268.8414930556 54269.9307175926 802039010 41499.7 30000 41515.7 41507.7 0 41499.7 2 2 0 2 1 0 0 34337.1 34337.1 94047.9 0 PROCESSED 54319.4653240741 54695 54319.4765740741 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020119 We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. EXTRAGALACTIC DIFFUSE SOURCES 8 B TAKEI YOH NULL NULL JAP 2 AO2 DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES XIS Y FORNAX_GALACTIC_2 49.9904 -32.0719 230.76086762 -57.49880076 52.7651 54280.3368518518 54280.9897453704 802040010 21074.6 20000 21082.6 21082.6 0 21074.6 2 2 0 2 1 0 0 20131 20131 56393.9 1 PROCESSED 54322.4314467593 54696 54322.4474537037 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020119 We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. EXTRAGALACTIC DIFFUSE SOURCES 8 B TAKEI YOH NULL NULL JAP 2 AO2 DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES XIS Y AWM7 EAST OFFSET 44.9753 41.5792 147.26183994 -15.14450792 259.3934 54492.7386458333 54494.7016087963 802044010 85617.7 80000 85617.7 85617.7 0 85617.7 2 2 0 2 1 0 0 80600.3 80600.3 169583.8 1 PROCESSED 54515.2186689815 54888 54515.5758796296 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020139 The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. EXTRAGALACTIC DIFFUSE SOURCES 8 B ISHISAKI YOSHITAKA NULL NULL JAP 2 AO2 TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT XIS Y AWM7 SOUTH OFFSET 43.219 40.631 146.52769464 -16.61135361 257.3934 54494.7028703704 54496.618275463 802045010 31295.9 0 31303.9 31303.9 0 31295.9 2 2 0 2 1 0 0 78229.8 78229.8 165471.8 1 PROCESSED 54515.1538310185 54888 54515.1834837963 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020139 The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. EXTRAGALACTIC DIFFUSE SOURCES 8 B ISHISAKI YOSHITAKA NULL NULL JAP 2 AO2 TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT XIS Y AWM7 SOUTH OFFSET 43.2198 40.6314 146.52805812 -16.61071542 257.3937 54519.4104861111 54521.6112847222 802045020 91227.2 80000 91227.2 91227.2 0 91227.2 2 2 0 2 1 0 0 80028.5 80028.5 190113.9 2 PROCESSED 54535.2660763889 54904 54535.283599537 2.2.7.18 1 Hea_12Dec2007_V6.4_Suzaku_06Dec2007_V7.0 020139 The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. EXTRAGALACTIC DIFFUSE SOURCES 8 B ISHISAKI YOSHITAKA NULL NULL JAP 2 AO2 TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT XIS Y OPHIUCHUS CLUSTER 258.1093 -23.379 0.56233145 9.26925896 277.7852 54367.8835069444 54370.5939351852 802046010 100525 100000 100525 100525 0 100525 2 2 0 2 1 0 0 82949.5 82949.5 234161.9 3 PROCESSED 54402.5190046296 54770 54402.5613194444 2.1.6.15 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020143 The verification of the resonance scattering effect to resonance lines in an intracluster medium (ICM) is a big problem that has been carried over from ASCA. Though two interpretations for abnormality of intensity ratio of Fe-Kalpha/Fe Kbeta line, "resonance scattering effect" and "Ni overabundance", have been proposed, a determinate result has not been obtained. Both interpretations give a very big impact to the understanding of chemical evolution of ICM that has been obtained so far. To solve the problem, we propose the measurement of Ni and Fe lines with high precision for Ophiuchus cluster which is bright and hot enough for measuring the K lines. Moreover, this cluster is suggested the existence of non-thermal radiation from observations with Beppo-SAX, INTEGRAL, Swift. EXTRAGALACTIC DIFFUSE SOURCES 8 B FURUZAWA AKIHIRO NULL NULL JAP 2 AO2 APPROCHING RESONANCE SCATTERING/NI-OVERABUNDANCE PROBLEM IN THE OPHIUCHUS CLUSTER XIS Y COMA_45OFF 194.2558 27.5714 52.91406039 88.6829823 127.9482 54436.4228703704 54437.2085185185 802047010 31615.1 30000 31615.1 31615.1 0 31615.1 2 2 0 2 1 0 0 26169.1 26169.1 67824 0 PROCESSED 54445.1521759259 54814 54445.1600925926 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020149 With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays. EXTRAGALACTIC DIFFUSE SOURCES 8 C INOUE SUSUMU NULL NULL JAP 2 AO2 EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER HXD Y COMA_60OFF 194.0251 27.4252 49.19228369 88.92228234 126.7582 54438.1998726852 54439.1946990741 802048010 36666.9 30000 36666.9 36666.9 0 36666.9 2 2 0 2 1 0 0 31696.2 31696.2 85921.9 1 PROCESSED 54445.288912037 54814 54445.3011689815 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 020149 With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays. EXTRAGALACTIC DIFFUSE SOURCES 8 C INOUE SUSUMU NULL NULL JAP 2 AO2 EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER HXD Y NGC 1553 64.0253 -55.7788 265.63371114 -43.7014546 176.9406 54429.7042939815 54431.9029976852 802050010 98722.2 95000 98722.2 98722.2 0 98722.2 2 2 0 2 1 0 0 87790.3 87790.3 189915.9 2 PROCESSED 54438.4005324074 54806 54438.4258101852 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021401 As driving engines of metal enrichment, early-type galaxies provide vital laboratories to investigate how it operates. In our Chandra survey of galaxies, we found solar ISM abundances (Zfe), similar to the stars and implying enrichment homology from clusters to moderate-Lx galaxies. The only outlier was NGC1553, for which we found a tantalizing hint of very subsolar Zfe, inconsistent with simple models. Unlike other galaxies with recent reports of low Zfe, NGC1553 has a bright gas halo, so the results are insensitive to the modelling of unresolved LMXB. We propose an 80ks observation of NGC1553 to measure definitively the ISM abundances of Fe and other crucial diagnostic elements. These data will either confirm enrichment bimodality or provide a vital low-Lx data-point to anchor models. EXTRAGALACTIC DIFFUSE SOURCES 8 C HUMPHREY PHILIP NULL NULL USA 2 AO2 NGC 1553: PROOF OF BIMODAL METAL ENRICHMENT? XIS Y DRACO 260.0265 57.929 86.38548758 34.73420948 52.1224 54196.7611458333 54198.2216898148 802051010 63323.2 67000 63323.2 63323.2 0 63323.2 2 2 0 2 1 0 0 64957.2 64957.2 126181.8 2 PROCESSED 54324.7246875 54829 54203.3603703704 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021405 We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. EXTRAGALACTIC DIFFUSE SOURCES 8 A LOEWENSTEIN MICHAEL NULL NULL USA 2 AO2 SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES XIS Y URSA MINOR 227.2517 67.2307 104.9865755 44.80382561 40.7921 54195.7731944444 54196.7557175926 802052010 70882.3 67000 70890.3 70882.3 0 70890.3 2 2 0 2 1 0 0 59587.2 59587.2 84876 1 PROCESSED 54322.9199305556 54695 54203.3200462963 2.0.6.13 2 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021405 We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. EXTRAGALACTIC DIFFUSE SOURCES 8 A LOEWENSTEIN MICHAEL NULL NULL USA 2 AO2 SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES XIS Y BOOTES GROUP 7 217.7796 35.0938 59.62119131 67.30227758 316.719 54266.3117592593 54267.3863310185 802053010 42124.4 38000 42132.4 42124.4 0 42132.4 2 2 0 2 1 0 0 37338.4 37338.4 92823.8 0 PROCESSED 54322.4493402778 54695 54322.4630324074 2.0.6.13 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021424 We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. EXTRAGALACTIC DIFFUSE SOURCES 8 B BAUTZ MARSHALL NULL NULL USA 2 AO2 SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES XIS Y BOOTES GROUP 1 218.7136 35.7235 60.71261374 66.41229506 153.2269 54440.1222106482 54441.2015972222 802054010 42224.2 38000 42224.2 42224.2 0 42224.2 2 2 0 2 1 0 0 41302.3 41302.3 93254 0 PROCESSED 54448.2139236111 54815 54448.2273842593 2.1.6.16 1 Hea_27Jul2007_V6.3.1_Suzaku_24Jul2007_V6.0 021424 We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. d