DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 1259
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | Crab Nebula | 83.6449 | 22.0152 | 82.892626 | 21.982571 | 84.11016 | -1.295832 | 184.56274906 | -5.77473152 | 84.9987 | 53614.1083449074 | 2005-09-01 02:36:01 | 53614.1771759259 | 2005-09-01 04:15:08 | 100015030 | 2.1 | 5 | 2.1 | 2.1 | 2.1 | 2.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.3074 | 2.3074 | 5.9439 | 0 | PROCESSED | 57527.235150463 | 2016-05-19 05:38:37 | 54247 | 2007-05-27 00:00:00 | 54109.3966782407 | 2007-01-09 09:31:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD boresight check with Crab | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015030/ | |||||
2 | E0102-72 | 15.9884 | -72.0403 | 15.58329 | -72.308299 | 314.593543 | -65.036118 | 301.56673438 | -45.05476105 | 119.5512 | 53595.2489236111 | 2005-08-13 05:58:27 | 53595.4618518518 | 2005-08-13 11:05:04 | 100001020 | 4.1598 | 10 | 4.1598 | 4.1598 | 4.1598 | 4.1598 | 1 | 1 | 1 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6779861111 | 2016-05-12 16:16:18 | 54247 | 2007-05-27 00:00:00 | 54035.6312731482 | 2006-10-27 15:09:02 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000001 | XIS door open with a SMC SNR E0102-72 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | XIS door open | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100001020/ | Quick Look | ![]() |
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3 | N132D | 81.2751 | -69.6506 | 81.377584 | -69.69262 | 312.405312 | -85.522517 | 280.31335191 | -32.77744994 | 53.3312 | 53598.2402777778 | 2005-08-16 05:46:00 | 53598.5140046296 | 2005-08-16 12:20:10 | 100002060 | 5.9635 | 7 | 5.9635 | 5.9635 | 5.9635 | 5.9635 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6925115741 | 2016-05-12 16:37:13 | 54247 | 2007-05-27 00:00:00 | 54038.4700810185 | 2006-10-30 11:16:55 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD HV ON WITH N132D | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002060/ | Quick Look | ![]() |
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4 | DEM_L71/N23 | 76.4474 | -67.958 | 76.476582 | -68.023213 | 338.826937 | -84.59461 | 278.75859594 | -34.83581885 | 70.5849 | 53598.5206365741 | 2005-08-16 12:29:43 | 53599.6042592593 | 2005-08-17 14:30:08 | 100003010 | 5.7897 | 40 | 5.7897 | 5.7897 | 5.7897 | 5.7897 | 2 | 2 | 2 | 2 | 0 | 0 | 0 | 0 | 0 | 93.6061 | 0 | PROCESSED | 57520.7098611111 | 2016-05-12 17:02:12 | 54247 | 2007-05-27 00:00:00 | 54035.7018171296 | 2006-10-27 16:50:37 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000003 | LMC SNRs L71/N23 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | LMC SNRs | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100003010/ | Quick Look | ![]() |
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5 | A 2052 | 229.2779 | 6.8766 | 228.662841 | 7.059342 | 224.77082 | 24.150691 | 9.31339919 | 49.96215441 | 281.2328 | 53602.4238078704 | 2005-08-20 10:10:17 | 53602.743287037 | 2005-08-20 17:50:20 | 100006010 | 13.9021 | 20 | 13.9021 | 13.9021 | 13.9021 | 13.9021 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13.4163 | 13.4163 | 27.5839 | 0 | PROCESSED | 57520.7207407407 | 2016-05-12 17:17:52 | 53705 | 2005-12-01 00:00:00 | 53905.4607523148 | 2006-06-19 11:03:29 | 3.0.22.43 | 11 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Outer region of A 2052 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006010/ | Quick Look | ![]() |
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6 | A 2052 | 229.3237 | 7.1059 | 228.709513 | 7.288472 | 224.747048 | 24.38343 | 9.64711471 | 50.05514889 | 281.2373 | 53602.7440393518 | 2005-08-20 17:51:25 | 53603.3406944445 | 2005-08-21 08:10:36 | 100006020 | 25.7431 | 20 | 25.7431 | 25.7431 | 25.7431 | 25.7431 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21.0642 | 21.0642 | 51.5199 | 0 | PROCESSED | 57520.7246527778 | 2016-05-12 17:23:30 | 53705 | 2005-12-01 00:00:00 | 53905.4610300926 | 2006-06-19 11:03:53 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Outer region of A 2052 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006020/ | Quick Look | ![]() |
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7 | A 2052 | 229.0933 | 7.1516 | 228.479191 | 7.335016 | 224.492199 | 24.361996 | 9.50335527 | 50.26933049 | 281.2093 | 53603.3412615741 | 2005-08-21 08:11:25 | 53603.6114351852 | 2005-08-21 14:40:28 | 100006030 | 12.969 | 20 | 12.969 | 12.969 | 12.969 | 12.969 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13.1413 | 13.1413 | 23.3279 | 0 | PROCESSED | 57520.7271527778 | 2016-05-12 17:27:06 | 53705 | 2005-12-01 00:00:00 | 53905.4613310185 | 2006-06-19 11:04:19 | 3.0.22.43 | 9 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Outer region of A 2052 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006030/ | Quick Look | ![]() |
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8 | A 2052 | 229.3311 | 7.2632 | 228.717502 | 7.445744 | 224.705557 | 24.536292 | 9.85579143 | 50.13807877 | 91.2371 | 53762.482650463 | 2006-01-27 11:35:01 | 53762.9209953704 | 2006-01-27 22:06:14 | 100006050 | 22.366 | 20 | 22.366 | 22.366 | 22.366 | 22.366 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.388 | 20.388 | 37.8659 | 0 | PROCESSED | 57532.800162037 | 2016-05-24 19:12:14 | 54247 | 2007-05-27 00:00:00 | 54040.5318634259 | 2006-11-01 12:45:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Outer region of A 2052 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006050/ | Quick Look | ![]() |
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9 | NGC 4945 | 196.3681 | -49.4152 | 195.638243 | -49.147517 | 216.98939 | -38.593586 | 305.27752827 | 13.39262005 | 96.1296 | 53750.3365625 | 2006-01-15 08:04:39 | 53752.9655092593 | 2006-01-17 23:10:20 | 100008030 | 95.0663 | 10 | 95.0817 | 95.1297 | 95.0663 | 95.1063 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 84.9813 | 84.9813 | 227.1157 | 2 | PROCESSED | 57532.7353240741 | 2016-05-24 17:38:52 | 54247 | 2007-05-27 00:00:00 | 54040.3587615741 | 2006-11-01 08:36:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000008 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | NGC 4945 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100008030/ | Quick Look | ![]() |
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10 | PSR1509-58 | 228.4798 | -59.0943 | 227.494741 | -58.907902 | 243.862404 | -39.360151 | 320.34145971 | -1.12587132 | 287.6342 | 53605.36 | 2005-08-23 08:38:24 | 53606.8597569444 | 2005-08-24 20:38:03 | 100009010 | 65.1618 | 60 | 65.1618 | 65.3227 | 65.2427 | 65.2427 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 49.7357 | 49.7357 | 129.5298 | 4 | PROCESSED | 57526.9045486111 | 2016-05-18 21:42:33 | 53705 | 2005-12-01 00:00:00 | 53905.4622337963 | 2006-06-19 11:05:37 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000009 | HXD spectrum and timing check | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | PSR1509-58 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100009010/ | Quick Look | ![]() |
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11 | Crab Nebula | 83.6267 | 22.0751 | 82.874095 | 22.042383 | 84.095945 | -1.235244 | 184.50282132 | -5.75691305 | 86.8655 | 53607.0070833333 | 2005-08-25 00:10:12 | 53607.1389814815 | 2005-08-25 03:20:08 | 100010010 | 2.9379 | 5 | 2.9379 | 2.9379 | 2.9379 | 2.9379 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 3.4387 | 3.4387 | 11.3819 | 0 | PROCESSED | 57526.8678703704 | 2016-05-18 20:49:44 | 54247 | 2007-05-27 00:00:00 | 54118.9886689815 | 2007-01-18 23:43:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010010/ | Quick Look | ![]() |
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12 | Crab nebula | 83.6336 | 21.9568 | 82.881657 | 21.924117 | 84.097114 | -1.353715 | 184.60669551 | -5.81484075 | 86.8687 | 53607.1394560185 | 2005-08-25 03:20:49 | 53607.2779282407 | 2005-08-25 06:40:13 | 100010020 | 3.6533 | 5 | 3.6533 | 3.6533 | 3.6533 | 3.6533 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.8067 | 3.8067 | 11.934 | 0 | PROCESSED | 57526.8772337963 | 2016-05-18 21:03:13 | 54247 | 2007-05-27 00:00:00 | 54118.9337615741 | 2007-01-18 22:24:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010020/ | Quick Look | ![]() |
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13 | Crab nebula | 83.6511 | 21.6763 | 82.900722 | 21.643705 | 84.100986 | -1.634666 | 184.85366771 | -5.95118505 | 86.8795 | 53607.5153125 | 2005-08-25 12:22:03 | 53607.7153472222 | 2005-08-25 17:10:06 | 100010040 | 9.5806 | 5 | 9.5806 | 9.5806 | 9.5806 | 9.5806 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.1783 | 8.1783 | 17.248 | 0 | PROCESSED | 57526.8981828704 | 2016-05-18 21:33:23 | 54247 | 2007-05-27 00:00:00 | 54118.943125 | 2007-01-18 22:38:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010040/ | Quick Look | ![]() |
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14 | Crab nebula | 83.5677 | 22.0135 | 82.815455 | 21.980499 | 84.038563 | -1.294359 | 184.52566905 | -5.83608695 | 86.8444 | 53607.9175810185 | 2005-08-25 22:01:19 | 53608.0695023148 | 2005-08-26 01:40:05 | 100010060 | 4.8779 | 5 | 4.8779 | 4.8779 | 4.8779 | 4.8779 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5.0217 | 5.0217 | 13.076 | 0 | PROCESSED | 57526.9066087963 | 2016-05-18 21:45:31 | 54247 | 2007-05-27 00:00:00 | 54122.4195486111 | 2007-01-22 10:04:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010060/ | Quick Look | ![]() |
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15 | Crab nebula | 83.6922 | 22.0221 | 82.939876 | 21.989699 | 84.154283 | -1.290862 | 184.58047361 | -5.73399538 | 86.8671 | 53608.0699768518 | 2005-08-26 01:40:46 | 53608.2084027778 | 2005-08-26 05:00:06 | 100010070 | 4.0899 | 5 | 4.0899 | 4.0899 | 4.0899 | 4.0899 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4.2283 | 4.2283 | 11.9259 | 0 | PROCESSED | 57526.9072222222 | 2016-05-18 21:46:24 | 54247 | 2007-05-27 00:00:00 | 54119.0149074074 | 2007-01-19 00:21:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010070/ | Quick Look | ![]() |
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16 | Crab nebula | 83.5807 | 22.8483 | 82.82374 | 22.81535 | 84.087744 | -0.460898 | 183.82410841 | -5.37832099 | 86.8677 | 53608.3175810185 | 2005-08-26 07:37:19 | 53608.5139583333 | 2005-08-26 12:20:06 | 100010090 | 6.716 | 5 | 6.716 | 6.716 | 6.716 | 6.716 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6.3768 | 6.3768 | 16.9501 | 0 | PROCESSED | 57526.9164699074 | 2016-05-18 21:59:43 | 54247 | 2007-05-27 00:00:00 | 54119.0235648148 | 2007-01-19 00:33:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010090/ | Quick Look | ![]() |
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17 | Crab nebula | 83.5122 | 24.0135 | 82.748583 | 23.980205 | 84.077056 | 0.70598 | 182.80375415 | -4.80497322 | 86.8675 | 53608.7179976852 | 2005-08-26 17:13:55 | 53608.930625 | 2005-08-26 22:20:06 | 100010110 | 9.4805 | 5 | 9.4805 | 9.4805 | 9.4805 | 9.4805 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 7.363 | 7.363 | 18.336 | 0 | PROCESSED | 57526.9265162037 | 2016-05-18 22:14:11 | 54247 | 2007-05-27 00:00:00 | 54118.98625 | 2007-01-18 23:40:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010110/ | Quick Look | ![]() |
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18 | Crab nebula | 83.6374 | 21.9009 | 82.885769 | 21.868236 | 84.09817 | -1.409717 | 184.65605757 | -5.84178049 | 86.8664 | 53608.9333217593 | 2005-08-26 22:23:59 | 53609.069525463 | 2005-08-27 01:40:07 | 100010120 | 4.7456 | 5 | 4.7456 | 4.7456 | 4.7456 | 4.7456 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 5.1787 | 5.1787 | 11.7579 | 1 | PROCESSED | 57526.9343287037 | 2016-05-18 22:25:26 | 54247 | 2007-05-27 00:00:00 | 54118.9946180556 | 2007-01-18 23:52:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010120/ | Quick Look | ![]() |
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19 | Crab nebula | 83.5044 | 22.0116 | 82.752181 | 21.978293 | 83.979835 | -1.293628 | 184.49566519 | -5.88665136 | 86.8658 | 53609.0701388889 | 2005-08-27 01:41:00 | 53609.2014583333 | 2005-08-27 04:50:06 | 100010130 | 4.222 | 5 | 4.222 | 4.222 | 4.222 | 4.222 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4.3724 | 4.3724 | 11.3359 | 0 | PROCESSED | 57526.9346180556 | 2016-05-18 22:25:51 | 54247 | 2007-05-27 00:00:00 | 54119.0454282407 | 2007-01-19 01:05:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010130/ | Quick Look | ![]() |
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20 | Galactic bulge | 236.4313 | -31.7013 | 235.648361 | -31.545749 | 241.296308 | -11.543137 | 340.99994533 | 17.99808229 | 283.5446 | 53609.4365856482 | 2005-08-27 10:28:41 | 53611.060625 | 2005-08-29 01:27:18 | 100011010 | 61.133 | 70 | 61.133 | 61.133 | 61.133 | 61.133 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 47.9834 | 47.9834 | 140.282 | 2 | PROCESSED | 57526.962037037 | 2016-05-18 23:05:20 | 54247 | 2007-05-27 00:00:00 | 54034.8288310185 | 2006-10-26 19:53:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000011 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Galactic bulge | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100011010/ | Quick Look | ![]() |
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21 | Eta Carinae | 161.281 | -59.6845 | 160.794333 | -59.421136 | 202.162077 | -58.916082 | 287.6040589 | -0.62575348 | 343.8621 | 53611.0750347222 | 2005-08-29 01:48:03 | 53612.0627546296 | 2005-08-30 01:30:22 | 100012010 | 49.782 | 40 | 49.79 | 49.782 | 49.782 | 49.798 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55.9607 | 55.9607 | 85.2529 | 0 | PROCESSED | 57526.9773032407 | 2016-05-18 23:27:19 | 53705 | 2005-12-01 00:00:00 | 53905.4648842593 | 2006-06-19 11:09:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000012 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Eta Carinae | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100012010/ | Quick Look | ![]() |
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22 | N103B | 77.2315 | -68.7507 | 77.290508 | -68.812132 | 329.838884 | -84.691105 | 279.61119012 | -34.36730962 | 73.8586 | 53612.0740162037 | 2005-08-30 01:46:35 | 53613.0626273148 | 2005-08-31 01:30:11 | 100013010 | 33.0646 | 40 | 33.0646 | 33.0646 | 33.0646 | 33.0646 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.2814 | 37.2814 | 85.4059 | 1 | PROCESSED | 57526.9730324074 | 2016-05-18 23:21:10 | 54247 | 2007-05-27 00:00:00 | 54034.8733449074 | 2006-10-26 20:57:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000013 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | N103B | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100013010/ | Quick Look | ![]() |
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23 | E0102-72 | 15.9813 | -72.0378 | 15.57605 | -72.305808 | 314.596715 | -65.033076 | 301.56958331 | -45.05740554 | 140.1798 | 53613.0710648148 | 2005-08-31 01:42:20 | 53613.7640509259 | 2005-08-31 18:20:14 | 100014010 | 24.3339 | 20 | 24.3339 | 24.3339 | 24.3339 | 24.3339 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.5144 | 24.5144 | 59.8639 | 2 | PROCESSED | 57511.5174884259 | 2016-05-03 12:25:11 | 53705 | 2005-12-01 00:00:00 | 53905.4615740741 | 2006-06-19 11:04:40 | 3.0.22.43 | 13 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000014 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | XIS monitor with E0102-72 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100014010/ | Quick Look | ![]() |
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24 | Crab Nebula | 83.6296 | 22.1792 | 82.876409 | 22.146495 | 84.103227 | -1.131361 | 184.41590928 | -5.69889955 | 84.9998 | 53613.9762152778 | 2005-08-31 23:25:45 | 53614.1077314815 | 2005-09-01 02:35:08 | 100015020 | 4.95 | 5 | 4.95 | 4.95 | 4.95 | 4.95 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5.1178 | 5.1178 | 11.3599 | 0 | PROCESSED | 57527.2276388889 | 2016-05-19 05:27:48 | 54247 | 2007-05-27 00:00:00 | 54109.1090972222 | 2007-01-09 02:37:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD boresight check with Crab | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015020/ | Quick Look | ![]() |
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25 | SN1006 SW BG | 224.655 | -42.4005 | 223.837497 | -42.201017 | 234.783022 | -24.341132 | 326.632731 | 14.54333558 | 310.4886 | 53624.9999189815 | 2005-09-11 23:59:53 | 53626.0071643518 | 2005-09-13 00:10:19 | 100019040 | 32.3334 | 50 | 32.3334 | 32.3494 | 32.3414 | 32.3414 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.6736 | 24.6736 | 87.0159 | 5 | PROCESSED | 57527.3647453704 | 2016-05-19 08:45:14 | 54247 | 2007-05-27 00:00:00 | 54035.4482638889 | 2006-10-27 10:45:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | SN1006 observation with XIS and HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019040/ | Quick Look | ![]() |
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26 | SN1006 SW BG | 224.6468 | -42.4025 | 223.829311 | -42.202989 | 234.777387 | -24.344913 | 326.62625739 | 14.54451897 | 100.3489 | 53761.7199652778 | 2006-01-26 17:16:45 | 53762.4752777778 | 2006-01-27 11:24:24 | 100019060 | 27.9813 | 50 | 27.9813 | 27.9893 | 27.9973 | 27.9973 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 29.5504 | 29.5504 | 65.2499 | 2 | PROCESSED | 57532.7989814815 | 2016-05-24 19:10:32 | 54247 | 2007-05-27 00:00:00 | 54040.5663541667 | 2006-11-01 13:35:33 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | SN1006 observation with XIS and HXD | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019060/ | Quick Look | ![]() |
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27 | Fornax Cluster | 54.6395 | -35.4918 | 54.160816 | -35.653913 | 38.755932 | -52.830853 | 236.7850293 | -53.61976834 | 103.5002 | 53626.0756018518 | 2005-09-13 01:48:52 | 53627.5002662037 | 2005-09-14 12:00:23 | 100020010 | 76.0782 | 100 | 76.0782 | 76.0782 | 76.0782 | 76.0782 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 71.1128 | 71.1128 | 123.0639 | 3 | PROCESSED | 57527.3377430556 | 2016-05-19 08:06:21 | 54247 | 2007-05-27 00:00:00 | 54035.4442013889 | 2006-10-27 10:39:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000020 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Fornax Cluster | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100020010/ | Quick Look | ![]() |
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28 | Crab Nebula | 82.7325 | 21.9883 | 81.980613 | 21.951274 | 83.263643 | -1.282782 | 184.12771921 | -6.50224239 | 88.0978 | 53628.3006828704 | 2005-09-15 07:12:59 | 53628.5835416667 | 2005-09-15 14:00:18 | 100022020 | 10.9198 | 10 | 10.9198 | 10.9198 | 10.9198 | 10.9198 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6.3401 | 6.3401 | 24.4 | 2 | PROCESSED | 57527.3262615741 | 2016-05-19 07:49:49 | 54247 | 2007-05-27 00:00:00 | 54109.1486342593 | 2007-01-09 03:34:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000022 | Crab at 50arcmin off from the XIS aimpoint to study stray light. | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab at 50 arcmin off | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022020/ | Quick Look | ![]() |
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29 | Crab Nebula | 84.5289 | 22.0469 | 83.776247 | 22.018539 | 84.930453 | -1.297747 | 184.974122 | -5.06424795 | 87.5879 | 53629.0921759259 | 2005-09-16 02:12:44 | 53629.368275463 | 2005-09-16 08:50:19 | 100022030 | 12.8244 | 10 | 12.8404 | 12.8324 | 12.8244 | 12.8484 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 10.3518 | 10.3518 | 23.824 | 1 | PROCESSED | 57527.3478009259 | 2016-05-19 08:20:50 | 54247 | 2007-05-27 00:00:00 | 54109.1621527778 | 2007-01-09 03:53:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000022 | Crab at 50arcmin off from the XIS aimpoint to study stray light. | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab at 50 arcmin off | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022030/ | Quick Look | ![]() |
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30 | Crab Nebula | 83.6282 | 22.0761 | 82.875589 | 22.04339 | 84.097378 | -1.234306 | 184.5027205 | -5.75520363 | 87.79 | 53628.5852199074 | 2005-09-15 14:02:43 | 53628.8265393518 | 2005-09-15 19:50:13 | 100023010 | 11.9978 | 10 | 11.9978 | 11.9978 | 11.9978 | 11.9978 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10.5132 | 10.5132 | 20.8239 | 0 | PROCESSED | 57527.3355902778 | 2016-05-19 08:03:15 | 54247 | 2007-05-27 00:00:00 | 54109.2268287037 | 2007-01-09 05:26:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Crab at nominal positions | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100023010/ | Quick Look | ![]() |
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31 | BD +30 3639 | 293.6887 | 30.5051 | 293.198078 | 30.394341 | 303.540216 | 51.224252 | 64.77556877 | 5.01383279 | 277.8713 | 53634.3814930556 | 2005-09-21 09:09:21 | 53635.2473842593 | 2005-09-22 05:56:14 | 100025010 | 35.2146 | 40 | 35.2306 | 35.2306 | 35.2146 | 35.2226 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.3728 | 33.3728 | 74.8039 | 1 | PROCESSED | 57527.3931597222 | 2016-05-19 09:26:09 | 54247 | 2007-05-27 00:00:00 | 54035.4664583333 | 2006-10-27 11:11:42 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Observation of planetary nebula BD +30 3639 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100025010/ | Quick Look | ![]() |
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32 | RXJ1713-3946-BKGD2 | 257.2742 | -41.0338 | 256.397744 | -40.970376 | 259.926088 | -18.035902 | 345.80577047 | -0.54060643 | 270.0033 | 53641.2980671296 | 2005-09-28 07:09:13 | 53642.1843055556 | 2005-09-29 04:25:24 | 100026030 | 37.5132 | 40 | 37.5372 | 37.5292 | 37.5132 | 37.5132 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 31.8982 | 31.8982 | 76.5659 | 0 | PROCESSED | 57527.4461574074 | 2016-05-19 10:42:28 | 54247 | 2007-05-27 00:00:00 | 54035.6187268518 | 2006-10-27 14:50:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Observation of RXJ1713.7-3946 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100026030/ | Quick Look | ![]() |
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33 | M82-Wind | 148.8893 | 69.7655 | 147.850184 | 70.002482 | 118.869306 | 52.161633 | 141.33880284 | 40.49464345 | 137.7608 | 53647.5072800926 | 2005-10-04 12:10:29 | 53648.1418287037 | 2005-10-05 03:24:14 | 100033010 | 32.3274 | 100 | 32.3274 | 32.3274 | 32.3274 | 32.3274 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.2224 | 30.2224 | 54.8021 | 0 | PROCESSED | 57527.5155092593 | 2016-05-19 12:22:20 | 54247 | 2007-05-27 00:00:00 | 54037.0057175926 | 2006-10-29 00:08:14 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033010/ | Quick Look | ![]() |
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34 | Sgr_A_west | 266.3057 | -29.1697 | 265.509983 | -29.149828 | 266.748763 | -5.770252 | 359.75546849 | -0.04768885 | 264.9601 | 53637.5953356482 | 2005-09-24 14:17:17 | 53638.7273032407 | 2005-09-25 17:27:19 | 100027020 | 42.8148 | 50 | 42.8148 | 42.8148 | 42.8148 | 42.8148 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 36.091 | 36.091 | 97.8 | 0 | PROCESSED | 57527.4293865741 | 2016-05-19 10:18:19 | 54247 | 2007-05-27 00:00:00 | 54035.5135532407 | 2006-10-27 12:19:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027020/ | Quick Look | ![]() |
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35 | E0102-72 | 16.139 | -72.1205 | 15.73725 | -72.388297 | 314.467235 | -65.111919 | 301.50933431 | -44.97149935 | 119.4064 | 53593.3086458333 | 2005-08-11 07:24:27 | 53595.2485069444 | 2005-08-13 05:57:51 | 100001010 | 2.4068 | 70 | 2.4068 | 2.4068 | 2.4068 | 2.4068 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6843287037 | 2016-05-12 16:25:26 | 54247 | 2007-05-27 00:00:00 | 54035.5925115741 | 2006-10-27 14:13:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000001 | XIS door open with a SMC SNR E0102-72 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | XIS door open | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100001010/ | Quick Look | ![]() |
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36 | 1E1743.1-2843(GC_BGD_3) | 266.592 | -28.6516 | 265.799503 | -28.633124 | 266.987582 | -5.246121 | 0.32828705 | 0.00813221 | 264.88 | 53638.7286111111 | 2005-09-25 17:29:12 | 53638.793275463 | 2005-09-25 19:02:19 | 100027050 | 1.9846 | 5 | 1.9846 | 1.9846 | 1.9846 | 1.9846 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.7934 | 1.7934 | 5.5679 | 0 | PROCESSED | 57527.4093055556 | 2016-05-19 09:49:24 | 54247 | 2007-05-27 00:00:00 | 53905.6343055556 | 2006-06-19 15:13:24 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027050/ | Quick Look | ![]() |
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37 | HESS J1616-508 | 244.1248 | -50.8971 | 243.177731 | -50.773494 | 251.629905 | -29.09136 | 332.40352084 | -0.15000913 | 282.8476 | 53632.5000231482 | 2005-09-19 12:00:02 | 53633.8183333333 | 2005-09-20 19:38:24 | 100028010 | 41.352 | 50 | 41.352 | 41.376 | 41.352 | 41.368 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.3731 | 35.3731 | 113.8899 | 0 | PROCESSED | 57527.3838194444 | 2016-05-19 09:12:42 | 54247 | 2007-05-27 00:00:00 | 54035.4361111111 | 2006-10-27 10:28:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000028 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028010/ | Quick Look | ![]() |
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38 | HESS J1616-508_BGD1 | 243.666 | -51.1742 | 242.717138 | -51.048595 | 251.369654 | -29.420684 | 332.00349288 | -0.15039556 | 283.0062 | 53631.9497222222 | 2005-09-18 22:47:36 | 53632.4990856482 | 2005-09-19 11:58:41 | 100028020 | 19.3277 | 25 | 19.3277 | 20.63 | 19.36 | 19.6323 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 16.6426 | 16.6426 | 47.4479 | 0 | PROCESSED | 57527.3573148148 | 2016-05-19 08:34:32 | 54247 | 2007-05-27 00:00:00 | 54035.1692476852 | 2006-10-27 04:03:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000028 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028020/ | Quick Look | ![]() |
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39 | GRO J1655-40 | 253.5027 | -39.8455 | 252.639975 | -39.764411 | 256.800671 | -17.156383 | 344.98315976 | 2.45489032 | 268.0237 | 53635.3140625 | 2005-09-22 07:32:15 | 53636.2968055556 | 2005-09-23 07:07:24 | 100029010 | 35.2228 | 40 | 0 | 35.2336 | 35.2228 | 35.2308 | 0 | 1 | 2 | 2 | 1 | 0 | 0 | 28.7315 | 28.7315 | 84.9019 | 1 | PROCESSED | 57527.3997337963 | 2016-05-19 09:35:37 | 54247 | 2007-05-27 00:00:00 | 54035.4940625 | 2006-10-27 11:51:27 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | GRO J1655-40 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100029010/ | Quick Look | ![]() |
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40 | NGC3516 | 166.7299 | 72.5779 | 165.877553 | 72.848305 | 123.367172 | 57.997458 | 133.2179652 | 42.40001774 | 148.9366 | 53655.5813541667 | 2005-10-12 13:57:09 | 53658.3801388889 | 2005-10-15 09:07:24 | 100031010 | 134.4696 | 150 | 134.5096 | 134.5956 | 134.5096 | 134.4696 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 122.818 | 122.818 | 241.6848 | 0 | PROCESSED | 57527.6243634259 | 2016-05-19 14:59:05 | 54247 | 2007-05-27 00:00:00 | 54036.4704976852 | 2006-10-28 11:17:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | NGC 3516 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100031010/ | Quick Look | ![]() |
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41 | M82-Wind | 148.894 | 69.7643 | 147.854963 | 70.001295 | 118.872596 | 52.161537 | 141.33883884 | 40.49666381 | 146.246 | 53662.0401273148 | 2005-10-19 00:57:47 | 53662.9390393518 | 2005-10-19 22:32:13 | 100033020 | 40.3586 | 100 | 40.3586 | 40.3826 | 40.3586 | 40.3666 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.3533 | 38.3533 | 77.658 | 0 | PROCESSED | 57527.6127546296 | 2016-05-19 14:42:22 | 54247 | 2007-05-27 00:00:00 | 54036.4196296296 | 2006-10-28 10:04:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033020/ | Quick Look | ![]() |
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42 | M82-Wind | 148.8885 | 69.7652 | 147.849381 | 70.00218 | 118.869202 | 52.16123 | 141.33933547 | 40.4945935 | 137.7608 | 53670.4681134259 | 2005-10-27 11:14:05 | 53671.1002199074 | 2005-10-28 02:24:19 | 100033030 | 28.3638 | 100 | 28.3798 | 28.3798 | 28.3718 | 28.3638 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.8121 | 25.8121 | 54.604 | 1 | PROCESSED | 57527.6784606482 | 2016-05-19 16:16:59 | 54247 | 2007-05-27 00:00:00 | 54036.8639467593 | 2006-10-28 20:44:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033030/ | Quick Look | ![]() |
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43 | Her X-1 | 254.465 | 35.3306 | 254.01442 | 35.406187 | 246.002276 | 57.482156 | 58.13562438 | 37.51514805 | 249.5714 | 53648.6450462963 | 2005-10-05 15:28:52 | 53649.4341898148 | 2005-10-06 10:25:14 | 100035010 | 36.1235 | 40 | 36.9235 | 36.1235 | 36.9235 | 36.9235 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 33.3229 | 33.3229 | 68.178 | 0 | PROCESSED | 57527.5593518518 | 2016-05-19 13:25:28 | 54247 | 2007-05-27 00:00:00 | 54036.0084375 | 2006-10-28 00:12:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000035 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD Performance Verification using Her X-1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100035010/ | Quick Look | ![]() |
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44 | Sgr_A_west | 266.3063 | -29.1685 | 265.51059 | -29.148631 | 266.749258 | -5.769039 | 359.75676556 | -0.04750971 | 264.9604 | 53642.1914467593 | 2005-09-29 04:35:41 | 53643.187025463 | 2005-09-30 04:29:19 | 100037010 | 43.7412 | 50 | 43.7412 | 43.7492 | 43.7492 | 43.7492 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.3941 | 39.3941 | 86.0139 | 0 | PROCESSED | 57527.4581828704 | 2016-05-19 10:59:47 | 54247 | 2007-05-27 00:00:00 | 54035.6663310185 | 2006-10-27 15:59:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037010/ | Quick Look | ![]() |
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45 | GRS1915+105 | 288.8014 | 10.9368 | 288.21144 | 10.848425 | 292.141211 | 32.943669 | 45.35928754 | -0.22611181 | 260.5762 | 53659.6951967593 | 2005-10-16 16:41:05 | 53661.9724305556 | 2005-10-18 23:20:18 | 100039010 | 84.7777 | 80 | 85.0631 | 86.4305 | 85.0711 | 84.7777 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 68.8623 | 68.8623 | 196.7338 | 2 | PROCESSED | 57527.9188541667 | 2016-05-19 22:03:09 | 54247 | 2007-05-27 00:00:00 | 54043.8117476852 | 2006-11-04 19:28:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Campaign of coordinated observation of GRS 1915+105 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100039010/ | Quick Look | ![]() |
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46 | RXJ1856.5-3754 | 284.1433 | -37.91 | 283.291633 | -37.976029 | 281.504649 | -15.032837 | 358.59722216 | -17.21146697 | 84.0127 | 53817.9388078704 | 2006-03-23 22:31:53 | 53819.4433217593 | 2006-03-25 10:38:23 | 100041020 | 79.169 | 80 | 79.177 | 79.169 | 79.177 | 79.177 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.2099 | 53.2099 | 129.9759 | 1 | PROCESSED | 57533.3325231482 | 2016-05-25 07:58:50 | 54247 | 2007-05-27 00:00:00 | 54042.2967824074 | 2006-11-03 07:07:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | LOW ENERGY QE CALIBRATION OF XIS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100041020/ | Quick Look | ![]() |
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47 | Crab nebula | 83.6399 | 21.8519 | 82.888543 | 21.819249 | 84.098328 | -1.458773 | 184.69891686 | -5.86604099 | 86.8683 | 53604.3898263889 | 2005-08-22 09:21:21 | 53604.4890972222 | 2005-08-22 11:44:18 | 100007030 | 2.7861 | 5 | 2.7861 | 2.7861 | 2.7901 | 2.7861 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.1927 | 2.1927 | 8.5541 | 0 | PROCESSED | 57520.7416203704 | 2016-05-12 17:47:56 | 54247 | 2007-05-27 00:00:00 | 54105.2865393518 | 2007-01-05 06:52:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Nebula | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007030/ | Quick Look | ![]() |
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48 | Crab nebula | 83.9887 | 22.0345 | 83.236236 | 22.00353 | 84.429494 | -1.290207 | 184.71743044 | -5.49499441 | 86.8666 | 53608.5155902778 | 2005-08-26 12:22:27 | 53608.7153472222 | 2005-08-26 17:10:06 | 100010100 | 9.694 | 5 | 9.694 | 9.694 | 9.694 | 9.694 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 7.5812 | 7.5812 | 17.2479 | 0 | PROCESSED | 57526.9259606482 | 2016-05-18 22:13:23 | 54247 | 2007-05-27 00:00:00 | 54122.4242939815 | 2007-01-22 10:10:59 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010100/ | Quick Look | ![]() |
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49 | Vega | 279.2264 | 38.7699 | 278.806278 | 38.72626 | 285.283614 | 61.72204 | 67.43212753 | 19.23869014 | 301.7896 | 53615.367349537 | 2005-09-02 08:48:59 | 53615.603587963 | 2005-09-02 14:29:10 | 100017010 | 11.3985 | 10 | 11.4065 | 11.4065 | 11.4065 | 11.3985 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11.5751 | 11.5751 | 20.4039 | 0 | PROCESSED | 57527.2607407407 | 2016-05-19 06:15:28 | 54247 | 2007-05-27 00:00:00 | 53906.0764814815 | 2006-06-20 01:50:08 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000017 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | XIS OBF check with Vega | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100017010/ | Quick Look | ![]() |
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50 | A0535+026 | 84.7243 | 26.3189 | 83.946776 | 26.291426 | 85.267864 | 2.964757 | 181.44092218 | -2.64422146 | 83.608 | 53627.5694907407 | 2005-09-14 13:40:04 | 53628.0418865741 | 2005-09-15 01:00:19 | 100021010 | 21.761 | 20 | 21.761 | 21.761 | 21.761 | 21.761 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.2572 | 21.2572 | 40.7839 | 1 | PROCESSED | 57527.3122337963 | 2016-05-19 07:29:37 | 54247 | 2007-05-27 00:00:00 | 54035.0644444444 | 2006-10-27 01:32:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | TOO Observation of A0535+026 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100021010/ | Quick Look | ![]() |
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51 | Crab nebula | 83.7552 | 22.0249 | 83.002845 | 21.992803 | 84.212769 | -1.290605 | 184.60948321 | -5.68314749 | 86.8656 | 53609.2022106482 | 2005-08-27 04:51:11 | 53609.3125810185 | 2005-08-27 07:30:07 | 100010140 | 3.419 | 5 | 3.419 | 3.419 | 3.419 | 3.419 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.7554 | 3.7554 | 9.5319 | 0 | PROCESSED | 57526.9383217593 | 2016-05-18 22:31:11 | 54247 | 2007-05-27 00:00:00 | 54118.9983796296 | 2007-01-18 23:57:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010140/ | Quick Look | ![]() |
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52 | Crab Nebula | 83.6309 | 22.0151 | 82.87863 | 21.982404 | 84.097185 | -1.295359 | 184.55585082 | -5.78574816 | 87.8466 | 53628.8269212963 | 2005-09-15 19:50:46 | 53629.0904976852 | 2005-09-16 02:10:19 | 100023020 | 12.5271 | 10 | 12.5311 | 12.5271 | 12.5364 | 12.5351 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 13.3529 | 13.3529 | 22.764 | 1 | PROCESSED | 57527.3409143518 | 2016-05-19 08:10:55 | 54247 | 2007-05-27 00:00:00 | 54109.193599537 | 2007-01-09 04:38:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Crab at nominal positions | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100023020/ | Quick Look | ![]() |
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53 | NGC 2110 | 88.0444 | -7.458 | 87.440268 | -7.468978 | 87.743148 | -30.884192 | 212.92660512 | -16.54877043 | 103.4188 | 53629.3796296296 | 2005-09-16 09:06:40 | 53631.8308333333 | 2005-09-18 19:56:24 | 100024010 | 101.7487 | 100 | 101.9265 | 103.7601 | 101.7487 | 102.1483 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 86.0433 | 86.0433 | 211.7558 | 4 | PROCESSED | 57527.4030324074 | 2016-05-19 09:40:22 | 54247 | 2007-05-27 00:00:00 | 54035.4624189815 | 2006-10-27 11:05:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Narrow Emission Line Galaxy NGC 2110 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100024010/ | Quick Look | ![]() |
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54 | COMA CLUSTER OFFSET | 194.6939 | 27.9466 | 194.090146 | 28.216217 | 181.281218 | 31.269541 | 60.06105128 | 88.1791818 | 318.0815 | 53885.0996412037 | 2006-05-30 02:23:29 | 53886.8384722222 | 2006-05-31 20:07:24 | 801044010 | 79.172 | 80 | 79.172 | 79.172 | 79.172 | 79.172 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.2282 | 75.2282 | 150.2049 | 2 | PROCESSED | 57534.5195949074 | 2016-05-26 12:28:13 | 54394 | 2007-10-21 00:00:00 | 53926.7587384259 | 2006-07-10 18:12:35 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801044010/ | Quick Look | ![]() |
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55 | SS 433 | 287.9527 | 4.99 | 287.334904 | 4.905608 | 290.182673 | 27.181461 | 39.69879316 | -2.23786427 | 78.6446 | 53833.4611458333 | 2006-04-08 11:04:03 | 53834.4579166667 | 2006-04-09 10:59:24 | 401004010 | 40.1976 | 40 | 40.2216 | 40.1976 | 40.2296 | 40.2136 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.4749 | 30.4749 | 86.11 | 2 | PROCESSED | 57533.4357638889 | 2016-05-25 10:27:30 | 54400 | 2007-10-27 00:00:00 | 53906.5501736111 | 2006-06-20 13:12:15 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/ | Quick Look | ![]() |
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56 | MRK 1073 | 48.7759 | 41.9723 | 47.948749 | 41.787366 | 57.835678 | 23.02641 | 149.56255257 | -13.3516285 | 258.3737 | 54135.7651851852 | 2007-02-04 18:21:52 | 54136.6641087963 | 2007-02-05 15:56:19 | 701007020 | 39.5111 | 40 | 39.5191 | 39.5111 | 0 | 39.5191 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1814 | 37.1814 | 77.6519 | 0 | PROCESSED | 57537.3263657407 | 2016-05-29 07:49:58 | 54735 | 2008-09-26 00:00:00 | 54151.4969444445 | 2007-02-20 11:55:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007020/ | Quick Look | ![]() |
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57 | 1E1207.4-5209 | 182.4916 | -52.442 | 181.83735 | -52.163724 | 209.144209 | -45.784625 | 296.53791481 | 9.91413144 | 148.6893 | 54146.2087384259 | 2007-02-15 05:00:35 | 54147.6390509259 | 2007-02-16 15:20:14 | 401030020 | 49.8266 | 50 | 50.0734 | 49.8266 | 0 | 50.0894 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 44.4468 | 44.4468 | 123.576 | 2 | PROCESSED | 57537.4372337963 | 2016-05-29 10:29:37 | 54750 | 2008-10-11 00:00:00 | 54153.9886458333 | 2007-02-22 23:43:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ATSUMASA YOSHIDA | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/ | Quick Look | ![]() |
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58 | V1223 SGR | 283.7445 | -31.105 | 282.940068 | -31.169256 | 281.851865 | -8.228404 | 5.0082738 | -14.31987205 | 79.9528 | 54203.4803240741 | 2007-04-13 11:31:40 | 54204.9418055556 | 2007-04-14 22:36:12 | 402002010 | 60.706 | 60 | 60.706 | 60.706 | 0 | 60.706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.2861 | 46.2861 | 126.2719 | 2 | PROCESSED | 57538.1822800926 | 2016-05-30 04:22:29 | 54744 | 2008-10-05 00:00:00 | 54210.6596875 | 2007-04-20 15:49:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MANABU ISHIDA | JAP | 2 | AO2 | MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402002010/ | Quick Look | ![]() |
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59 | PSR B1259-63 | 195.6556 | -63.8839 | 194.86632 | -63.61523 | 227.712317 | -50.941906 | 304.16255435 | -1.03887935 | 293.4832 | 54304.2811226852 | 2007-07-23 06:44:49 | 54304.6877777778 | 2007-07-23 16:30:24 | 402014050 | 19.7023 | 20 | 19.7023 | 19.7023 | 0 | 19.7023 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.7549 | 17.7549 | 35.1279 | 0 | PROCESSED | 57539.3024768518 | 2016-05-31 07:15:34 | 54707 | 2008-08-29 00:00:00 | 54339.2175347222 | 2007-08-27 05:13:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014050/ | Quick Look | ![]() |
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60 | LS 5039 | 276.5633 | -14.9109 | 275.848755 | -14.941003 | 276.400444 | 8.383997 | 16.82651822 | -1.31880921 | 270.412 | 54352.6780555556 | 2007-09-09 16:16:24 | 54358.4725 | 2007-09-15 11:20:24 | 402015010 | 203.2399 | 200 | 203.2399 | 203.2399 | 0 | 203.2399 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 181.095 | 181.095 | 442.0879 | 4 | PROCESSED | 57540.0947685185 | 2016-06-01 02:16:28 | 54745 | 2008-10-06 00:00:00 | 54384.7259027778 | 2007-10-11 17:25:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 2 | AO2 | SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402015010/ | Quick Look | ![]() |
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61 | SN1006 SW-Rim | 225.5051 | -42.0698 | 224.686984 | -41.873221 | 235.327536 | -23.832864 | 327.36692545 | 14.52303039 | 297.2712 | 53623.5862962963 | 2005-09-10 14:04:16 | 53624.993287037 | 2005-09-11 23:50:20 | 100019030 | 28.5245 | 50 | 28.5325 | 28.5245 | 28.5409 | 28.5405 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27.0082 | 27.0082 | 121.5519 | 5 | PROCESSED | 57527.3126967593 | 2016-05-19 07:30:17 | 54247 | 2007-05-27 00:00:00 | 54034.9697453704 | 2006-10-26 23:16:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | SN1006 observation with XIS and HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019030/ | Quick Look | ![]() |
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62 | 4U 1700+24 | 256.6316 | 23.9071 | 256.110961 | 23.972677 | 252.098688 | 46.519124 | 45.07419011 | 32.98144858 | 280.149 | 54334.7787615741 | 2007-08-22 18:41:25 | 54335.875162037 | 2007-08-23 21:00:14 | 402023010 | 50.2445 | 50 | 50.2525 | 50.2605 | 0 | 50.2445 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.3268 | 45.3268 | 94.7158 | 2 | PROCESSED | 57539.6636226852 | 2016-05-31 15:55:37 | 54723 | 2008-09-14 00:00:00 | 54350.4606481482 | 2007-09-07 11:03:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | OSAMU NAGAE | JAP | 2 | AO2 | STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402023010/ | Quick Look | ![]() |
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63 | CYG OB2 ASSOCIATION | 308.2175 | 41.2935 | 307.768848 | 41.122144 | 329.008943 | 57.17316 | 80.16491027 | 0.83267098 | 220.3949 | 54452.9185532407 | 2007-12-18 22:02:43 | 54453.843912037 | 2007-12-19 20:15:14 | 402030010 | 41.1147 | 40 | 41.1147 | 41.1147 | 0 | 41.1147 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.9181 | 37.9181 | 79.9439 | 0 | PROCESSED | 57540.9006597222 | 2016-06-01 21:36:57 | 54828 | 2008-12-28 00:00:00 | 54460.6521643518 | 2007-12-26 15:39:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHUNJI KITAMOTO | JAP | 2 | AO2 | STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402030010/ | Quick Look | ![]() |
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64 | EMS0071 | 16.6433 | 48.9425 | 15.913472 | 48.675321 | 36.903288 | 38.099489 | 125.49064727 | -13.85403968 | 69.9406 | 55392.4123148148 | 2010-07-15 09:53:44 | 55392.8855092593 | 2010-07-15 21:15:08 | 705010010 | 23.0102 | 20 | 23.0102 | 23.0102 | 0 | 23.0102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.568 | 19.568 | 40.8819 | 0 | PROCESSED | 57552.6419560185 | 2016-06-13 15:24:25 | 55779 | 2011-08-06 00:00:00 | 55411.2637384259 | 2010-08-03 06:19:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705010010/ | Quick Look | ![]() |
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65 | BD +30 3639 | 293.6993 | 30.5065 | 293.208675 | 30.395694 | 303.554886 | 51.223276 | 64.78119899 | 5.00649051 | 237.7342 | 53676.9934837963 | 2005-11-02 23:50:37 | 53677.8230324074 | 2005-11-03 19:45:10 | 100025020 | 31.1384 | 40 | 31.1384 | 31.1624 | 31.1464 | 31.1544 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27.1258 | 27.1258 | 71.638 | 1 | PROCESSED | 57527.9315509259 | 2016-05-19 22:21:26 | 54247 | 2007-05-27 00:00:00 | 54037.1080902778 | 2006-10-29 02:35:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Observation of planetary nebula BD +30 3639 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100025020/ | Quick Look | ![]() |
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66 | KS1741-293(GC_BGD_2) | 266.2069 | -29.3515 | 265.410046 | -29.331146 | 266.666918 | -5.954235 | 359.55541243 | -0.06909433 | 265.0174 | 53637.5288541667 | 2005-09-24 12:41:33 | 53637.5946296296 | 2005-09-24 14:16:16 | 100027040 | 1.937 | 5 | 1.937 | 1.937 | 1.937 | 1.937 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.7637 | 1.7637 | 5.68 | 0 | PROCESSED | 57527.404525463 | 2016-05-19 09:42:31 | 54247 | 2007-05-27 00:00:00 | 53907.393275463 | 2006-06-21 09:26:19 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027040/ | Quick Look | ![]() |
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67 | HESS J1616-508_BGD2 | 244.4656 | -50.6883 | 243.5199 | -50.566183 | 251.824242 | -28.844194 | 332.70353325 | -0.14997577 | 283.1793 | 53633.8196412037 | 2005-09-20 19:40:17 | 53634.3120833333 | 2005-09-21 07:29:24 | 100028030 | 21.8735 | 25 | 21.8895 | 21.8895 | 21.8815 | 21.8735 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18.2063 | 18.2063 | 42.5359 | 0 | PROCESSED | 57527.3722800926 | 2016-05-19 08:56:05 | 54247 | 2007-05-27 00:00:00 | 54035.4698842593 | 2006-10-27 11:16:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000028 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028030/ | Quick Look | ![]() |
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68 | GC_SOUTH_1 | 268.0988 | -29.4771 | 267.30082 | -29.465922 | 268.32614 | -6.047082 | 0.29758282 | -1.54591478 | 274.6002 | 56190.0385069444 | 2012-09-20 00:55:27 | 56191.3341435185 | 2012-09-21 08:01:10 | 507028010 | 51.7619 | 50 | 51.7619 | 51.7699 | 0 | 51.7699 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 41.1534 | 41.1534 | 111.9318 | 1 | PROCESSED | 57607.1304398148 | 2016-08-07 03:07:50 | 56584 | 2013-10-19 00:00:00 | 56218.5464930556 | 2012-10-18 13:06:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507028010/ | Quick Look | ![]() |
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69 | ULXs in NGC 1313 | 49.5245 | -66.5352 | 49.373425 | -66.716272 | 341.380796 | -74.178462 | 283.41323765 | -44.63106544 | 172.6337 | 53658.556400463 | 2005-10-15 13:21:13 | 53659.6252777778 | 2005-10-16 15:00:24 | 100032010 | 32.878 | 40 | 32.878 | 32.878 | 32.878 | 32.878 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 30.38 | 30.38 | 92.3439 | 1 | PROCESSED | 57527.587349537 | 2016-05-19 14:05:47 | 54247 | 2007-05-27 00:00:00 | 54036.1929398148 | 2006-10-28 04:37:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | ULXs in NGC 1313 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100032010/ | Quick Look | ![]() |
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70 | JUPITER | 104.4639 | 23.0622 | 103.708176 | 23.129949 | 103.287865 | 0.285992 | 192.81439153 | 11.62759441 | 264.6138 | 56767.1149421296 | 2014-04-20 02:45:31 | 56767.448125 | 2014-04-20 10:45:18 | 508023110 | 16.7417 | 160 | 16.7417 | 16.7737 | 0 | 16.7657 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9630671296 | 2016-08-14 23:06:49 | 57212 | 2015-07-09 00:00:00 | 56789.801712963 | 2014-05-12 19:14:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023110/ | Quick Look | ![]() |
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71 | CYGNUS LOOP BLOWOUT3 | 312.3799 | 29.0257 | 311.853293 | 28.839005 | 325.853846 | 44.599011 | 72.47923846 | -9.33489782 | 78.1517 | 55688.6493981482 | 2011-05-07 15:35:08 | 55689.9654976852 | 2011-05-08 23:10:19 | 506013010 | 60.2669 | 60 | 60.2669 | 60.2749 | 0 | 60.2669 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.9803 | 55.9803 | 113.6288 | 1 | PROCESSED | 57601.9873611111 | 2016-08-01 23:41:48 | 56066 | 2012-05-19 00:00:00 | 55700.4602083333 | 2011-05-19 11:02:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506013010/ | Quick Look | ![]() |
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72 | HYDRA A-2 | 139.672 | -11.9467 | 139.069416 | -11.735403 | 146.240414 | -26.215979 | 242.89463155 | 25.29884455 | 94.9986 | 55509.1804861111 | 2010-11-09 04:19:54 | 55510.3008680556 | 2010-11-10 07:13:15 | 805008010 | 41.8231 | 40 | 41.8311 | 41.8231 | 0 | 41.8311 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.5896 | 34.5896 | 96.7898 | 2 | PROCESSED | 57554.050162037 | 2016-06-15 01:12:14 | 55890 | 2011-11-25 00:00:00 | 55524.1344791667 | 2010-11-24 03:13:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050012 | X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 5 | AO5 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805008010/ | Quick Look | ![]() |
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73 | A 3376 | 90.5561 | -39.9584 | 90.148808 | -39.956705 | 90.960808 | -63.398292 | 246.50686261 | -25.98989573 | 107.6124 | 53649.6153703704 | 2005-10-06 14:46:08 | 53653.4495833333 | 2005-10-10 10:47:24 | 100034010 | 118.7792 | 150 | 118.7792 | 121.7373 | 118.8498 | 119.3357 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 100.5401 | 100.5401 | 331.2537 | 3 | PROCESSED | 57527.6218171296 | 2016-05-19 14:55:25 | 54247 | 2007-05-27 00:00:00 | 54109.6396990741 | 2007-01-09 15:21:10 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Diffuse Hard X-rays from Clusters | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100034010/ | Quick Look | ![]() |
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74 | 1E1743.1-2843 GCBGD3 | 266.5944 | -28.6526 | 265.801896 | -28.634135 | 266.98972 | -5.247071 | 0.32852719 | 0.00581314 | 264.8798 | 53644.2657523148 | 2005-10-01 06:22:41 | 53644.3162268518 | 2005-10-01 07:35:22 | 100037050 | 2.4 | 5 | 2.4 | 2.4 | 2.4 | 2.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.2329 | 2.2329 | 4.3539 | 0 | PROCESSED | 57527.4530902778 | 2016-05-19 10:52:27 | 54247 | 2007-05-27 00:00:00 | 54056.1970833333 | 2006-11-17 04:43:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037050/ | Quick Look | ![]() |
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75 | 1E 1048.1-5937 | 162.5452 | -59.8394 | 162.049535 | -59.57411 | 203.219635 | -58.558248 | 288.24102095 | -0.47209541 | 101.4368 | 54800.9597337963 | 2008-11-30 23:02:01 | 54802.5927083333 | 2008-12-02 14:13:30 | 403005010 | 100.4231 | 100 | 100.443 | 100.4231 | 0 | 100.4231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.1049 | 68.1049 | 141.0819 | 0 | PROCESSED | 57544.6078472222 | 2016-06-05 14:35:18 | 55178 | 2009-12-13 00:00:00 | 54812.0471875 | 2008-12-12 01:07:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUMPEI TAKATA | JAP | 3 | AO3 | X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403005010/ | Quick Look | ![]() |
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76 | MARS-P3 | 102.9612 | 25.1565 | 102.192848 | 25.217116 | 101.724463 | 2.241555 | 190.28784034 | 11.26022306 | 298.032 | 54559.4933796296 | 2008-04-03 11:50:28 | 54559.5766087963 | 2008-04-03 13:50:19 | 403006030 | 3.886 | 100 | 3.886 | 3.91 | 0 | 3.894 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.1134 | 3.1134 | 7.1839 | 0 | PROCESSED | 57542.0373148148 | 2016-06-03 00:53:44 | 54953 | 2009-05-02 00:00:00 | 54577.0484259259 | 2008-04-21 01:09:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006030/ | Quick Look | ![]() |
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77 | MARS-P11 | 103.2936 | 25.1207 | 102.525618 | 25.182892 | 102.027614 | 2.233108 | 190.44969799 | 11.5184009 | 298.1493 | 54560.1601041667 | 2008-04-04 03:50:33 | 54560.2433333333 | 2008-04-04 05:50:24 | 403006110 | 4.6198 | 100 | 4.6278 | 4.6198 | 0 | 4.6358 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.0749 | 4.0749 | 7.1839 | 0 | PROCESSED | 57542.0559490741 | 2016-06-03 01:20:34 | 54953 | 2009-05-02 00:00:00 | 54577.1745023148 | 2008-04-21 04:11:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006110/ | Quick Look | ![]() |
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78 | MARS-P13 | 103.3779 | 25.1101 | 102.610021 | 25.172691 | 102.104653 | 2.229561 | 190.49210676 | 11.58330245 | 298.1799 | 54560.3267708333 | 2008-04-04 07:50:33 | 54560.41 | 2008-04-04 09:50:24 | 403006130 | 4.2518 | 100 | 4.2678 | 4.2518 | 0 | 4.2678 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.529 | 3.529 | 7.1839 | 0 | PROCESSED | 57542.0605671296 | 2016-06-03 01:27:13 | 54953 | 2009-05-02 00:00:00 | 54577.9292939815 | 2008-04-21 22:18:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006130/ | Quick Look | ![]() |
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79 | MARS-P16 | 103.503 | 25.0968 | 102.735261 | 25.159983 | 102.218767 | 2.2268 | 190.55275085 | 11.68067717 | 298.2223 | 54560.5768171296 | 2008-04-04 13:50:37 | 54560.66 | 2008-04-04 15:50:24 | 403006160 | 2.3262 | 100 | 2.3262 | 2.3262 | 0 | 2.3262 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2.134 | 2.134 | 7.1799 | 0 | PROCESSED | 57542.0664236111 | 2016-06-03 01:35:39 | 54953 | 2009-05-02 00:00:00 | 54577.9478935185 | 2008-04-21 22:44:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006160/ | Quick Look | ![]() |
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80 | MARS-P21 | 103.7101 | 25.0688 | 102.942627 | 25.132964 | 102.408276 | 2.21649 | 190.65860601 | 11.8395058 | 298.2947 | 54560.9933217593 | 2008-04-04 23:50:23 | 54561.0765509259 | 2008-04-05 01:50:14 | 403006210 | 2.8808 | 100 | 2.8808 | 2.8808 | 0 | 2.8808 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.4516 | 3.4516 | 7.1839 | 0 | PROCESSED | 57542.0774884259 | 2016-06-03 01:51:35 | 54953 | 2009-05-02 00:00:00 | 54578.0612847222 | 2008-04-22 01:28:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006210/ | Quick Look | ![]() |
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81 | MARS-P23 | 103.7955 | 25.0599 | 103.028122 | 25.124467 | 102.486187 | 2.214951 | 190.69976585 | 11.90614711 | 298.325 | 54561.1600347222 | 2008-04-05 03:50:27 | 54561.2432175926 | 2008-04-05 05:50:14 | 403006230 | 4.5188 | 100 | 4.5268 | 4.5188 | 0 | 4.5348 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.6868 | 3.6868 | 7.1839 | 0 | PROCESSED | 57542.0791898148 | 2016-06-03 01:54:02 | 54953 | 2009-05-02 00:00:00 | 54578.1176157407 | 2008-04-22 02:49:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006230/ | Quick Look | ![]() |
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82 | MARS-P25 | 103.8803 | 25.0503 | 103.113021 | 25.115268 | 102.56363 | 2.212708 | 190.74132534 | 11.97202775 | 298.3546 | 54561.3266550926 | 2008-04-05 07:50:23 | 54561.4098842593 | 2008-04-05 09:50:14 | 403006250 | 4.2612 | 100 | 4.2692 | 4.2612 | 0 | 4.2692 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.2511 | 3.2511 | 7.1839 | 0 | PROCESSED | 57542.2336458333 | 2016-06-03 05:36:27 | 54953 | 2009-05-02 00:00:00 | 54578.1323032407 | 2008-04-22 03:10:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006250/ | Quick Look | ![]() |
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83 | MARS-P26 | 103.921 | 25.0474 | 103.153759 | 25.112561 | 102.600638 | 2.213348 | 190.75967691 | 12.00436516 | 298.3671 | 54561.4100347222 | 2008-04-05 09:50:27 | 54561.4932175926 | 2008-04-05 11:50:14 | 403006260 | 4.7976 | 100 | 4.8136 | 4.7976 | 0 | 4.8216 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.7622 | 3.7622 | 7.1839 | 0 | PROCESSED | 57542.2337962963 | 2016-06-03 05:36:40 | 54953 | 2009-05-02 00:00:00 | 54578.1374074074 | 2008-04-22 03:17:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006260/ | Quick Look | ![]() |
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84 | COMA SUBHALO2 | 194.5069 | 27.3689 | 193.901795 | 27.638743 | 181.411119 | 30.679028 | 42.63932899 | 88.51577103 | 315.0001 | 56452.5504976852 | 2013-06-09 13:12:43 | 56453.0265046296 | 2013-06-10 00:38:10 | 808020010 | 21.1563 | 20 | 21.1563 | 21.1563 | 0 | 21.1563 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.608 | 17.608 | 41.1199 | 1 | PROCESSED | 57611.5058564815 | 2016-08-11 12:08:26 | 56872 | 2014-08-03 00:00:00 | 56506.7547222222 | 2013-08-02 18:06:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808020010/ | Quick Look | ![]() |
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85 | A3376 NORTH | 90.6541 | -39.7108 | 90.244762 | -39.708634 | 91.122885 | -63.149983 | 246.26196714 | -25.85404299 | 80.8001 | 56553.3109143518 | 2013-09-18 07:27:43 | 56554.8453935185 | 2013-09-19 20:17:22 | 808029010 | 57.6912 | 57 | 57.6912 | 57.6992 | 0 | 57.7072 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.8185 | 50.8185 | 132.57 | 0 | PROCESSED | 57612.703275463 | 2016-08-12 16:52:43 | 56956 | 2014-10-26 00:00:00 | 56588.7436689815 | 2013-10-23 17:50:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808029010/ | Quick Look | ![]() |
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86 | NORTH POLAR SPUR | 260.5905 | 4.7489 | 259.972652 | 4.795886 | 259.371969 | 27.842624 | 26.83412197 | 21.95376599 | 264.1143 | 53646.4785763889 | 2005-10-03 11:29:09 | 53647.4515277778 | 2005-10-04 10:50:12 | 100038010 | 43.0689 | 50 | 43.1489 | 44.2129 | 43.0689 | 43.2929 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40.7715 | 40.7715 | 84.0019 | 0 | PROCESSED | 57527.5342824074 | 2016-05-19 12:49:22 | 54247 | 2007-05-27 00:00:00 | 54035.8928009259 | 2006-10-27 21:25:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | North Polar Spur | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100038010/ | Quick Look | ![]() |
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87 | ARCHES CLUSTER | 266.4808 | -28.778 | 265.687528 | -28.758983 | 266.892731 | -5.374834 | 0.16960578 | 0.02569084 | 109.9998 | 54911.0857407407 | 2009-03-21 02:03:28 | 54913.7681712963 | 2009-03-23 18:26:10 | 403009010 | 110.7933 | 100 | 110.7933 | 110.7933 | 0 | 110.7933 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.6578 | 91.6578 | 231.7417 | 3 | PROCESSED | 57545.9555787037 | 2016-06-06 22:56:02 | 55330 | 2010-05-14 00:00:00 | 54924.3822106482 | 2009-04-03 09:10:23 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAHIRO TSUJIMOTO | JAP | 3 | AO3 | A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403009010/ | Quick Look | ![]() |
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88 | LS I+61 303_1 | 40.1455 | 61.188 | 39.183267 | 60.973753 | 59.828193 | 42.868734 | 135.69810374 | 1.0510579 | 270.0003 | 54853.9515856482 | 2009-01-22 22:50:17 | 54854.8648032407 | 2009-01-23 20:45:19 | 403015010 | 40.5514 | 40 | 40.5514 | 40.5514 | 0 | 40.5514 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7312 | 25.7312 | 78.868 | 0 | PROCESSED | 57545.3022916667 | 2016-06-06 07:15:18 | 55329 | 2010-05-13 00:00:00 | 54880.5343865741 | 2009-02-18 12:49:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403015010/ | Quick Look | ![]() |
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89 | LS I+61 303_2 | 40.1457 | 61.1877 | 39.18347 | 60.973453 | 59.828143 | 42.868421 | 135.69831419 | 1.05082335 | 270.0006 | 54856.6966087963 | 2009-01-25 16:43:07 | 54858.1766666667 | 2009-01-27 04:14:24 | 403016010 | 61.0667 | 60 | 61.0784 | 61.0667 | 0 | 61.0784 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.6591 | 26.6591 | 127.8398 | 1 | PROCESSED | 57545.3828819444 | 2016-06-06 09:11:21 | 55329 | 2010-05-13 00:00:00 | 54880.5522106482 | 2009-02-18 13:15:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403016010/ | Quick Look | ![]() |
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90 | LS I+61 303_3 | 40.2018 | 61.1949 | 39.239095 | 60.980826 | 59.865781 | 42.86376 | 135.72005286 | 1.06843757 | 246.2753 | 54872.1842592593 | 2009-02-10 04:25:20 | 54873.7252199074 | 2009-02-11 17:24:19 | 403017010 | 68.6273 | 60 | 68.6273 | 68.6273 | 0 | 68.6273 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.0685 | 65.0685 | 133.1218 | 1 | PROCESSED | 57545.5290856482 | 2016-06-06 12:41:53 | 55330 | 2010-05-14 00:00:00 | 54893.4210300926 | 2009-03-03 10:06:17 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403017010/ | Quick Look | ![]() |
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91 | A1689-OFFSET3 | 197.7048 | -1.4241 | 197.062246 | -1.158416 | 196.866357 | 5.631394 | 312.98436439 | 61.06880263 | 289.9992 | 54672.423599537 | 2008-07-25 10:09:59 | 54673.474525463 | 2008-07-26 11:23:19 | 803026010 | 44.0942 | 40 | 44.0942 | 44.0942 | 0 | 44.0942 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7063 | 37.7063 | 90.7878 | 1 | PROCESSED | 57543.149537037 | 2016-06-04 03:35:20 | 55076 | 2009-09-02 00:00:00 | 54707.1173263889 | 2008-08-29 02:48:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803026010/ | Quick Look | ![]() |
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92 | IGR J16194-2810 | 244.8908 | -28.0663 | 244.116394 | -27.946439 | 247.849887 | -6.534784 | 349.1669856 | 15.58223604 | 95.1879 | 54867.1762152778 | 2009-02-05 04:13:45 | 54868.4314236111 | 2009-02-06 10:21:15 | 403024010 | 45.5687 | 50 | 45.5687 | 45.5738 | 0 | 45.5687 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.7859 | 38.7859 | 108.4358 | 1 | PROCESSED | 57545.4895023148 | 2016-06-06 11:44:53 | 55329 | 2010-05-13 00:00:00 | 54880.5743518518 | 2009-02-18 13:47:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | OSAMU NAGAE | JAP | 3 | AO3 | ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403024010/ | Quick Look | ![]() |
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93 | V709 CAS | 7.1951 | 59.3013 | 6.498819 | 59.024957 | 38.349683 | 49.774418 | 120.03837674 | -3.44309479 | 84.0816 | 54637.4334837963 | 2008-06-20 10:24:13 | 54638.1542824074 | 2008-06-21 03:42:10 | 403025010 | 35.8982 | 30 | 35.8982 | 35.8982 | 0 | 35.8982 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.3823 | 33.3823 | 62.2679 | 0 | PROCESSED | 57542.8811921296 | 2016-06-03 21:08:55 | 55014 | 2009-07-02 00:00:00 | 54648.3358101852 | 2008-07-01 08:03:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403025010/ | Quick Look | ![]() |
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94 | RX J1940.1-1025 | 295.0445 | -10.4193 | 294.356962 | -10.535652 | 295.074294 | 10.867465 | 28.98688715 | -15.49869645 | 79.7405 | 54572.8979976852 | 2008-04-16 21:33:07 | 54573.743275463 | 2008-04-17 17:50:19 | 403027010 | 32.4536 | 30 | 32.4536 | 32.4536 | 0 | 32.4536 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.4657 | 26.4657 | 73.0219 | 2 | PROCESSED | 57542.3241087963 | 2016-06-03 07:46:43 | 54953 | 2009-05-02 00:00:00 | 54587.0481481482 | 2008-05-01 01:09:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403027010/ | Quick Look | ![]() |
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95 | Crab Nebula | 83.6372 | 22.097 | 82.884469 | 22.064333 | 84.106634 | -1.213794 | 184.48946706 | -5.73697 | 84.9994 | 53613.8323032407 | 2005-08-31 19:58:31 | 53613.975787037 | 2005-08-31 23:25:08 | 100015010 | 5.6587 | 5 | 5.6587 | 5.6587 | 5.6587 | 5.6587 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5.7907 | 5.7907 | 12.3879 | 0 | PROCESSED | 57527.2296412037 | 2016-05-19 05:30:41 | 54247 | 2007-05-27 00:00:00 | 54109.1053240741 | 2007-01-09 02:31:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD boresight check with Crab | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015010/ | Quick Look | ![]() |
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96 | GS 1826-238 | 277.3735 | -23.8572 | 276.610421 | -23.891095 | 276.73109 | -0.588705 | 9.22092987 | -6.12003001 | 267.2862 | 55125.8488310185 | 2009-10-21 20:22:19 | 55127.9502777778 | 2009-10-23 22:48:24 | 404007010 | 102.5154 | 100 | 102.5154 | 102.5314 | 0 | 102.5372 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.9996 | 87.9996 | 181.5418 | 2 | PROCESSED | 57549.0104976852 | 2016-06-10 00:15:07 | 55534 | 2010-12-04 00:00:00 | 55166.4220833333 | 2009-12-01 10:07:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUTAKA YAMAOKA | JAP | 4 | AO4 | SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404007010/ | Quick Look | ![]() |
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97 | EUVE J0317-85.5 | 48.9864 | -85.5003 | 51.11405 | -85.679196 | 278.533864 | -69.749958 | 299.84736337 | -30.72881529 | 65.46 | 55028.6017476852 | 2009-07-16 14:26:31 | 55030.1460185185 | 2009-07-18 03:30:16 | 404019010 | 63.0843 | 60 | 63.0843 | 63.0843 | 0 | 63.0843 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.8965 | 56.8965 | 133.4138 | 1 | PROCESSED | 57547.8712847222 | 2016-06-08 20:54:39 | 55406 | 2010-07-29 00:00:00 | 55040.2674305556 | 2009-07-28 06:25:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ATSUSHI HARAYAMA | JAP | 4 | AO4 | FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404019010/ | Quick Look | ![]() |
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98 | TT ARI | 31.7181 | 15.2972 | 31.038138 | 15.059527 | 34.795947 | 2.311089 | 148.52228749 | -43.79443 | 71.0668 | 55018.4424652778 | 2009-07-06 10:37:09 | 55019.3023611111 | 2009-07-07 07:15:24 | 404021010 | 35.7421 | 35 | 35.7421 | 35.7796 | 0 | 35.7876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.794 | 31.794 | 74.2578 | 1 | PROCESSED | 57547.7822453704 | 2016-06-08 18:46:26 | 55399 | 2010-07-22 00:00:00 | 55029.236712963 | 2009-07-17 05:40:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404021010/ | Quick Look | ![]() |
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99 | TX COL | 85.7822 | -41.0648 | 85.383592 | -41.086265 | 82.635964 | -64.399356 | 246.79781267 | -29.77494364 | 322.4827 | 54963.6800578704 | 2009-05-12 16:19:17 | 54965.2502199074 | 2009-05-14 06:00:19 | 404031010 | 59.7818 | 40 | 59.7898 | 59.7898 | 0 | 59.7818 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.123 | 51.123 | 135.654 | 0 | PROCESSED | 57546.5734143518 | 2016-06-07 13:45:43 | 55345 | 2010-05-29 00:00:00 | 54978.2105439815 | 2009-05-27 05:03:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404031010/ | Quick Look | ![]() |
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100 | Crab nebula | 83.6105 | 22.3483 | 82.856361 | 22.315501 | 84.093042 | -0.96164 | 184.26290563 | -5.62323625 | 86.8596 | 53607.2790509259 | 2005-08-25 06:41:50 | 53607.5139583333 | 2005-08-25 12:20:06 | 100010030 | 8.1129 | 5 | 8.1129 | 8.1129 | 8.1129 | 8.1129 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7.8359 | 7.8359 | 20.264 | 1 | PROCESSED | 57526.8876388889 | 2016-05-18 21:18:12 | 54247 | 2007-05-27 00:00:00 | 54118.9698958333 | 2007-01-18 23:16:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010030/ | Quick Look | ![]() |
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101 | DA 240 EAST LOBE | 117.3573 | 55.877 | 116.349381 | 56.002734 | 108.151975 | 34.146502 | 161.8466677 | 30.16323196 | 293.7777 | 55274.9306134259 | 2010-03-19 22:20:05 | 55276.7238657407 | 2010-03-21 17:22:22 | 704020010 | 81.7834 | 80 | 81.7834 | 81.7914 | 0 | 81.7914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.3033 | 74.3033 | 154.9218 | 1 | PROCESSED | 57550.9753587963 | 2016-06-11 23:24:31 | 55654 | 2011-04-03 00:00:00 | 55286.3268518518 | 2010-03-31 07:50:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 4 | AO4 | SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704020010/ | Quick Look | ![]() |
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102 | N132D | 81.2794 | -69.6524 | 81.381964 | -69.694399 | 312.375338 | -85.522525 | 280.31514531 | -32.77566051 | 53.3291 | 53595.4703125 | 2005-08-13 11:17:15 | 53597.5313541667 | 2005-08-15 12:45:09 | 100002010 | 7.4066 | 80 | 7.4066 | 7.4066 | 7.4066 | 7.4066 | 2 | 2 | 2 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.7109606482 | 2016-05-12 17:03:47 | 54247 | 2007-05-27 00:00:00 | 54038.5875925926 | 2006-10-30 14:06:08 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD HV ON WITH N132D | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002010/ | Quick Look | ![]() |
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103 | NGC 5044 OFFSET1 | 198.8505 | -16.143 | 198.184446 | -15.87899 | 203.499232 | -7.562902 | 311.28196707 | 46.33985641 | 290.0004 | 53919.3604398148 | 2006-07-03 08:39:02 | 53920.9599305556 | 2006-07-04 23:02:18 | 801047010 | 54.6204 | 60 | 54.6204 | 54.6204 | 54.6204 | 54.6204 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.8033 | 45.8033 | 138.1899 | 1 | PROCESSED | 57534.8941203704 | 2016-05-26 21:27:32 | 54394 | 2007-10-21 00:00:00 | 53942.4615740741 | 2006-07-26 11:04:40 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801047010/ | Quick Look | ![]() |
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104 | V773TAU | 63.5571 | 28.1952 | 62.783682 | 28.069565 | 66.716115 | 6.867305 | 168.22500409 | -16.34364304 | 260.6557 | 55610.1581712963 | 2011-02-18 03:47:46 | 55611.9815277778 | 2011-02-19 23:33:24 | 405011010 | 82.2463 | 80 | 82.2543 | 82.2463 | 0 | 82.2543 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.8287 | 72.8287 | 157.5258 | 2 | PROCESSED | 57601.0256134259 | 2016-08-01 00:36:53 | 55990 | 2012-03-04 00:00:00 | 55621.2978703704 | 2011-03-01 07:08:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOHKO TSUBOI | JAP | 5 | AO5 | NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405011010/ | Quick Look | ![]() |
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105 | 1E 1547.0-5408 | 237.7284 | -54.3676 | 236.761869 | -54.21692 | 248.127922 | -33.347549 | 327.20000551 | -0.18012949 | 271.1663 | 55415.1611921296 | 2010-08-07 03:52:07 | 55415.9633796296 | 2010-08-07 23:07:16 | 405024010 | 51.6728 | 50 | 51.6728 | 51.7928 | 0 | 52.1529 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 42.7812 | 42.7812 | 69.2999 | 0 | PROCESSED | 57552.8870949074 | 2016-06-13 21:17:25 | 55793 | 2011-08-20 00:00:00 | 55427.247025463 | 2010-08-19 05:55:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI NISHIOKA | 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 | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405024010/ | Quick Look | ![]() |
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106 | EMS1150 | 263.083 | -32.7212 | 262.264926 | -32.685689 | 264.095488 | -9.421504 | 355.27740066 | 0.39306698 | 91.2452 | 55611.9964930556 | 2011-02-19 23:54:57 | 55612.6968055556 | 2011-02-20 16:43:24 | 405026010 | 20.9186 | 20 | 20.9186 | 20.9186 | 0 | 20.9186 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.2639 | 17.2639 | 60.5039 | 0 | PROCESSED | 57600.9777893518 | 2016-07-31 23:28:01 | 55988 | 2012-03-02 00:00:00 | 55621.1440740741 | 2011-03-01 03:27:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405026010/ | Quick Look | ![]() |
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107 | ABELL1835 OFFSET2 | 210.2863 | 2.6798 | 209.652404 | 2.920968 | 207.209815 | 14.079845 | 340.21334307 | 60.40388756 | 306.816 | 55384.1224884259 | 2010-07-07 02:56:23 | 55385.4667939815 | 2010-07-08 11:12:11 | 805038010 | 45.6036 | 50 | 45.6036 | 45.6276 | 0 | 45.6116 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2826 | 41.2826 | 116.1298 | 0 | PROCESSED | 57552.5623611111 | 2016-06-13 13:29:48 | 55801 | 2011-08-28 00:00:00 | 55434.3364930556 | 2010-08-26 08:04:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NOBUHIRO OKABE | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805038010/ | Quick Look | ![]() |
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108 | 4U1812-12 | 273.8053 | -12.0935 | 273.104949 | -12.110284 | 273.784611 | 11.297146 | 18.04900466 | 2.37362039 | 267.159 | 55838.1400347222 | 2011-10-04 03:21:39 | 55839.9168981482 | 2011-10-05 22:00:20 | 406008010 | 62.0143 | 60 | 62.0143 | 62.0143 | 0 | 62.0143 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.5441 | 53.5441 | 153.5099 | 1 | PROCESSED | 57603.3255902778 | 2016-08-03 07:48:51 | 56226 | 2012-10-26 00:00:00 | 55858.3124768518 | 2011-10-24 07:29:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SOKI SAKURAI | JAP | 6 | AO6 | REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406008010/ | Quick Look | ![]() |
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109 | VW HYI | 62.3084 | -71.2978 | 62.399199 | -71.427045 | 322.000013 | -79.107776 | 284.88912946 | -38.12913625 | 338.7313 | 56049.8124305556 | 2012-05-02 19:29:54 | 56050.1668171296 | 2012-05-03 04:00:13 | 406009040 | 16.8177 | 20 | 16.8257 | 16.8257 | 0 | 16.8177 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13.9478 | 13.9478 | 30.6159 | 0 | PROCESSED | 57605.3312847222 | 2016-08-05 07:57:03 | 56449 | 2013-06-06 00:00:00 | 56083.0857060185 | 2012-06-05 02:03:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009040/ | Quick Look | ![]() |
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110 | CYG X-1 | 299.5916 | 35.1745 | 299.121401 | 35.038023 | 313.64901 | 54.223609 | 71.31236822 | 3.05181611 | 279.5001 | 55839.9245023148 | 2011-10-05 22:11:17 | 55840.9169328704 | 2011-10-06 22:00:23 | 406013010 | 3.7027 | 40 | 3.832 | 3.7027 | 0 | 40.2718 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32.9625 | 32.9625 | 85.7339 | 1 | PROCESSED | 57603.3954166667 | 2016-08-03 09:29:24 | 56582 | 2013-10-17 00:00:00 | 56212.7247916667 | 2012-10-12 17:23:42 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIN'YA YAMADA | JAP | 6 | AO6 | REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406013010/ | Quick Look | ![]() |
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111 | AXP 4U 0142+614 | 26.5682 | 61.7591 | 25.700455 | 61.509234 | 52.151654 | 46.394786 | 129.37061357 | -0.42523158 | 40.384 | 55811.6552314815 | 2011-09-07 15:43:32 | 55812.5731134259 | 2011-09-08 13:45:17 | 406031010 | 38.6497 | 60 | 38.6497 | 38.6497 | 0 | 38.6825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.1964 | 42.1964 | 79.292 | 0 | PROCESSED | 57603.1220138889 | 2016-08-03 02:55:42 | 56218 | 2012-10-18 00:00:00 | 55851.4406828704 | 2011-10-17 10:34:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUJIN NAKAGAWA | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406031010/ | Quick Look | ![]() |
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112 | NGC 253 | 11.9272 | -25.3509 | 11.313264 | -25.623648 | 0.061683 | -27.85028 | 97.52826827 | -88.03578801 | 242.9951 | 56643.3716203704 | 2013-12-17 08:55:08 | 56645.502962963 | 2013-12-19 12:04:16 | 808053010 | 99.6864 | 100 | 99.6864 | 99.6864 | 0 | 99.6864 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.5642 | 98.5642 | 184.1038 | 0 | PROCESSED | 57613.6331481482 | 2016-08-13 15:11:44 | 57031 | 2015-01-09 00:00:00 | 56664.7662962963 | 2014-01-07 18:23:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080070 | We propose the observation of edge-on starburst galaxies NGC253 and NGC 2146 for 150 ks and 100 ks, respectively. One of the mechanisms that promote the chemical evolution of the universe, starburst outflows have been studied from both aspects of multi-wavelength observations and theory so far. Suzaku original attempts focusing on the abundance patterns has given new insights for a starburst-driven outflow scenario. In AO8, we try to extract the abundance pattern from the south region in NGC 253 and the central region in NGC 2146. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOSHIKI SATO | JAP | 8 | AO8 | OBSERVATION OF EDGE-ON STARBURST GALAXIES NGC 253 & NGC 2146 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808053010/ | Quick Look | ![]() |
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113 | H1743-322 | 266.5672 | -32.235 | 265.751321 | -32.216345 | 267.052375 | -8.828926 | 357.25482673 | -1.83530791 | 277.9713 | 56212.4049884259 | 2012-10-12 09:43:11 | 56213.3744560185 | 2012-10-13 08:59:13 | 407005030 | 21.361 | 40 | 21.3706 | 21.3722 | 0 | 21.361 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 40.615 | 40.615 | 83.736 | 1 | PROCESSED | 57607.7385416667 | 2016-08-07 17:43:30 | 56598 | 2013-11-02 00:00:00 | 56232.473275463 | 2012-11-01 11:21:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005030/ | Quick Look | ![]() |
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114 | CYG X-1 | 299.5875 | 35.2031 | 299.117489 | 35.06664 | 313.660052 | 54.251673 | 71.33506579 | 3.06957776 | 88.7802 | 56390.0953472222 | 2013-04-08 02:17:18 | 56391.9585532407 | 2013-04-09 23:00:19 | 407015010 | 4.1499 | 85 | 8.503 | 4.1499 | 0 | 66.4751 | 2 | 1 | 0 | 1 | 1 | 0 | 0 | 71.7128 | 71.7128 | 160.9658 | 3 | PROCESSED | 57611.2046875 | 2016-08-11 04:54:45 | 56808 | 2014-05-31 00:00:00 | 56402.1391087963 | 2013-04-20 03:20:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA YAMADA | JAP | 7 | AO7 | INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015010/ | Quick Look | ![]() |
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115 | Z CAM | 126.3 | 73.123 | 124.909699 | 73.28505 | 106.108743 | 51.709102 | 141.36861973 | 32.62424745 | 91.2043 | 56239.0368981482 | 2012-11-08 00:53:08 | 56239.7800347222 | 2012-11-08 18:43:15 | 407016010 | 35.852 | 35 | 35.852 | 35.852 | 0 | 35.852 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.8968 | 33.8968 | 64.1939 | 1 | PROCESSED | 57607.9797337963 | 2016-08-07 23:30:49 | 56631 | 2013-12-05 00:00:00 | 56264.602349537 | 2012-12-03 14:27:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 7 | AO7 | COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407016010/ | Quick Look | ![]() |
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116 | AX J1445.7-5931 | 221.4519 | -59.5275 | 220.50216 | -59.317243 | 239.705831 | -41.083897 | 316.97780419 | 0.18867801 | 281.526 | 56143.2829513889 | 2012-08-04 06:47:27 | 56144.2918865741 | 2012-08-05 07:00:19 | 407021010 | 40.0525 | 40 | 41.0682 | 41.0602 | 0 | 40.0525 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 36.8089 | 36.8089 | 87.1579 | 1 | PROCESSED | 57606.7459722222 | 2016-08-06 17:54:12 | 56533 | 2013-08-29 00:00:00 | 56167.2116319444 | 2012-08-28 05:04:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUO MAKISHIMA | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407021010/ | Quick Look | ![]() |
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117 | IGR J17091-3624 | 257.2866 | -36.4073 | 256.446112 | -36.344023 | 259.498562 | -13.427876 | 349.52701092 | 2.20940495 | 283.8915 | 56202.8636689815 | 2012-10-02 20:43:41 | 56203.7202662037 | 2012-10-03 17:17:11 | 407037010 | 42.0759 | 120 | 42.0759 | 42.0837 | 0 | 42.0797 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 40.392 | 40.392 | 74.0079 | 0 | PROCESSED | 57607.2660069444 | 2016-08-07 06:23:03 | 56728 | 2014-03-12 00:00:00 | 56226.6701388889 | 2012-10-26 16:05:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUTAKA YAMAOKA | JAP | 7 | AO7 | SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407037010/ | Quick Look | ![]() |
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118 | PG 1658 +440 | 254.9348 | 44.0094 | 254.55381 | 44.082621 | 242.595421 | 66.02047 | 69.11167171 | 38.06633743 | 330.9998 | 56115.6740972222 | 2012-07-07 16:10:42 | 56116.8301041667 | 2012-07-08 19:55:21 | 407040010 | 51.0329 | 50 | 51.0329 | 51.0329 | 0 | 51.0329 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46.6746 | 46.6746 | 99.8718 | 1 | PROCESSED | 57606.5897222222 | 2016-08-06 14:09:12 | 56508 | 2013-08-04 00:00:00 | 56142.1447337963 | 2012-08-03 03:28:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ATSUSHI HARAYAMA | JAP | 7 | AO7 | SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407040010/ | Quick Look | ![]() |
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119 | GC20 | 265.6604 | -28.73 | 264.867608 | -28.707008 | 266.169302 | -5.346539 | 359.83402449 | 0.66365416 | 262.9349 | 54385.4117939815 | 2007-10-12 09:52:59 | 54385.9099421296 | 2007-10-12 21:50:19 | 502008010 | 23.7786 | 20 | 23.7906 | 23.7866 | 0 | 23.7786 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.9234 | 22.9234 | 43.032 | 0 | PROCESSED | 57540.2572337963 | 2016-06-01 06:10:25 | 54771 | 2008-11-01 00:00:00 | 54403.0227314815 | 2007-10-30 00:32:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502008010/ | Quick Look | ![]() |
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120 | 4U 0142+61 | 26.5838 | 61.7628 | 25.715895 | 61.512967 | 52.16359 | 46.394147 | 129.37704782 | -0.4200572 | 82.997 | 56504.4205902778 | 2013-07-31 10:05:39 | 56506.6252430556 | 2013-08-02 15:00:21 | 408011010 | 101.1678 | 100 | 101.1678 | 101.1828 | 0 | 101.1828 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.4739 | 102.4739 | 190.4637 | 1 | PROCESSED | 57612.1558680556 | 2016-08-12 03:44:27 | 56953 | 2014-10-23 00:00:00 | 56587.5059606482 | 2013-10-22 12:08:35 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080035 | A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61. | GALACTIC POINT SOURCES | 4 | A | TERUAKI ENOTO | JAP | 8 | AO8 | TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408011010/ | Quick Look | ![]() |
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121 | SGR 0501+4516 | 75.2774 | 45.2864 | 74.365802 | 45.213531 | 78.849797 | 22.414701 | 161.53821228 | 1.95483036 | 87.7054 | 56535.9761574074 | 2013-08-31 23:25:40 | 56536.8752662037 | 2013-09-01 21:00:23 | 408013010 | 36.1244 | 40 | 36.1244 | 41.2611 | 0 | 41.2452 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 35.7177 | 35.7177 | 77.6719 | 1 | PROCESSED | 57612.459375 | 2016-08-12 11:01:30 | 56974 | 2014-11-13 00:00:00 | 56608.6586342593 | 2013-11-12 15:48:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080040 | Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. | GALACTIC POINT SOURCES | 4 | B | TERUAKI ENOTO | JAP | 8 | AO8 | ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408013010/ | Quick Look | ![]() |
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122 | SAGITTARIUS A* | 266.4146 | -29.0065 | 265.619896 | -28.987158 | 266.840205 | -5.604694 | 359.94434823 | -0.0438121 | 107.0001 | 56728.6474537037 | 2014-03-12 15:32:20 | 56729.1147569445 | 2014-03-13 02:45:15 | 408017060 | 21.1387 | 20 | 21.1427 | 21.1387 | 0 | 21.1595 | 2 | 2 | 0 | 3 | 1 | 0 | 0 | 20.4844 | 20.4844 | 40.368 | 0 | PROCESSED | 57614.0078240741 | 2016-08-14 00:11:16 | 57113 | 2015-04-01 00:00:00 | 56747.6540972222 | 2014-03-31 15:41:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017060/ | Quick Look | ![]() |
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123 | X 1630-472 | 248.5012 | -47.3939 | 247.580186 | -47.289758 | 254.085797 | -25.132076 | 336.90807869 | 0.25236055 | 88.6321 | 57077.0625578704 | 2015-02-24 01:30:05 | 57078.1140277778 | 2015-02-25 02:44:12 | 409007020 | 5.5296 | 40 | 5.547 | 5.5659 | 0 | 5.5296 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6879282407 | 2016-08-17 16:30:37 | 57454 | 2016-03-07 00:00:00 | 57087.4605208333 | 2015-03-06 11:03:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | 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 | YOSHIHIRO UEDA | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007020/ | Quick Look | ![]() |
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124 | ASO0376 | 263.1417 | -31.5448 | 262.331507 | -31.509592 | 264.088273 | -8.244108 | 356.29011362 | 0.99386623 | 267.5095 | 55082.1506365741 | 2009-09-08 03:36:55 | 55083.1084606482 | 2009-09-09 02:36:11 | 504049010 | 37.2278 | 20 | 38.9878 | 39.2598 | 0 | 37.2278 | 5 | 4 | 0 | 4 | 1 | 0 | 0 | 31.8134 | 31.8134 | 82.7299 | 1 | PROCESSED | 57548.4976041667 | 2016-06-09 11:56:33 | 55479 | 2010-10-10 00:00:00 | 55113.2260069444 | 2009-10-09 05:25:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504049010/ | Quick Look | ![]() |
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125 | H1743-322 | 266.2607 | -32.2285 | 265.444935 | -32.208359 | 266.789922 | -8.828952 | 357.12541364 | -1.6105206 | 285.4288 | 56932.6365625 | 2014-10-02 15:16:39 | 56933.284837963 | 2014-10-03 06:50:10 | 409008010 | 15.0094 | 40 | 15.6012 | 15.6169 | 0 | 15.0094 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6096527778 | 2016-08-16 14:37:54 | 57345 | 2015-11-19 00:00:00 | 56979.4022569444 | 2014-11-18 09:39:15 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | 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 | YOSHIHIRO UEDA | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008010/ | Quick Look | ![]() |
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126 | A2163SE | 244.1024 | -6.3096 | 243.434314 | -6.186546 | 243.31547 | 14.764116 | 6.72311865 | 30.24259241 | 94.6291 | 57074.4179282407 | 2015-02-21 10:01:49 | 57075.8002662037 | 2015-02-22 19:12:23 | 809009010 | 43.2945 | 50 | 43.2945 | 51.0623 | 0 | 51.0943 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6399421296 | 2016-08-17 15:21:31 | 57453 | 2016-03-06 00:00:00 | 57087.4694212963 | 2015-03-06 11:15:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809009010/ | Quick Look | ![]() |
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127 | H1743-322 | 266.5672 | -32.2343 | 265.751326 | -32.215645 | 267.052358 | -8.828226 | 357.25542532 | -1.83494451 | 273.3773 | 56939.7339236111 | 2014-10-09 17:36:51 | 56940.5245138889 | 2014-10-10 12:35:18 | 409008020 | 19.0006 | 40 | 19.0006 | 19.0145 | 0 | 19.0115 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6317824074 | 2016-08-16 15:09:46 | 57345 | 2015-11-19 00:00:00 | 56979.407974537 | 2014-11-18 09:47:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | 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 | YOSHIHIRO UEDA | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409008020/ | Quick Look | ![]() |
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128 | SAGITTARIUS A* | 266.4193 | -29.0102 | 265.624572 | -28.990881 | 266.844426 | -5.60829 | 359.94333122 | -0.04924818 | 267.3027 | 56929.1441550926 | 2014-09-29 03:27:35 | 56929.6668402778 | 2014-09-29 16:00:15 | 409011010 | 20.2183 | 20 | 20.2183 | 20.3303 | 0 | 20.3543 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5861226852 | 2016-08-16 14:04:01 | 56748 | 2014-04-01 00:00:00 | 56979.4039814815 | 2014-11-18 09:41:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011010/ | Quick Look | ![]() |
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129 | SAGITTARIUS A* | 266.4217 | -29.0078 | 265.626986 | -28.988492 | 266.846474 | -5.605838 | 359.94647323 | -0.04978962 | 278.8011 | 56938.0879861111 | 2014-10-08 02:06:42 | 56938.4619097222 | 2014-10-08 11:05:09 | 409011020 | 17.2605 | 20 | 17.2605 | 17.2605 | 0 | 17.2605 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6209606482 | 2016-08-16 14:54:11 | 56748 | 2014-04-01 00:00:00 | 56979.4091087963 | 2014-11-18 09:49:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011020/ | Quick Look | ![]() |
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130 | 1RXSJ182853.8-241746 | 277.2212 | -24.2932 | 276.455559 | -24.326354 | 276.570172 | -1.017121 | 8.76671438 | -6.19414371 | 87.3419 | 57120.5005092593 | 2015-04-08 12:00:44 | 57120.8217476852 | 2015-04-08 19:43:19 | 409013010 | 9.7072 | 12 | 9.7072 | 11.8422 | 0 | 11.8502 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9447453704 | 2016-08-17 22:40:26 | 57496 | 2016-04-18 00:00:00 | 57129.4074189815 | 2015-04-17 09:46:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 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 | B | HIDEYUKI MORI | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409013010/ | Quick Look | ![]() |
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131 | GK PER | 52.8052 | 43.8974 | 51.953057 | 43.727495 | 61.505862 | 24.068527 | 150.96310366 | -10.10758836 | 250.0842 | 57086.777037037 | 2015-03-05 18:38:56 | 57090.7709606482 | 2015-03-09 18:30:11 | 409018020 | 182.886 | 140 | 0 | 0 | 0 | 182.886 | 0 | 0 | 0 | 2 | 1 | 0 | 0 | 134.9166 | 134.9166 | 344.9376 | 0 | PROCESSED | 57617.786712963 | 2016-08-17 18:52:52 | 57468 | 2016-03-21 00:00:00 | 57101.0913657407 | 2015-03-20 02:11:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090055 | A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI YUASA | JAP | 9 | AO9 | CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018020/ | Quick Look | ![]() |
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132 | Crab nebula | 83.6222 | 22.1365 | 82.869251 | 22.10376 | 84.094492 | -1.173718 | 184.44846107 | -5.72755512 | 86.8666 | 53608.2089236111 | 2005-08-26 05:00:51 | 53608.316087963 | 2005-08-26 07:35:10 | 100010080 | 3.382 | 5 | 3.382 | 3.382 | 3.382 | 3.382 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.7003 | 3.7003 | 9.2539 | 0 | PROCESSED | 57526.9140856482 | 2016-05-18 21:56:17 | 54247 | 2007-05-27 00:00:00 | 54119.0056134259 | 2007-01-19 00:08:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010080/ | Quick Look | ![]() |
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133 | VELA JR P26 | 132.8787 | -46.6693 | 132.45444 | -46.480585 | 159.781455 | -60.154541 | 266.46476457 | -1.49839932 | 347.0019 | 54653.4341203704 | 2008-07-06 10:25:08 | 54653.837025463 | 2008-07-06 20:05:19 | 503038010 | 14.553 | 10 | 14.553 | 14.553 | 0 | 14.553 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.9536 | 10.9536 | 34.7839 | 0 | PROCESSED | 57542.9869675926 | 2016-06-03 23:41:14 | 55048 | 2009-08-05 00:00:00 | 54679.3709606482 | 2008-08-01 08:54:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503038010/ | Quick Look | ![]() |
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134 | 1RXJ0603 | 90.7832 | 42.2686 | 89.889602 | 42.270241 | 90.61448 | 18.829705 | 170.16927881 | 9.72454424 | 80.0992 | 56207.7131828704 | 2012-10-07 17:06:59 | 56210.6307986111 | 2012-10-10 15:08:21 | 807001010 | 124.3416 | 120 | 124.3511 | 124.3439 | 0 | 124.3416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 125.1948 | 125.1948 | 252.0559 | 1 | PROCESSED | 57607.7803009259 | 2016-08-07 18:43:38 | 56595 | 2013-10-30 00:00:00 | 56226.6645717593 | 2012-10-26 15:56:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070025 | We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HIROKI AKAMATSU | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807001010/ | Quick Look | ![]() |
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135 | A1674 | 195.9676 | 67.5471 | 195.510877 | 67.814977 | 143.551001 | 62.83408 | 121.10331631 | 49.53698634 | 114.9985 | 54085.1434837963 | 2006-12-16 03:26:37 | 54087.0426388889 | 2006-12-18 01:01:24 | 801062010 | 68.4138 | 100 | 68.4218 | 68.4218 | 0 | 68.4138 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.0131 | 109.0131 | 164.064 | 2 | PROCESSED | 57536.3777546296 | 2016-05-28 09:03:58 | 54750 | 2008-10-11 00:00:00 | 54094.6003935185 | 2006-12-25 14:24:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801062010/ | Quick Look | ![]() |
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136 | FORNAX A W-LOBE W | 50.2219 | -37.0341 | 49.742698 | -37.213173 | 32.331063 | -52.814253 | 239.92107074 | -57.06786371 | 27.0759 | 54990.6810763889 | 2009-06-08 16:20:45 | 54991.75375 | 2009-06-09 18:05:24 | 804036010 | 60.3625 | 50 | 60.3625 | 60.3625 | 0 | 60.3625 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.3965 | 56.3965 | 92.6519 | 1 | PROCESSED | 57547.532974537 | 2016-06-08 12:47:29 | 55367 | 2010-06-20 00:00:00 | 55001.0562615741 | 2009-06-19 01:21:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MAKOTO TASHIRO | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804036010/ | Quick Look | ![]() |
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137 | COMA_45OFF | 194.2558 | 27.5714 | 193.650381 | 27.84154 | 181.073902 | 30.760176 | 52.91406039 | 88.6829823 | 127.9482 | 54436.4228703704 | 2007-12-02 10:08:56 | 54437.2085185185 | 2007-12-03 05:00:16 | 802047010 | 31.6151 | 30 | 31.6151 | 31.6151 | 0 | 31.6151 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.1691 | 26.1691 | 67.824 | 0 | PROCESSED | 57540.7702083333 | 2016-06-01 18:29:06 | 54814 | 2008-12-14 00:00:00 | 54445.1600925926 | 2007-12-11 03:50:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SUSUMU INOUE | JAP | 2 | AO2 | EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802047010/ | Quick Look | ![]() |
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138 | CYGNUS_LOOP_P8 | 313.9965 | 31.4722 | 313.478406 | 31.279742 | 329.042886 | 46.311836 | 75.29540263 | -8.88432445 | 62.5181 | 53868.0059837963 | 2006-05-13 00:08:37 | 53868.1717476852 | 2006-05-13 04:07:19 | 501028010 | 4.8706 | 6 | 4.8706 | 4.8706 | 4.8706 | 4.8706 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.328 | 2.328 | 14.316 | 0 | PROCESSED | 57534.2851736111 | 2016-05-26 06:50:39 | 54394 | 2007-10-21 00:00:00 | 53914.3326157407 | 2006-06-28 07:58:58 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501028010/ | Quick Look | ![]() |
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139 | M82 X-1 | 149.1432 | 69.7042 | 148.108278 | 69.941832 | 119.044016 | 52.159559 | 141.33659361 | 40.60182861 | 163.0524 | 54367.135775463 | 2007-09-24 03:15:31 | 54367.8716898148 | 2007-09-24 20:55:14 | 702026010 | 35.5999 | 40 | 36.0319 | 35.5999 | 0 | 36.0239 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.4749 | 30.4749 | 63.5699 | 1 | PROCESSED | 57540.0638194444 | 2016-06-01 01:31:54 | 54770 | 2008-10-31 00:00:00 | 54402.2563657407 | 2007-10-29 06:09:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYOHEI MIYAWAKI | JAP | 2 | AO2 | HARD X-RAY SPECTRAL STUDY OF M82 X-1 WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702026010/ | Quick Look | ![]() |
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140 | 1H0323+342 | 51.1746 | 34.1741 | 50.388045 | 33.998103 | 57.519907 | 15.008853 | 155.73224486 | -18.75935356 | 251.4848 | 56352.6173611111 | 2013-03-01 14:49:00 | 56354.8078819444 | 2013-03-03 19:23:21 | 707015010 | 101.272 | 100 | 101.288 | 101.272 | 0 | 101.288 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.1283 | 97.1283 | 189.2516 | 0 | PROCESSED | 57610.7547916667 | 2016-08-10 18:06:54 | 56739 | 2014-03-23 00:00:00 | 56372.5724189815 | 2013-03-21 13:44:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 7 | AO7 | STUDY OF X-RAY SPECTRAL VARIABILITY OF A NARROW-LINE RADIO-LOUD GAMAM-RAY EMITTING SEYFERT 1 GALAXY 1H0323+342 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707015010/ | Quick Look | ![]() |
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141 | PSR J1957+5036 | 299.4354 | 50.5474 | 299.08901 | 50.41133 | 327.273287 | 68.217535 | 84.58480161 | 10.99652902 | 216.5649 | 55543.4586689815 | 2010-12-13 11:00:29 | 55544.0842939815 | 2010-12-14 02:01:23 | 405016010 | 32.469 | 30 | 32.485 | 32.469 | 0 | 32.485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.3139 | 25.3139 | 54.0339 | 2 | PROCESSED | 57554.3965393518 | 2016-06-15 09:31:01 | 55959 | 2012-02-02 00:00:00 | 55592.9341782407 | 2011-01-31 22:25:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405016010/ | Quick Look | ![]() |
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142 | VELA PWN N4 | 128.8415 | -44.0453 | 128.410682 | -43.871484 | 152.26227 | -59.375821 | 262.64764922 | -2.10667439 | 326.4998 | 56110.0169097222 | 2012-07-02 00:24:21 | 56110.3459953704 | 2012-07-02 08:18:14 | 507051010 | 17.289 | 15 | 17.289 | 17.289 | 0 | 17.289 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.6558 | 17.6558 | 28.4019 | 0 | PROCESSED | 57606.5331018518 | 2016-08-06 12:47:40 | 56646 | 2013-12-20 00:00:00 | 56280.6029050926 | 2012-12-19 14:28:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507051010/ | Quick Look | ![]() |
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143 | VELA PWN W1 | 128.3503 | -45.1912 | 127.929525 | -45.019236 | 152.791152 | -60.544208 | 263.35940671 | -3.07091685 | 303.5014 | 56438.6169444444 | 2013-05-26 14:48:24 | 56439.0342476852 | 2013-05-27 00:49:19 | 508042010 | 14.1172 | 15 | 14.1172 | 14.1252 | 0 | 14.1252 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2844 | 13.2844 | 36.0239 | 0 | PROCESSED | 57611.3765046296 | 2016-08-11 09:02:10 | 56864 | 2014-07-26 00:00:00 | 56498.6138888889 | 2013-07-25 14:44:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, 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 western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508042010/ | Quick Look | ![]() |
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144 | G359.0-0.9 NW | 266.56 | -30.3287 | 265.756777 | -30.310042 | 266.999862 | -6.92337 | 358.88098313 | -0.83974756 | 102 | 56723.5510648148 | 2014-03-07 13:13:32 | 56724.8162268518 | 2014-03-08 19:35:22 | 508058010 | 52.0885 | 50 | 52.0885 | 52.0965 | 0 | 52.1045 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.5738 | 45.5738 | 109.2758 | 2 | PROCESSED | 57613.9935416667 | 2016-08-13 23:50:42 | 57100 | 2015-03-19 00:00:00 | 56734.6649189815 | 2014-03-18 15:57:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508058010/ | Quick Look | ![]() |
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145 | SS433_JET_KNOT | 288.5694 | 4.9037 | 287.951117 | 4.816458 | 290.852472 | 27.010013 | 39.90628699 | -2.82264549 | 256.6998 | 56597.9130555556 | 2013-11-01 21:54:48 | 56600.2502314815 | 2013-11-04 06:00:20 | 508024010 | 106.8942 | 100 | 106.8942 | 106.8942 | 0 | 106.8942 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.4583 | 102.4583 | 201.8897 | 3 | PROCESSED | 57613.2427777778 | 2016-08-13 05:49:36 | 56980 | 2014-11-19 00:00:00 | 56611.6875578704 | 2013-11-15 16:30:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080065 | We propose an observation of the jet of SS 433. Our purpose is to detect high-temperature diffuse plasma component made by the black hole jet. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDEKI UCHIYAMA | JAP | 8 | AO8 | SEARCHING DIFFUSE HOT-PLASMA COMPONENT MADE BY A BLACK HOLE JET OF SS 433 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508024010/ | Quick Look | ![]() |
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146 | AWM7 NW2 | 42.4678 | 42.1132 | 41.659195 | 41.906559 | 53.004907 | 24.584739 | 145.29354682 | -15.55850289 | 257.0018 | 56705.8674421296 | 2014-02-17 20:49:07 | 56706.6667824074 | 2014-02-18 16:00:10 | 808024010 | 35.333 | 35 | 35.341 | 35.333 | 0 | 35.349 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0596 | 30.0596 | 69.0559 | 0 | PROCESSED | 57613.8687268518 | 2016-08-13 20:50:58 | 57130 | 2015-04-18 00:00:00 | 56764.8062847222 | 2014-04-17 19:21:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808024010/ | Quick Look | ![]() |
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147 | GC_SGR_B_EAST | 267.0203 | -28.3518 | 266.229607 | -28.335406 | 267.358668 | -4.938031 | 0.77973231 | -0.1584432 | 71.8708 | 54162.5141203704 | 2007-03-03 12:20:20 | 54164.5273726852 | 2007-03-05 12:39:25 | 501039010 | 96.4018 | 100 | 96.4018 | 96.4018 | 0 | 96.4018 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.0829 | 91.0829 | 173.9318 | 3 | PROCESSED | 57537.6522800926 | 2016-05-29 15:39:17 | 54736 | 2008-09-27 00:00:00 | 54171.4429050926 | 2007-03-12 10:37:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501039010/ | Quick Look | ![]() |
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148 | CXO J172641.7-354052 | 261.6769 | -35.6761 | 260.838718 | -35.633773 | 263.074511 | -12.434469 | 352.17176486 | -0.26901827 | 279.4529 | 56540.003275463 | 2013-09-05 00:04:43 | 56540.8015509259 | 2013-09-05 19:14:14 | 408021010 | 37.3165 | 40 | 37.3317 | 37.3349 | 0 | 37.3165 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 35.3693 | 35.3693 | 68.9659 | 0 | PROCESSED | 57612.5112037037 | 2016-08-12 12:16:08 | 56956 | 2014-10-26 00:00:00 | 56587.7063541667 | 2013-10-22 16:57:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080100 | We propose an additional Suzaku observation of an unclassified gamma-ray source detected with the Fermi LAT telescope. In previous cycles, we found an enigmatic source XSS J12270-4859 to be the first gamma-ray binary among the low-mass X-ray binaries. This proposal aims to find a second source of the same nature for the most prospective target extracted from our catalogue search. | GALACTIC POINT SOURCES | 4 | C | MASAHIRO TSUJIMOTO | JAP | 8 | AO8 | X-RAY SEARCH OF ANOTHER ENIGMATIC SOURCE IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408021010/ | Quick Look | ![]() |
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149 | CYGNUS X-3 | 308.2593 | 40.981 | 307.808438 | 40.809488 | 328.80084 | 56.880196 | 79.93230299 | 0.62160244 | 252.424 | 54052.0902893518 | 2006-11-13 02:10:01 | 54054.3676388889 | 2006-11-15 08:49:24 | 401011010 | 99.7445 | 100 | 99.7462 | 99.7462 | 0 | 99.7445 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.3893 | 95.3893 | 196.745 | 1 | PROCESSED | 57536.1520717593 | 2016-05-28 03:38:59 | 54456 | 2007-12-22 00:00:00 | 54088.9545023148 | 2006-12-19 22:54:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHUNJI KITAMOTO | JAP | 1 | AO1 | WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU | SPE | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401011010/ | Quick Look | ![]() |
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150 | 1RXS J070407.9+26250 | 106.0341 | 26.4126 | 105.260164 | 26.487679 | 104.355942 | 3.767203 | 190.27497025 | 14.29877104 | 282.0717 | 54548.4868865741 | 2008-03-23 11:41:07 | 54549.9862384259 | 2008-03-24 23:40:11 | 402008010 | 58.3157 | 50 | 58.3237 | 58.3157 | 0 | 58.3237 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 49.4766 | 49.4766 | 129.5278 | 0 | PROCESSED | 57541.9808912037 | 2016-06-02 23:32:29 | 54933 | 2009-04-12 00:00:00 | 54566.326712963 | 2008-04-10 07:50:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MANABU ISHIDA | JAP | 2 | AO2 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402008010/ | Quick Look | ![]() |
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151 | U SCO | 245.6288 | -17.8156 | 244.907071 | -17.699112 | 246.808077 | 3.684973 | 357.72079613 | 21.90901194 | 93.2747 | 55233.0102430556 | 2010-02-06 00:14:45 | 55234.2918865741 | 2010-02-07 07:00:19 | 404018010 | 46.0764 | 20 | 46.0764 | 46.0764 | 0 | 46.0764 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.6117 | 37.6117 | 110.7199 | 1 | PROCESSED | 57550.518599537 | 2016-06-11 12:26:47 | 55617 | 2011-02-25 00:00:00 | 55250.1559375 | 2010-02-23 03:44:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | DAI TAKEI | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018010/ | Quick Look | ![]() |
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152 | HESSJ1741-A | 265.3548 | -30.1316 | 264.55314 | -30.107106 | 265.945938 | -6.755753 | 358.50289854 | 0.15030933 | 73.8229 | 54886.7117013889 | 2009-02-24 17:04:51 | 54888.0419328704 | 2009-02-26 01:00:23 | 503076010 | 52.9323 | 50 | 52.9323 | 52.9323 | 0 | 52.9323 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7708 | 43.7708 | 114.9158 | 1 | PROCESSED | 57545.6752546296 | 2016-06-06 16:12:22 | 55330 | 2010-05-14 00:00:00 | 54902.4869791667 | 2009-03-12 11:41:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503076010/ | Quick Look | ![]() |
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153 | II PEG | 358.7744 | 28.6284 | 358.137778 | 28.350132 | 11.171995 | 26.557383 | 108.23861581 | -32.63076231 | 231.1411 | 56301.1877314815 | 2013-01-09 04:30:20 | 56303.6487962963 | 2013-01-11 15:34:16 | 407038010 | 17.0176 | 100 | 111.5065 | 111.5145 | 0 | 17.0176 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 107.9058 | 107.9058 | 212.6198 | 2 | PROCESSED | 57608.5074305556 | 2016-08-08 12:10:42 | 56724 | 2014-03-08 00:00:00 | 56363.602037037 | 2013-03-12 14:26:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOHKO TSUBOI | JAP | 7 | AO7 | NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEG | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407038010/ | Quick Look | ![]() |
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154 | SWIFT J1922.7-1716 | 290.6403 | -17.2233 | 289.918336 | -17.319807 | 289.738469 | 4.813727 | 20.73500926 | -14.48356253 | 80.064 | 54198.231099537 | 2007-04-08 05:32:47 | 54200.4321643518 | 2007-04-10 10:22:19 | 702028010 | 78.6386 | 80 | 78.6386 | 78.6386 | 0 | 78.6386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.3533 | 61.3533 | 190.1298 | 0 | PROCESSED | 57538.1728356482 | 2016-05-30 04:08:53 | 54744 | 2008-10-05 00:00:00 | 54206.3754166667 | 2007-04-16 09:00:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 2 | AO2 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702028010/ | Quick Look | ![]() |
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155 | 2MASX J15115979-2119 | 227.9997 | -21.3083 | 227.279118 | -21.120692 | 231.351076 | -3.323732 | 341.57056512 | 30.81939061 | 105.6253 | 55979.0551388889 | 2012-02-22 01:19:24 | 55980.937650463 | 2012-02-23 22:30:13 | 706010010 | 83.8162 | 80 | 83.8162 | 83.8162 | 0 | 83.8162 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.2568 | 82.2568 | 162.6359 | 1 | PROCESSED | 57604.7185763889 | 2016-08-04 17:14:45 | 56361 | 2013-03-10 00:00:00 | 55995.1640393518 | 2012-03-09 03:56:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 6 | AO6 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706010010/ | Quick Look | ![]() |
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156 | FJ1 | 238.114 | 22.5674 | 237.571568 | 22.715547 | 229.271734 | 41.603316 | 36.86878642 | 48.89749971 | 115.0005 | 56698.0557638889 | 2014-02-10 01:20:18 | 56701.0001851852 | 2014-02-13 00:00:16 | 808041010 | 111.8457 | 100 | 111.8537 | 111.8457 | 0 | 111.8537 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8229166667 | 2016-08-13 19:45:00 | 57130 | 2015-04-18 00:00:00 | 56765.6012152778 | 2014-04-18 14:25:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080054 | Filament Junctions are known to be the most active regions in structure formation in the Universe. These regions can be identified using our original method based on galaxy distribution. In AO8, we try to detect (1) a galaxy-scale halo with a radio relic structure often observed after merger and (2) a galaxy-scale halo just before merger at the Filament Junction. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IKUYUKI MITSUISHI | JAP | 8 | AO8 | EXPLORING EVOLUTION OF GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808041010/ | Quick Look | ![]() |
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157 | A1689-OFFSET4 | 197.7965 | -1.1735 | 197.154302 | -0.90795 | 196.855647 | 5.897997 | 313.25406527 | 61.301843 | 290 | 54673.475 | 2008-07-26 11:24:00 | 54674.5091898148 | 2008-07-27 12:13:14 | 803027010 | 42.0199 | 40 | 42.0279 | 42.0279 | 0 | 42.0199 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.8505 | 36.8505 | 89.354 | 2 | PROCESSED | 57543.1496527778 | 2016-06-04 03:35:30 | 55076 | 2009-09-02 00:00:00 | 54707.0673032407 | 2008-08-29 01:36:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803027010/ | Quick Look | ![]() |
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158 | FILAMENT OF GALAXIES | 238.2847 | 27.6247 | 237.767937 | 27.772087 | 227.420415 | 46.484967 | 44.49442625 | 49.89393343 | 305.997 | 55408.8620833333 | 2010-07-31 20:41:24 | 55410.6883101852 | 2010-08-02 16:31:10 | 805030010 | 61.7703 | 80 | 61.7703 | 61.7703 | 0 | 61.7703 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.5833 | 55.5833 | 157.7518 | 0 | PROCESSED | 57552.8205671296 | 2016-06-13 19:41:37 | 55793 | 2011-08-20 00:00:00 | 55427.2133449074 | 2010-08-19 05:07:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050032 | Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAJIME KAWAHARA | JAP | 5 | AO5 | SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805030010/ | Quick Look | ![]() |
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159 | DRACO HVC REGION B | 243.9603 | 59.1738 | 243.739297 | 59.296448 | 199.753416 | 76.165002 | 90.07720195 | 42.68363475 | 80.282 | 53816.0059953704 | 2006-03-22 00:08:38 | 53817.4148611111 | 2006-03-23 09:57:24 | 501005010 | 61.632 | 60 | 61.6447 | 61.644 | 61.632 | 61.636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.6865 | 60.6865 | 121.7099 | 2 | PROCESSED | 57533.3166319444 | 2016-05-25 07:35:57 | 54400 | 2007-10-27 00:00:00 | 53906.4964583333 | 2006-06-20 11:54:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKESHI TSURU | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501005010/ | Quick Look | ![]() |
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160 | CYGNUS_LOOP_P9 | 311.8173 | 30.594 | 311.299257 | 30.409327 | 326.059392 | 46.235255 | 73.41991066 | -7.98099126 | 239.9998 | 54416.7228935185 | 2007-11-12 17:20:58 | 54417.2502199074 | 2007-11-13 06:00:19 | 501019010 | 19.5656 | 15 | 19.5656 | 19.5656 | 0 | 19.5656 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.3446 | 17.3446 | 45.5379 | 0 | PROCESSED | 57540.4965393518 | 2016-06-01 11:55:01 | 54798 | 2008-11-28 00:00:00 | 54430.2327546296 | 2007-11-26 05:35:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501019010/ | Quick Look | ![]() |
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161 | CENA LOBE 2 | 201.7888 | -39.7615 | 201.063878 | -39.502282 | 215.867885 | -28.246306 | 310.35736359 | 22.59471631 | 296.9216 | 56141.4611921296 | 2012-08-02 11:04:07 | 56143.2779861111 | 2012-08-04 06:40:18 | 807041030 | 65.8666 | 65 | 65.8746 | 65.8746 | 0 | 65.8666 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.8659 | 57.8659 | 156.9538 | 2 | PROCESSED | 57606.7677893518 | 2016-08-06 18:25:37 | 56018 | 2012-04-01 00:00:00 | 56162.2467013889 | 2012-08-23 05:55:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807041030/ | Quick Look | ![]() |
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162 | COMA SUBHALO1 S | 195.2527 | 28.7629 | 194.651674 | 29.031827 | 181.36326 | 32.219878 | 71.19878606 | 87.32773157 | 296.8003 | 56452.0686458333 | 2013-06-09 01:38:51 | 56452.5459490741 | 2013-06-09 13:06:10 | 808019010 | 20.4808 | 20 | 20.4888 | 20.4808 | 0 | 20.4968 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.4968 | 21.4968 | 41.2319 | 0 | PROCESSED | 57611.4938541667 | 2016-08-11 11:51:09 | 56869 | 2014-07-31 00:00:00 | 56503.6109606482 | 2013-07-30 14:39:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808019010/ | Quick Look | ![]() |
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163 | A3376 SOUTH | 90.6172 | -40.196 | 90.211877 | -40.194003 | 91.07062 | -63.635447 | 246.775776 | -26.0046965 | 124.8629 | 56580.8395486111 | 2013-10-15 20:08:57 | 56582.2918055556 | 2013-10-17 07:00:12 | 808030010 | 66.5346 | 57 | 66.5347 | 66.5346 | 0 | 66.5346 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 56.9771 | 56.9771 | 125.45 | 1 | PROCESSED | 57613.0188541667 | 2016-08-13 00:27:09 | 57004 | 2014-12-13 00:00:00 | 56637.6639351852 | 2013-12-11 15:56:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808030010/ | Quick Look | ![]() |
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164 | 1RXSJ173905.2-392615 | 264.7748 | -39.4365 | 263.906258 | -39.409033 | 265.79264 | -16.071333 | 350.35081336 | -4.37467046 | 271.2006 | 56188.8237384259 | 2012-09-18 19:46:11 | 56189.3446990741 | 2012-09-19 08:16:22 | 407029010 | 22.0638 | 15 | 22.0718 | 22.0638 | 0 | 22.0718 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.2515 | 18.2515 | 44.9999 | 0 | PROCESSED | 57607.0891898148 | 2016-08-07 02:08:26 | 56584 | 2013-10-19 00:00:00 | 56218.4994212963 | 2012-10-18 11:59:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEYUKI MORI | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407029010/ | Quick Look | ![]() |
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165 | U GEM IN QUIECSECNCE | 118.777 | 21.9977 | 118.037172 | 22.130129 | 116.517698 | 1.166962 | 199.22882002 | 23.39765052 | 280.879 | 56041.5636921296 | 2012-04-24 13:31:43 | 56044.5765856482 | 2012-04-27 13:50:17 | 407034010 | 119.1136 | 120 | 119.1136 | 119.1136 | 0 | 119.1136 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 102.8354 | 102.8354 | 260.306 | 1 | PROCESSED | 57605.3496064815 | 2016-08-05 08:23:26 | 56434 | 2013-05-22 00:00:00 | 56068.6228356482 | 2012-05-21 14:56:53 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI HAYASHI | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407034010/ | Quick Look | ![]() |
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166 | A2163BGD1 | 244.2972 | -6.0675 | 243.630135 | -5.945298 | 243.467732 | 15.036983 | 7.08170195 | 30.23063611 | 97.9997 | 57078.1207523148 | 2015-02-25 02:53:53 | 57078.9737384259 | 2015-02-25 23:22:11 | 809010010 | 28.6539 | 30 | 28.6539 | 28.6619 | 0 | 28.6699 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6666782407 | 2016-08-17 16:00:01 | 57454 | 2016-03-07 00:00:00 | 57087.4740393518 | 2015-03-06 11:22:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809010010/ | Quick Look | ![]() |
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167 | PKS 2356-61 | 359.7661 | -60.908 | 359.120501 | -61.186478 | 324.284485 | -53.222548 | 314.02525269 | -55.07790138 | 249.6445 | 54075.7140740741 | 2006-12-06 17:08:16 | 54078.21625 | 2006-12-09 05:11:24 | 801016010 | 100.8372 | 100 | 100.8452 | 100.8372 | 0 | 100.8532 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.1255 | 92.1255 | 216.1579 | 3 | PROCESSED | 57536.3143171296 | 2016-05-28 07:32:37 | 54456 | 2007-12-22 00:00:00 | 54088.6546759259 | 2006-12-19 15:42:44 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SOOJING HONG | JAP | 1 | AO1 | HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801016010/ | Quick Look | ![]() |
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168 | NGC 4593 | 189.915 | -5.3482 | 189.270103 | -5.073686 | 191.205514 | -0.992169 | 297.48487911 | 57.39893055 | 292.7762 | 56824.1040972222 | 2014-06-16 02:29:54 | 56824.8563888889 | 2014-06-16 20:33:12 | 709014010 | 29.7616 | 30 | 29.7696 | 29.7616 | 0 | 29.7696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.185 | 24.185 | 64.9919 | 1 | PROCESSED | 57615.2408449074 | 2016-08-15 05:46:49 | 57204 | 2015-07-01 00:00:00 | 56835.7291435185 | 2014-06-27 17:29:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014010/ | Quick Look | ![]() |
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169 | HYDRA A-1 | 139.3695 | -11.9475 | 138.767154 | -11.737163 | 145.930071 | -26.316597 | 242.69436566 | 25.06487811 | 95 | 55508.1097569444 | 2010-11-08 02:38:03 | 55509.1800115741 | 2010-11-09 04:19:13 | 805007010 | 42.5647 | 40 | 42.5727 | 42.5647 | 0 | 42.5727 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.2072 | 35.2072 | 92.4558 | 1 | PROCESSED | 57554.0434143518 | 2016-06-15 01:02:31 | 55890 | 2011-11-25 00:00:00 | 55524.1752430556 | 2010-11-24 04:12:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050012 | X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 5 | AO5 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805007010/ | Quick Look | ![]() |
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170 | 1RXS J180340.0+40121 | 270.932 | 40.2098 | 270.526529 | 40.206239 | 271.586717 | 63.644696 | 66.8583442 | 25.77561005 | 157.538 | 54478.0290972222 | 2008-01-13 00:41:54 | 54479.1877777778 | 2008-01-14 04:30:24 | 402009010 | 53.0907 | 50 | 53.0907 | 53.0907 | 0 | 53.0907 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44.3489 | 44.3489 | 100.0959 | 3 | PROCESSED | 57541.2965625 | 2016-06-02 07:07:03 | 54864 | 2009-02-02 00:00:00 | 54490.0707291667 | 2008-01-25 01:41:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MANABU ISHIDA | JAP | 2 | AO2 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402009010/ | Quick Look | ![]() |
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171 | SAGITTARIUS A* | 266.4179 | -29.0156 | 265.623138 | -28.996274 | 266.843332 | -5.613719 | 359.938084 | -0.05101613 | 284.9967 | 56561.9008101852 | 2013-09-26 21:37:10 | 56562.4828587963 | 2013-09-27 11:35:19 | 408017040 | 18.3285 | 20 | 18.3422 | 18.3285 | 0 | 18.3422 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 18.9519 | 18.9519 | 50.282 | 0 | PROCESSED | 57612.7244560185 | 2016-08-12 17:23:13 | 56956 | 2014-10-26 00:00:00 | 56588.4972222222 | 2013-10-23 11:56:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017040/ | Quick Look | ![]() |
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172 | SAGITTARIUS A* | 266.4147 | -29.0052 | 265.620004 | -28.985859 | 266.84026 | -5.603392 | 359.94550345 | -0.04320951 | 106.9995 | 56723.0565277778 | 2014-03-07 01:21:24 | 56723.5487384259 | 2014-03-07 13:10:11 | 408017050 | 21.9949 | 20 | 21.9949 | 22.0029 | 0 | 22.0144 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.862 | 15.862 | 42.5199 | 1 | PROCESSED | 57613.9706828704 | 2016-08-13 23:17:47 | 57100 | 2015-03-19 00:00:00 | 56734.6444328704 | 2014-03-18 15:27:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017050/ | Quick Look | ![]() |
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173 | GALACTIC CENTER | 265.3803 | -29.7558 | 264.581055 | -29.731436 | 265.955939 | -6.379444 | 358.83357751 | 0.33021849 | 269 | 54016.4324074074 | 2006-10-08 10:22:40 | 54017.0968055556 | 2006-10-09 02:19:24 | 501049010 | 19.5627 | 20 | 19.5627 | 19.5627 | 19.5627 | 19.5627 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.6336 | 17.6336 | 57.3959 | 1 | PROCESSED | 57535.7944675926 | 2016-05-27 19:04:02 | 54735 | 2008-09-26 00:00:00 | 54053.4403356482 | 2006-11-14 10:34:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501049010/ | Quick Look | ![]() |
174 | V2301 OPH | 270.1519 | 8.1612 | 269.551065 | 8.161911 | 270.165981 | 31.601449 | 34.53664844 | 14.98247082 | 262.0703 | 56573.9878356482 | 2013-10-08 23:42:29 | 56576.0002893518 | 2013-10-11 00:00:25 | 408024010 | 40.1356 | 150 | 40.1356 | 40.1356 | 0 | 40.1356 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.6843 | 65.6843 | 173.8587 | 1 | PROCESSED | 57612.9068981482 | 2016-08-12 21:45:56 | 57184 | 2015-06-11 00:00:00 | 56596.5744907407 | 2013-10-31 13:47:16 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI HAYASHI | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024010/ | Quick Look | ![]() |
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175 | FILAMENT JUNCTION 3 | 151.4159 | 39.7399 | 150.662748 | 39.98344 | 138.765722 | 26.114357 | 181.90509124 | 53.56333781 | 291.576 | 55672.3023611111 | 2011-04-21 07:15:24 | 55673.6362268518 | 2011-04-22 15:16:10 | 806005010 | 55.0232 | 60 | 55.0232 | 55.0312 | 0 | 55.0392 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.8669 | 49.8669 | 115.2299 | 2 | PROCESSED | 57601.5861921296 | 2016-08-01 14:04:07 | 56061 | 2012-05-14 00:00:00 | 55692.3338425926 | 2011-05-11 08:00:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806005010/ | Quick Look | ![]() |
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176 | NGC 2300 GROUP | 112.8158 | 85.6965 | 108.675805 | 85.795148 | 93.626997 | 62.54508 | 127.72434362 | 27.79082708 | 339.9138 | 55235.7626388889 | 2010-02-08 18:18:12 | 55236.5002893518 | 2010-02-09 12:00:25 | 804030010 | 37.0591 | 100 | 37.0591 | 37.0591 | 0 | 37.0591 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.4534 | 34.4534 | 63.7299 | 1 | PROCESSED | 57550.5366666667 | 2016-06-11 12:52:48 | 55619 | 2011-02-27 00:00:00 | 55251.1588310185 | 2010-02-24 03:48:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804030010/ | Quick Look | ![]() |
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177 | RCW86_WEST | 220.2753 | -62.427 | 219.29491 | -62.212988 | 240.606158 | -43.963376 | 315.24703456 | -2.20673417 | 96.1553 | 54864.7563194444 | 2009-02-02 18:09:06 | 54866.0134259259 | 2009-02-04 00:19:20 | 503001010 | 53.5519 | 50 | 53.5519 | 53.5519 | 0 | 53.5519 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9081 | 48.9081 | 108.602 | 1 | PROCESSED | 57545.4580324074 | 2016-06-06 10:59:34 | 55329 | 2010-05-13 00:00:00 | 54880.570462963 | 2009-02-18 13:41:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503001010/ | Quick Look | ![]() |
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178 | CYGNUS LOOP (P20) | 311.9894 | 31.1824 | 311.473917 | 30.997098 | 326.586885 | 46.721175 | 73.97872298 | -7.73281487 | 50.0002 | 54596.7397685185 | 2008-05-10 17:45:16 | 54597.51 | 2008-05-11 12:14:24 | 503056010 | 30.1129 | 25 | 30.1129 | 30.1343 | 0 | 30.1209 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.2057 | 27.2057 | 66.5339 | 0 | PROCESSED | 57545.8695023148 | 2016-06-06 20:52:05 | 54972 | 2009-05-21 00:00:00 | 54606.1121759259 | 2008-05-20 02:41:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503056010/ | Quick Look | ![]() |
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179 | RCW 86 | 221.2555 | -62.3618 | 220.269135 | -62.150858 | 241.140538 | -43.714444 | 315.68741681 | -2.33681001 | 278.3377 | 53959.4574652778 | 2006-08-12 10:58:45 | 53961.1294907407 | 2006-08-14 03:06:28 | 501037010 | 59.8054 | 60 | 59.8294 | 59.8054 | 59.8294 | 59.8214 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.405 | 54.405 | 144.42 | 1 | PROCESSED | 57535.2984259259 | 2016-05-27 07:09:44 | 54394 | 2007-10-21 00:00:00 | 54021.0740972222 | 2006-10-13 01:46:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYA YAMAGUCHI | JAP | 1 | AO1 | RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501037010/ | Quick Look | ![]() |
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180 | NGC 5347 | 208.2716 | 33.4399 | 207.717601 | 33.685673 | 191.037943 | 41.510938 | 62.06849004 | 75.29189994 | 312.225 | 54627.6603703704 | 2008-06-10 15:50:56 | 54628.6064699074 | 2008-06-11 14:33:19 | 703011010 | 42.1611 | 40 | 42.1611 | 42.1611 | 0 | 42.1611 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1302 | 37.1302 | 81.734 | 1 | PROCESSED | 57542.8072569444 | 2016-06-03 19:22:27 | 55008 | 2009-06-26 00:00:00 | 54637.3250810185 | 2008-06-20 07:48:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 3 | AO3 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703011010/ | Quick Look | ![]() |
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181 | VELA JR P30 | 134.1665 | -46.7036 | 133.737948 | -46.510338 | 161.294913 | -59.700207 | 267.059354 | -0.84402772 | 347.0006 | 54654.7208449074 | 2008-07-07 17:18:01 | 54655.0844328704 | 2008-07-08 02:01:35 | 503042010 | 10.1159 | 10 | 10.1159 | 10.1159 | 0 | 10.1159 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.0536 | 10.0536 | 31.3839 | 0 | PROCESSED | 57542.9967592593 | 2016-06-03 23:55:20 | 55048 | 2009-08-05 00:00:00 | 54679.397962963 | 2008-08-01 09:33:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503042010/ | Quick Look | ![]() |
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182 | 1E1207.4-5209 | 182.5062 | -52.436 | 181.851861 | -52.157726 | 209.149793 | -45.774623 | 296.5458403 | 9.92149786 | 302.4939 | 53946.5682060185 | 2006-07-30 13:38:13 | 53948.2603587963 | 2006-08-01 06:14:55 | 401030010 | 96.3519 | 120 | 96.3519 | 102.2784 | 96.3679 | 96.3519 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 94.0498 | 94.0498 | 135.3799 | 1 | PROCESSED | 57535.1230787037 | 2016-05-27 02:57:14 | 54750 | 2008-10-11 00:00:00 | 54132.8187268518 | 2007-02-01 19:38:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ATSUMASA YOSHIDA | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030010/ | Quick Look | ![]() |
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183 | A2218_offset | 244.4769 | 65.4468 | 244.387309 | 65.566901 | 174.329918 | 79.629039 | 97.72059475 | 40.11912915 | 237.1965 | 53645.3474537037 | 2005-10-02 08:20:20 | 53646.32375 | 2005-10-03 07:46:12 | 100030020 | 44.8592 | 50 | 44.8592 | 46.1907 | 44.9141 | 45.3747 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.5366 | 42.5366 | 84.3439 | 0 | PROCESSED | 57527.5203125 | 2016-05-19 12:29:15 | 54247 | 2007-05-27 00:00:00 | 54036.969224537 | 2006-10-28 23:15:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | A2218 and its offset observation | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100030020/ | Quick Look | ![]() |
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184 | RXJ1713-3946 | 258.1672 | -39.4231 | 257.303004 | -39.36394 | 260.487659 | -16.371231 | 347.50735004 | -0.13585591 | 267.9988 | 53989.9221643518 | 2006-09-11 22:07:55 | 53990.3106712963 | 2006-09-12 07:27:22 | 501065010 | 22.011 | 20 | 22.011 | 22.011 | 22.011 | 22.011 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.7973 | 20.7973 | 33.5579 | 0 | PROCESSED | 57535.5534606482 | 2016-05-27 13:16:59 | 54526 | 2008-03-01 00:00:00 | 54020.8390162037 | 2006-10-12 20:08:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501065010/ | Quick Look | ![]() |
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185 | GC SGR D | 267.0913 | -27.9356 | 266.303192 | -27.919557 | 267.412914 | -4.520645 | 1.16847417 | 0.00287016 | 108.7996 | 54174.7887847222 | 2007-03-15 18:55:51 | 54176.2127199074 | 2007-03-17 05:06:19 | 501059010 | 62.2372 | 63 | 62.2372 | 62.2452 | 0 | 62.2452 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.3697 | 54.3697 | 123.028 | 0 | PROCESSED | 57537.7233912037 | 2016-05-29 17:21:41 | 54736 | 2008-09-27 00:00:00 | 54185.4865740741 | 2007-03-26 11:40:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501059010/ | Quick Look | ![]() |
186 | SAGITTARIUS A* | 266.4197 | -29.0062 | 265.624997 | -28.986883 | 266.844677 | -5.604282 | 359.94692786 | -0.04746309 | 282.0043 | 56539.5310416667 | 2013-09-04 12:44:42 | 56540.000162037 | 2013-09-05 00:00:14 | 408017010 | 19.4579 | 20 | 19.4789 | 19.4579 | 0 | 19.4709 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.6423 | 20.6423 | 40.5219 | 0 | PROCESSED | 57612.4854976852 | 2016-08-12 11:39:07 | 56974 | 2014-11-13 00:00:00 | 56608.6493981482 | 2013-11-12 15:35:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017010/ | Quick Look | ![]() |
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187 | ASO0078 | 59.472 | 32.09 | 58.682067 | 31.946958 | 63.963224 | 11.368156 | 162.76236061 | -16.0043339 | 83.0007 | 55045.8202777778 | 2009-08-02 19:41:12 | 55046.3273032407 | 2009-08-03 07:51:19 | 504041010 | 21.312 | 20 | 21.32 | 21.32 | 0 | 21.312 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.2959 | 21.2959 | 43.7999 | 0 | PROCESSED | 57548.0349074074 | 2016-06-09 00:50:16 | 55430 | 2010-08-22 00:00:00 | 55064.0383912037 | 2009-08-21 00:55:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504041010/ | Quick Look | ![]() |
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188 | E1821+643 | 275.5207 | 64.3306 | 275.456094 | 64.303959 | 318.282096 | 86.807262 | 93.98984501 | 27.40177083 | 228.4067 | 56239.7868981482 | 2012-11-08 18:53:08 | 56241.8217708333 | 2012-11-10 19:43:21 | 707016010 | 100.4132 | 100 | 100.4132 | 100.4132 | 0 | 100.4132 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.5411 | 95.5411 | 175.7799 | 2 | PROCESSED | 57608.0299421296 | 2016-08-08 00:43:07 | 56631 | 2013-12-05 00:00:00 | 56265.6966319444 | 2012-12-04 16:43:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROUMI NODA | JAP | 7 | AO7 | SUZAKU STUDY OF MULTI-ZONE COMPTONIZATION PICTURE ON THE CENTRAL ENGINE OF RADIO-QUIET QUASAR E1821+643 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707016010/ | Quick Look | ![]() |
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189 | A133_S | 15.6819 | -22.1029 | 15.071421 | -22.371383 | 5.125588 | -26.4157 | 150.58121257 | -84.35810156 | 44.9946 | 55355.2966203704 | 2010-06-08 07:07:08 | 55356.727974537 | 2010-06-09 17:28:17 | 805022010 | 51.128 | 50 | 51.128 | 51.128 | 0 | 51.128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8599 | 42.8599 | 123.6558 | 1 | PROCESSED | 57551.9312962963 | 2016-06-12 22:21:04 | 55737 | 2011-06-25 00:00:00 | 55370.2538310185 | 2010-06-23 06:05:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805022010/ | Quick Look | ![]() |
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190 | CYGNUS_LOOP_P17 | 312.199 | 30.014 | 311.677424 | 29.82795 | 326.178147 | 45.573278 | 73.16561663 | -8.59879153 | 61.9999 | 53877.7613657407 | 2006-05-22 18:16:22 | 53878.0446064815 | 2006-05-23 01:04:14 | 501034010 | 14.1953 | 14 | 14.1993 | 14.2033 | 14.1993 | 14.1953 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.8231 | 14.8231 | 24.464 | 0 | PROCESSED | 57534.3944328704 | 2016-05-26 09:27:59 | 54394 | 2007-10-21 00:00:00 | 53926.1395833333 | 2006-07-10 03:21:00 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501034010/ | Quick Look | ![]() |
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191 | JUPITER | 103.8837 | 23.1078 | 103.127442 | 23.17281 | 102.752218 | 0.279385 | 192.54363279 | 11.16228902 | 264.4065 | 56762.7225115741 | 2014-04-15 17:20:25 | 56763.066099537 | 2014-04-16 01:35:11 | 508023030 | 8.9125 | 160 | 8.9125 | 8.9125 | 0 | 8.9125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.9063 | 6.9063 | 22.6469 | 0 | PROCESSED | 57614.254212963 | 2016-08-14 06:06:04 | 57212 | 2015-07-09 00:00:00 | 56833.5559722222 | 2014-06-25 13:20:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023030/ | Quick Look | ![]() |
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192 | HESSJ1741-B | 265.2407 | -30.3098 | 264.437915 | -30.284751 | 265.852586 | -6.937089 | 358.29952005 | 0.1396669 | 74.0024 | 54888.0423611111 | 2009-02-26 01:01:00 | 54889.4828587963 | 2009-02-27 11:35:19 | 503077010 | 51.2616 | 50 | 51.2696 | 51.2616 | 0 | 51.2696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7072 | 43.7072 | 124.4239 | 1 | PROCESSED | 57545.6763773148 | 2016-06-06 16:13:59 | 55330 | 2010-05-14 00:00:00 | 54908.5791550926 | 2009-03-18 13:53:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503077010/ | Quick Look | ![]() |
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193 | 1FGL J2339.7-0531 | 354.9077 | -5.5469 | 354.264388 | -5.824081 | 353.120926 | -3.069352 | 81.34836456 | -62.4702773 | 67.4026 | 55741.5915625 | 2011-06-29 14:11:51 | 55743.8092361111 | 2011-07-01 19:25:18 | 406007010 | 104.0914 | 100 | 104.0914 | 104.0914 | 0 | 104.0994 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.9022 | 92.9022 | 191.5837 | 2 | PROCESSED | 57602.4861805556 | 2016-08-02 11:40:06 | 56144 | 2012-08-05 00:00:00 | 55775.4025925926 | 2011-08-02 09:39:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ALBERT KONG | JUN KATAOKA | JAP | 6 | AO6 | REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406007010/ | Quick Look | ![]() |
194 | NGC 5044 OFFSET2 | 199.1117 | -16.388 | 198.444886 | -16.124395 | 203.827071 | -7.694393 | 311.59229028 | 46.06278821 | 290.7836 | 53920.9609143518 | 2006-07-04 23:03:43 | 53922.7598842593 | 2006-07-06 18:14:14 | 801048010 | 62.451 | 60 | 62.451 | 62.451 | 62.451 | 62.451 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57.1102 | 57.1102 | 155.3149 | 2 | PROCESSED | 57534.8962615741 | 2016-05-26 21:30:37 | 54422 | 2007-11-18 00:00:00 | 54034.2926736111 | 2006-10-26 07:01:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801048010/ | Quick Look | ![]() |
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195 | JUPITER | 104.3715 | 23.0706 | 103.615684 | 23.137913 | 103.202438 | 0.28593 | 192.77027841 | 11.55390373 | 264.582 | 56766.448287037 | 2014-04-19 10:45:32 | 56766.781400463 | 2014-04-19 18:45:13 | 508023090 | 11.9454 | 160 | 11.9534 | 11.9454 | 0 | 11.9614 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9588773148 | 2016-08-14 23:00:47 | 57212 | 2015-07-09 00:00:00 | 56782.506099537 | 2014-05-05 12:08:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023090/ | Quick Look | ![]() |
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196 | SWIFT J1200.8+0650 | 180.2185 | 6.7488 | 179.57779 | 7.027186 | 177.502279 | 6.275772 | 270.13481807 | 66.34579154 | 293.0035 | 54617.9027662037 | 2008-05-31 21:39:59 | 54619.9280555556 | 2008-06-02 22:16:24 | 703009010 | 84.4866 | 80 | 84.5106 | 84.4866 | 0 | 84.5106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.1109 | 71.1109 | 174.9638 | 3 | PROCESSED | 57542.752037037 | 2016-06-03 18:02:56 | 55003 | 2009-06-21 00:00:00 | 54634.1479282407 | 2008-06-17 03:33:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 3 | AO3 | THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703009010/ | Quick Look | ![]() |
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197 | VELA JR P27 | 133.2844 | -46.6061 | 132.858246 | -46.415943 | 160.180564 | -59.949881 | 266.59417196 | -1.24373956 | 347.0008 | 54653.8375925926 | 2008-07-06 20:06:08 | 54654.1668865741 | 2008-07-07 04:00:19 | 503039010 | 11.0337 | 10 | 11.0417 | 11.0417 | 0 | 11.0337 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.3372 | 11.3372 | 28.4479 | 0 | PROCESSED | 57542.9844560185 | 2016-06-03 23:37:37 | 55048 | 2009-08-05 00:00:00 | 54679.3497222222 | 2008-08-01 08:23:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503039010/ | Quick Look | ![]() |
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198 | SGR D SNR | 267.1922 | -28.1274 | 266.402882 | -28.111843 | 267.506075 | -4.710631 | 1.05009547 | -0.17236121 | 267.8977 | 54349.018599537 | 2007-09-06 00:26:47 | 54352.6738310185 | 2007-09-09 16:10:19 | 502020010 | 139.0808 | 133 | 139.0808 | 139.0808 | 0 | 139.0808 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124.5025 | 124.5025 | 315.7798 | 1 | PROCESSED | 57540.026087963 | 2016-06-01 00:37:34 | 54776 | 2008-11-06 00:00:00 | 54371.5203472222 | 2007-09-28 12:29:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 2 | AO2 | OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502020010/ | Quick Look | ![]() |
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199 | SN 1006 SW-Rim | 225.4961 | -42.0706 | 224.678007 | -41.87399 | 235.320846 | -23.835662 | 327.36052248 | 14.52564865 | 117.2713 | 53761.0914930556 | 2006-01-26 02:11:45 | 53761.7155555556 | 2006-01-26 17:10:24 | 100019050 | 28.4186 | 50 | 28.4186 | 28.4186 | 28.4186 | 28.4186 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.7444 | 24.7444 | 53.91 | 0 | PROCESSED | 57532.7834375 | 2016-05-24 18:48:09 | 54247 | 2007-05-27 00:00:00 | 54040.4586689815 | 2006-11-01 11:00:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | SN1006 observation with XIS and HXD | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019050/ | Quick Look | ![]() |
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200 | FORNAX OFFSET3 | 55.0322 | -35.1579 | 54.552305 | -35.31846 | 39.454432 | -52.642961 | 236.21473388 | -53.30533318 | 63.6008 | 54664.1800810185 | 2008-07-17 04:19:19 | 54665.2009143518 | 2008-07-18 04:49:19 | 803008010 | 41.2795 | 30 | 41.2875 | 41.2795 | 0 | 41.2955 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0699 | 35.0699 | 88.1898 | 0 | PROCESSED | 57543.0818055556 | 2016-06-04 01:57:48 | 55055 | 2009-08-12 00:00:00 | 54689.4341087963 | 2008-08-11 10:25:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803008010/ | Quick Look | ![]() |
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201 | PERSEUS OFFSET-F | 49.9431 | 41.79 | 49.113812 | 41.609338 | 58.684902 | 22.607146 | 150.41345254 | -13.03211324 | 269.9991 | 55609.6649305556 | 2011-02-17 15:57:30 | 55610.152974537 | 2011-02-18 03:40:17 | 805046010 | 20.7197 | 25 | 20.7197 | 20.7197 | 0 | 20.7197 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.813 | 18.813 | 42.1599 | 0 | PROCESSED | 57600.9628125 | 2016-07-31 23:06:27 | 55990 | 2012-03-04 00:00:00 | 55621.2476967593 | 2011-03-01 05:56:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805046010/ | Quick Look | ![]() |
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202 | HESSJ1857-A | 284.2126 | 2.7519 | 283.584668 | 2.685017 | 285.744612 | 25.418977 | 35.99783049 | 0.0515802 | 269.8116 | 55822.9197800926 | 2011-09-18 22:04:29 | 55823.984212963 | 2011-09-19 23:37:16 | 506019010 | 40.9249 | 40 | 40.9249 | 40.9249 | 0 | 40.9249 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.8469 | 35.8469 | 91.9279 | 1 | PROCESSED | 57603.2046180556 | 2016-08-03 04:54:39 | 56233 | 2012-11-02 00:00:00 | 55865.2326157407 | 2011-10-31 05:34:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506019010/ | Quick Look | ![]() |
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203 | IC 443 | 94.2974 | 22.7535 | 93.540286 | 22.772525 | 93.964523 | -0.628288 | 188.8890151 | 3.10517693 | 91.6993 | 56197.2290277778 | 2012-09-27 05:29:48 | 56199.7780324074 | 2012-09-29 18:40:22 | 507015010 | 101.8023 | 400 | 101.8103 | 101.8023 | 0 | 101.8103 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.994 | 91.994 | 220.1877 | 0 | PROCESSED | 57607.2728472222 | 2016-08-07 06:32:54 | 56018 | 2012-04-01 00:00:00 | 56225.5965162037 | 2012-10-25 14:18:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015010/ | Quick Look | ![]() |
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204 | FERMI_BUBBLE_N4 | 233.8333 | 7.0797 | 233.2207 | 7.24518 | 229.504794 | 25.578453 | 13.3126084 | 46.30488493 | 287.5 | 56146.4387268518 | 2012-08-07 10:31:46 | 56146.9862615741 | 2012-08-07 23:40:13 | 507004010 | 20.9469 | 20 | 20.9509 | 20.9469 | 0 | 20.9549 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.7048 | 20.7048 | 47.306 | 2 | PROCESSED | 57606.7955787037 | 2016-08-06 19:05:38 | 56535 | 2013-08-31 00:00:00 | 56169.0484375 | 2012-08-30 01:09:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507004010/ | Quick Look | ![]() |
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205 | GC15 | 266.9617 | -29.4257 | 266.164223 | -29.409004 | 267.329759 | -6.012747 | 359.83382525 | -0.66952641 | 260.7835 | 54383.1536226852 | 2007-10-10 03:41:13 | 54383.6391666667 | 2007-10-10 15:20:24 | 502003010 | 21.4671 | 20 | 21.4751 | 21.4671 | 0 | 21.4751 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9225 | 18.9225 | 41.9439 | 0 | PROCESSED | 57540.2312731482 | 2016-06-01 05:33:02 | 54771 | 2008-11-01 00:00:00 | 54402.7485532407 | 2007-10-29 17:57:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502003010/ | Quick Look | ![]() |
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206 | VELA JR P2 | 132.1691 | -45.7748 | 131.740578 | -45.588644 | 157.998003 | -59.663034 | 265.4613949 | -1.31133586 | 347.0033 | 54285.6908217593 | 2007-07-04 16:34:47 | 54285.9036342593 | 2007-07-04 21:41:14 | 502024010 | 10.8502 | 10 | 10.8742 | 10.8662 | 0 | 10.8502 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6037 | 9.6037 | 18.3759 | 0 | PROCESSED | 57539.0914467593 | 2016-05-31 02:11:41 | 54696 | 2008-08-18 00:00:00 | 54328.4167361111 | 2007-08-16 10:00:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502024010/ | Quick Look | ![]() |
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207 | 1FGL J1715.2-3319 | 258.713 | -33.4282 | 257.892464 | -33.371742 | 260.432113 | -10.360749 | 352.62684601 | 3.01774525 | 99.0737 | 56002.5629166667 | 2012-03-16 13:30:36 | 56003.3750810185 | 2012-03-17 09:00:07 | 406024010 | 32.165 | 30 | 32.165 | 32.165 | 0 | 32.165 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.9848 | 27.9848 | 70.166 | 0 | PROCESSED | 57604.9296064815 | 2016-08-04 22:18:38 | 56386 | 2013-04-04 00:00:00 | 56019.2516435185 | 2012-04-02 06:02:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASANORI OHNO | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406024010/ | Quick Look | ![]() |
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208 | VELA JR P33 | 133.4681 | -47.1616 | 133.045488 | -46.970785 | 161.00407 | -60.345222 | 267.10091899 | -1.50393046 | 347.0007 | 54655.5652777778 | 2008-07-08 13:34:00 | 54656.0084837963 | 2008-07-09 00:12:13 | 503045010 | 12.0155 | 10 | 12.0155 | 12.0155 | 0 | 12.0155 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.0116 | 11.0116 | 38.2899 | 0 | PROCESSED | 57543.0047106482 | 2016-06-04 00:06:47 | 55048 | 2009-08-05 00:00:00 | 54679.4195601852 | 2008-08-01 10:04:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503045010/ | Quick Look | ![]() |
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209 | NGC 4382 | 186.3492 | 18.1851 | 185.718232 | 18.461926 | 178.313661 | 19.153245 | 267.72488674 | 79.23166289 | 294.1787 | 54638.1652199074 | 2008-06-21 03:57:55 | 54640.4481944444 | 2008-06-23 10:45:24 | 803005010 | 99.0682 | 90 | 99.0682 | 99.0682 | 0 | 99.0682 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.4447 | 93.4447 | 197.2038 | 3 | PROCESSED | 57542.911412037 | 2016-06-03 21:52:26 | 55020 | 2009-07-08 00:00:00 | 54651.2282291667 | 2008-07-04 05:28:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030033 | We proposeto observe a S0 galaxy, NGC 4382 for 90 ks with Suzaku. The purpose of the observation is to study abundance pattern of O/Ne/Mg/Si/Fe of S0 galaxies and to study history of S0 galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 3 | AO3 | THE ISM ABUNDANCE OF A S0 GALAXY, NGC 4382 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803005010/ | Quick Look | ![]() |
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210 | FORNAX A W-LOBE S | 50.3569 | -37.3111 | 49.879649 | -37.489667 | 32.298971 | -53.110795 | 240.40306132 | -56.92864271 | 79.0007 | 55065.4424189815 | 2009-08-22 10:37:05 | 55066.6731365741 | 2009-08-23 16:09:19 | 804038020 | 45.5693 | 42 | 45.5693 | 45.5693 | 0 | 45.5693 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 38.9534 | 38.9534 | 106.2599 | 0 | PROCESSED | 57548.3175347222 | 2016-06-09 07:37:15 | 55444 | 2010-09-05 00:00:00 | 55078.0721064815 | 2009-09-04 01:43:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MAKOTO TASHIRO | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804038020/ | Quick Look | ![]() |
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211 | 1RXSJ135341.1-664002 | 208.4233 | -66.67 | 207.481758 | -66.423993 | 237.082372 | -50.124321 | 309.05087215 | -4.54070575 | 288.5314 | 55774.1593055556 | 2011-08-01 03:49:24 | 55774.6939236111 | 2011-08-01 16:39:15 | 406036010 | 23.2679 | 20 | 23.2759 | 23.2679 | 0 | 23.2759 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.4241 | 22.4241 | 46.1839 | 0 | PROCESSED | 57602.7124189815 | 2016-08-02 17:05:53 | 56166 | 2012-08-27 00:00:00 | 55802.4628472222 | 2011-08-29 11:06:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMITSU TAKAHASHI | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406036010/ | Quick Look | ![]() |
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212 | THE MOON | 131.4647 | 12.9515 | 130.775529 | 13.134573 | 130.365878 | -4.869219 | 213.82172975 | 31.16197152 | 285.4003 | 56783.5475578704 | 2014-05-06 13:08:29 | 56783.6842361111 | 2014-05-06 16:25:18 | 809001010 | 4.6424 | 45 | 4.6464 | 4.6424 | 0 | 4.6504 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.5647 | 4.5647 | 11.806 | 0 | PROCESSED | 57615.0366898148 | 2016-08-15 00:52:50 | 57162 | 2015-05-20 00:00:00 | 56793.5228125 | 2014-05-16 12:32:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001010/ | Quick Look | ![]() |
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213 | FORNAX A HOST GALAXY | 50.6684 | -37.2029 | 50.191244 | -37.380302 | 32.749558 | -53.117138 | 240.15407206 | -56.69497357 | 218.3809 | 54091.6179976852 | 2006-12-22 14:49:55 | 54092.8689699074 | 2006-12-23 20:51:19 | 801015010 | 48.7217 | 50 | 48.7217 | 48.7217 | 0 | 48.7217 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3987 | 48.3987 | 108.0839 | 1 | PROCESSED | 57536.4184837963 | 2016-05-28 10:02:37 | 54735 | 2008-09-26 00:00:00 | 54132.9200347222 | 2007-02-01 22:04:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO TASHIRO | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801015010/ | Quick Look | ![]() |
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214 | EMS0857 | 198.1882 | 0.8497 | 197.548985 | 1.114667 | 196.443673 | 7.917565 | 314.828891 | 63.22804034 | 111.0249 | 55578.1935532407 | 2011-01-17 04:38:43 | 55578.746087963 | 2011-01-17 17:54:22 | 705011010 | 22.07 | 20 | 22.078 | 22.07 | 0 | 22.085 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.3267 | 15.3267 | 47.7279 | 0 | PROCESSED | 57600.6315046296 | 2016-07-31 15:09:22 | 55962 | 2012-02-05 00:00:00 | 55595.4732986111 | 2011-02-03 11:21:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705011010/ | Quick Look | ![]() |
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215 | 3C454.3 | 343.4951 | 16.1379 | 342.877484 | 15.871411 | 351.362437 | 21.321746 | 86.10833014 | -38.194784 | 252.9263 | 55525.0494675926 | 2010-11-25 01:11:14 | 55526.0141087963 | 2010-11-26 00:20:19 | 705021010 | 41.0252 | 40 | 41.0332 | 41.0332 | 0 | 41.0252 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1412 | 37.1412 | 83.3278 | 0 | PROCESSED | 57554.2391319445 | 2016-06-15 05:44:21 | 55916 | 2011-12-21 00:00:00 | 55550.1355439815 | 2010-12-20 03:15:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5-TOO | SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705021010/ | Quick Look | ![]() |
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216 | 3C390.3_VICINITY_1 | 276.9861 | 79.7253 | 277.865171 | 79.689308 | 84.608267 | 76.703493 | 111.37115096 | 27.70478895 | 240.0064 | 56607.4234953704 | 2013-11-11 10:09:50 | 56608.4910648148 | 2013-11-12 11:47:08 | 808046010 | 57.71 | 50 | 57.71 | 57.72 | 0 | 57.7141 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.9408 | 52.9408 | 92.2319 | 1 | PROCESSED | 57613.2938425926 | 2016-08-13 07:03:08 | 56991 | 2014-11-30 00:00:00 | 56625.6961458333 | 2013-11-29 16:42:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080060 | We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO SAKAI | JAP | 8 | AO8 | DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808046010/ | Quick Look | ![]() |
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217 | BULLET-BKG | 105.498 | -55.9182 | 105.253708 | -55.844379 | 132.076188 | -77.080913 | 266.15428465 | -20.7753384 | 287.5121 | 56422.4617592593 | 2013-05-10 11:04:56 | 56424.0029976852 | 2013-05-12 00:04:19 | 808057010 | 51.0907 | 50 | 51.0987 | 51.0907 | 0 | 51.1067 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6938 | 46.6938 | 133.1496 | 0 | PROCESSED | 57611.3081365741 | 2016-08-11 07:23:43 | 56799 | 2014-05-22 00:00:00 | 56433.6980208333 | 2013-05-21 16:45:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808057010/ | Quick Look | ![]() |
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218 | LMC X-2 | 80.025 | -71.9941 | 80.229686 | -72.041872 | 298.35324 | -83.539153 | 283.14092563 | -32.7117801 | 313.3022 | 53849.381712963 | 2006-04-24 09:09:40 | 53850.7731365741 | 2006-04-25 18:33:19 | 401012010 | 56.152 | 60 | 56.1657 | 56.1657 | 56.152 | 56.16 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 73.408 | 73.408 | 120.1938 | 1 | PROCESSED | 57533.5735300926 | 2016-05-25 13:45:53 | 54394 | 2007-10-21 00:00:00 | 53907.6288078704 | 2006-06-21 15:05:29 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMITSU TAKAHASHI | JAP | 1 | AO1 | DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401012010/ | Quick Look | ![]() |
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219 | NGC 2300 GROUP | 112.834 | 85.6974 | 108.693645 | 85.79613 | 93.629136 | 62.546385 | 127.72312729 | 27.79205873 | 339.9186 | 55237.1794907407 | 2010-02-10 04:18:28 | 55238.2502777778 | 2010-02-11 06:00:24 | 804030020 | 52.5611 | 100 | 52.5611 | 52.5611 | 0 | 52.5611 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.712 | 47.712 | 92.498 | 0 | PROCESSED | 57550.5807986111 | 2016-06-11 13:56:21 | 55633 | 2011-03-13 00:00:00 | 55266.3365625 | 2010-03-11 08:04:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804030020/ | Quick Look | ![]() |
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220 | NGC 7130 | 327.065 | -34.8962 | 326.317147 | -35.128916 | 317.224283 | -20.334869 | 10.02903365 | -50.33744977 | 78.4767 | 54597.5198726852 | 2008-05-11 12:28:37 | 54598.56625 | 2008-05-12 13:35:24 | 703012010 | 44.4931 | 40 | 44.4931 | 44.4931 | 0 | 44.4931 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36.7677 | 36.7677 | 90.3759 | 1 | PROCESSED | 57542.510474537 | 2016-06-03 12:15:05 | 54975 | 2009-05-24 00:00:00 | 54609.0170949074 | 2008-05-23 00:24:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 3 | AO3 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703012010/ | Quick Look | ![]() |
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221 | CYGNUS_LOOP_P10 | 311.5744 | 30.3992 | 311.055864 | 30.215413 | 325.67249 | 46.135207 | 73.13474548 | -7.93635975 | 240.0007 | 54417.2506944444 | 2007-11-13 06:01:00 | 54417.6043402778 | 2007-11-13 14:30:15 | 501020010 | 16.7958 | 10 | 16.7958 | 16.8198 | 0 | 16.8038 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6729 | 12.6729 | 30.5499 | 0 | PROCESSED | 57540.5008333333 | 2016-06-01 12:01:12 | 54798 | 2008-11-28 00:00:00 | 54430.1578472222 | 2007-11-26 03:47:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501020010/ | Quick Look | ![]() |
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222 | SWIFT J2052.0-5704 | 312.9788 | -57.0176 | 312.02055 | -57.205734 | 297.951069 | -37.67562 | 340.05945565 | -38.72742848 | 73.9304 | 54945.6280671296 | 2009-04-24 15:04:25 | 54946.6863310185 | 2009-04-25 16:28:19 | 704010010 | 45.16 | 40 | 45.16 | 45.168 | 0 | 45.168 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.6242 | 57.6242 | 91.4098 | 1 | PROCESSED | 57546.2560416667 | 2016-06-07 06:08:42 | 55339 | 2010-05-23 00:00:00 | 54973.4487152778 | 2009-05-22 10:46:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704010010/ | Quick Look | ![]() |
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223 | SWIFT J1952.4+0237 | 298.0556 | 2.5705 | 297.425623 | 2.440903 | 300.700434 | 23.070542 | 42.31566647 | -12.27488447 | 82.9116 | 54929.8284722222 | 2009-04-08 19:53:00 | 54931.1079166667 | 2009-04-10 02:35:24 | 704011010 | 47.9211 | 40 | 47.9259 | 47.9211 | 0 | 47.9259 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3044 | 39.3044 | 110.5258 | 2 | PROCESSED | 57546.1208680556 | 2016-06-07 02:54:03 | 55324 | 2010-05-08 00:00:00 | 54949.4878356482 | 2009-04-28 11:42:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704011010/ | Quick Look | ![]() |
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224 | CTB109 NOTHWEST | 345.2638 | 59.0349 | 344.742477 | 58.766045 | 23.94959 | 57.015916 | 109.14185824 | -0.84931137 | 252.0017 | 55908.2838078704 | 2011-12-13 06:48:41 | 55909.1988078704 | 2011-12-14 04:46:17 | 506037010 | 40.7488 | 40 | 40.7488 | 40.7568 | 0 | 40.7648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.201 | 39.201 | 79.044 | 0 | PROCESSED | 57604.1345601852 | 2016-08-04 03:13:46 | 56288 | 2012-12-27 00:00:00 | 55921.0397685185 | 2011-12-26 00:57:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506037010/ | Quick Look | ![]() |
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225 | NGC1365 | 53.4052 | -36.1452 | 52.927869 | -36.31215 | 36.804669 | -53.045157 | 237.96410536 | -54.59489483 | 47.2005 | 56107.1526041667 | 2012-06-29 03:39:45 | 56107.9972916667 | 2012-06-29 23:56:06 | 707017010 | 30.6949 | 30 | 30.6949 | 30.6949 | 0 | 30.6949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.8321 | 27.8321 | 72.9738 | 0 | PROCESSED | 57606.5279050926 | 2016-08-06 12:40:11 | 56491 | 2013-07-18 00:00:00 | 56125.2372453704 | 2012-07-17 05:41:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017010/ | Quick Look | ![]() |
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226 | NGC 3516 | 166.6957 | 72.5543 | 165.843141 | 72.824666 | 123.386475 | 57.973853 | 133.24670004 | 42.41457084 | 283.0856 | 56435.1473148148 | 2013-05-23 03:32:08 | 56436.2952199074 | 2013-05-24 07:05:07 | 708006070 | 51.4752 | 50 | 51.4772 | 51.4752 | 0 | 51.4792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.7203 | 53.7203 | 99.1658 | 1 | PROCESSED | 57611.3639351852 | 2016-08-11 08:44:04 | 56383 | 2013-04-01 00:00:00 | 56449.6609027778 | 2013-06-06 15:51:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006070/ | Quick Look | ![]() |
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227 | CTB109 SOUTHEAST | 345.764 | 58.7015 | 345.237296 | 58.43203 | 23.8569 | 56.597018 | 109.24155205 | -1.25930647 | 252.0022 | 55910.7526851852 | 2011-12-15 18:03:52 | 55911.4007638889 | 2011-12-16 09:37:06 | 506040010 | 30.4455 | 30 | 30.4455 | 30.4455 | 0 | 30.4455 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.7511 | 28.7511 | 55.9879 | 1 | PROCESSED | 57604.1444212963 | 2016-08-04 03:27:58 | 56289 | 2012-12-28 00:00:00 | 55922.0080555556 | 2011-12-27 00:11:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506040010/ | Quick Look | ![]() |
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228 | NGC 4968 | 196.7464 | -23.7282 | 196.071371 | -23.461103 | 204.633939 | -15.321329 | 307.51234678 | 39.00523278 | 298.8345 | 53954.7307523148 | 2006-08-07 17:32:17 | 53955.6822222222 | 2006-08-08 16:22:24 | 701005010 | 39.0508 | 40 | 39.0508 | 39.0508 | 39.0508 | 39.0508 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.617 | 35.617 | 82.1979 | 1 | PROCESSED | 57535.2527546296 | 2016-05-27 06:03:58 | 54408 | 2007-11-04 00:00:00 | 54020.7898148148 | 2006-10-12 18:57:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701005010/ | Quick Look | ![]() |
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229 | AM HERCULES | 274.126 | 49.8084 | 273.81383 | 49.78911 | 279.176537 | 73.11739 | 77.81082077 | 25.81903319 | 234.8814 | 54768.8590162037 | 2008-10-29 20:36:59 | 54771.3043287037 | 2008-11-01 07:18:14 | 403007010 | 108.4965 | 100 | 108.5045 | 108.5045 | 0 | 108.4965 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.4671 | 94.4671 | 211.2577 | 3 | PROCESSED | 57544.3392476852 | 2016-06-05 08:08:31 | 55156 | 2009-11-21 00:00:00 | 54788.4722222222 | 2008-11-18 11:20:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | JAP | 3 | AO3 | NON THERMAL EMISSION FROM THE POLAR AM HERCULES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403007010/ | Quick Look | ![]() |
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230 | HESS J1356-645 1 | 209.4297 | -64.5068 | 208.507718 | -64.263148 | 235.862386 | -48.071536 | 309.98959301 | -2.54712319 | 106.5083 | 56318.4192939815 | 2013-01-26 10:03:47 | 56320.0002083333 | 2013-01-28 00:00:18 | 507019010 | 55.7489 | 50 | 55.762 | 55.7569 | 0 | 55.7489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.1023 | 65.1023 | 136.5678 | 2 | PROCESSED | 57608.6328587963 | 2016-08-08 15:11:19 | 56708 | 2014-02-20 00:00:00 | 56342.6666319444 | 2013-02-19 15:59:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAHISA FUJINAGA | JAP | 7 | AO7 | OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507019010/ | Quick Look | ![]() |
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231 | A 2052 | 229.0471 | 6.9211 | 228.432118 | 7.104686 | 224.516271 | 24.128025 | 9.16646689 | 50.17566284 | 281.2031 | 53603.6121875 | 2005-08-21 14:41:33 | 53603.9938425926 | 2005-08-21 23:51:08 | 100006040 | 16.7443 | 20 | 16.7443 | 16.7443 | 16.7443 | 16.7443 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12.8395 | 12.8395 | 32.9519 | 0 | PROCESSED | 57520.7325810185 | 2016-05-12 17:34:55 | 53705 | 2005-12-01 00:00:00 | 53905.4634143518 | 2006-06-19 11:07:19 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Outer region of A 2052 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006040/ | Quick Look | ![]() |
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232 | ABELL 262 CENTER | 28.1922 | 36.1591 | 27.457024 | 35.91293 | 39.406526 | 22.931602 | 136.56609466 | -25.08359968 | 69.9979 | 54329.1761921296 | 2007-08-17 04:13:43 | 54330.0446643518 | 2007-08-18 01:04:19 | 802001010 | 37.1645 | 36 | 37.1645 | 37.1645 | 0 | 37.1645 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.1304 | 34.1304 | 75.0299 | 1 | PROCESSED | 57539.6070949074 | 2016-05-31 14:34:13 | 54730 | 2008-09-21 00:00:00 | 54350.5576851852 | 2007-09-07 13:23:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802001010/ | Quick Look | ![]() |
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233 | Crab Nebula | 83.5484 | 22.0881 | 82.795741 | 22.055005 | 84.024019 | -1.219032 | 184.45272098 | -5.81121698 | 85.0004 | 53614.9103009259 | 2005-09-01 21:50:50 | 53615.0418518518 | 2005-09-02 01:00:16 | 100015050 | 5.3447 | 5 | 5.3447 | 5.3447 | 5.3447 | 5.3447 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5.4859 | 5.4859 | 11.356 | 0 | PROCESSED | 57527.2511342593 | 2016-05-19 06:01:38 | 54247 | 2007-05-27 00:00:00 | 54109.1357986111 | 2007-01-09 03:15:33 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD boresight check with Crab | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015050/ | Quick Look | ![]() |
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234 | EP DRA | 286.7359 | 69.1573 | 286.793684 | 69.076999 | 30.014466 | 83.210835 | 100.08892772 | 23.87463538 | 44.5637 | 57164.4409953704 | 2015-05-22 10:35:02 | 57166.2856365741 | 2015-05-24 06:51:19 | 410006010 | 80.2346 | 80 | 80.2346 | 80.2426 | 0 | 80.2426 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.9585 | 67.9585 | 155.5819 | 1 | PROCESSED | 57618.7517939815 | 2016-08-18 18:02:35 | 57558 | 2016-06-19 00:00:00 | 57176.3159027778 | 2015-06-03 07:34:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100018 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI HAYASHI | JAP | 10 | AO10 | CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410006010/ | Quick Look | ![]() |
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235 | Cas A | 350.8254 | 58.8156 | 350.259841 | 58.54105 | 27.364711 | 54.864063 | 111.72292809 | -2.12474901 | 12.9937 | 53614.2486458333 | 2005-09-01 05:58:03 | 53614.7640509259 | 2005-09-01 18:20:14 | 100016010 | 27.965 | 20 | 27.973 | 27.973 | 27.973 | 27.965 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.13 | 24.13 | 44.4959 | 2 | PROCESSED | 57527.2832175926 | 2016-05-19 06:47:50 | 53705 | 2005-12-01 00:00:00 | 53905.4659606482 | 2006-06-19 11:10:59 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000016 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Cas A | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100016010/ | Quick Look | ![]() |
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236 | VW HYI | 62.2833 | -71.2901 | 62.373607 | -71.419454 | 322.048735 | -79.101508 | 284.88594452 | -38.13999051 | 181.9815 | 55894.1004513889 | 2011-11-29 02:24:39 | 55895.1821759259 | 2011-11-30 04:22:20 | 406009010 | 70.0834 | 60 | 70.0914 | 70.0834 | 0 | 70.0914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.9701 | 64.9701 | 93.4468 | 1 | PROCESSED | 57604.0242939815 | 2016-08-04 00:34:59 | 56274 | 2012-12-13 00:00:00 | 55907.1562615741 | 2011-12-12 03:45:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009010/ | Quick Look | ![]() |
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237 | H2356_VICINITY_A | 359.8969 | -30.2089 | 359.255002 | -30.487352 | 346.863445 | -27.454803 | 14.71906615 | -78.22459894 | 68.0006 | 55696.8464583333 | 2011-05-15 20:18:54 | 55698.0938773148 | 2011-05-17 02:15:11 | 506028010 | 52.1657 | 50 | 52.1657 | 52.1657 | 0 | 52.1657 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5791 | 46.5791 | 107.7539 | 1 | PROCESSED | 57602.0723148148 | 2016-08-02 01:44:08 | 56075 | 2012-05-28 00:00:00 | 55708.0697106482 | 2011-05-27 01:40:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 6 | AO6 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506028010/ | Quick Look | ![]() |
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238 | H2356_VICINITY_B | 359.9868 | -29.9493 | 359.345168 | -30.227755 | 347.07269 | -27.257526 | 15.89682365 | -78.35224854 | 69.5008 | 55698.0951388889 | 2011-05-17 02:17:00 | 55699.3474305556 | 2011-05-18 08:20:18 | 506029010 | 51.4072 | 50 | 51.4312 | 51.4232 | 0 | 51.4072 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.546 | 42.546 | 108.1559 | 1 | PROCESSED | 57602.0868402778 | 2016-08-02 02:05:03 | 56075 | 2012-05-28 00:00:00 | 55708.1035069444 | 2011-05-27 02:29:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 6 | AO6 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506029010/ | Quick Look | ![]() |
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239 | HESS_J1809-193_S | 272.3365 | -19.5311 | 271.597005 | -19.540657 | 272.197453 | 3.891828 | 10.84429394 | 0.04252392 | 106.4999 | 54557.6901851852 | 2008-04-01 16:33:52 | 54558.6161805556 | 2008-04-02 14:47:18 | 503079010 | 44.2481 | 40 | 44.2481 | 44.2481 | 0 | 44.2481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.2142 | 32.2142 | 79.9698 | 1 | PROCESSED | 57542.0277546296 | 2016-06-03 00:39:58 | 54950 | 2009-04-29 00:00:00 | 54570.1866666667 | 2008-04-14 04:28:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYASU ANADA | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503079010/ | Quick Look | ![]() |
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240 | CYG_BGD1 | 306.6527 | 39.4856 | 306.195949 | 39.320312 | 325.617981 | 56.073001 | 78.0015669 | 0.73572902 | 218.9004 | 56280.1666666667 | 2012-12-19 04:00:00 | 56280.6286458333 | 2012-12-19 15:05:15 | 507041010 | 26.9324 | 25 | 26.9404 | 26.9324 | 0 | 26.9404 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.4527 | 20.4527 | 39.9119 | 0 | PROCESSED | 57608.3151273148 | 2016-08-08 07:33:47 | 56683 | 2014-01-26 00:00:00 | 56316.5312268518 | 2013-01-24 12:44:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TSUNEFUMI MIZUNO | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507041010/ | Quick Look | ![]() |
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241 | A1689-OFFSET2 | 197.956 | -1.5158 | 197.313284 | -1.250483 | 197.134748 | 5.642151 | 313.46570539 | 60.93832198 | 289.9994 | 54671.3493518518 | 2008-07-24 08:23:04 | 54672.423125 | 2008-07-25 10:09:18 | 803025010 | 43.5468 | 40 | 43.5468 | 43.5468 | 0 | 43.5468 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.5486 | 36.5486 | 92.7159 | 2 | PROCESSED | 57543.1297685185 | 2016-06-04 03:06:52 | 55076 | 2009-09-02 00:00:00 | 54707.2585763889 | 2008-08-29 06:12:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803025010/ | Quick Look | ![]() |
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242 | A2061_1 | 229.9941 | 30.5295 | 229.479101 | 30.70939 | 216.056203 | 46.759039 | 47.89500096 | 57.43543483 | 120.6365 | 56306.3817939815 | 2013-01-14 09:09:47 | 56307.4847800926 | 2013-01-15 11:38:05 | 807029010 | 42.2923 | 40 | 42.3006 | 42.2991 | 0 | 42.2923 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.1838 | 38.1838 | 95.294 | 0 | PROCESSED | 57608.511087963 | 2016-08-08 12:15:58 | 56703 | 2014-02-15 00:00:00 | 56337.5472222222 | 2013-02-14 13:08:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070070 | We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO OKABE | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807029010/ | Quick Look | ![]() |
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243 | 3C 236 BACKGROUND | 151.1488 | 34.7362 | 150.413548 | 34.979134 | 140.636655 | 21.408004 | 190.35215815 | 53.68789407 | 299.9977 | 56055.786712963 | 2012-05-08 18:52:52 | 56056.7919444444 | 2012-05-09 19:00:24 | 707006010 | 46.2113 | 40 | 46.2113 | 46.2113 | 0 | 46.2113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1095 | 44.1095 | 86.8399 | 0 | PROCESSED | 57605.3836574074 | 2016-08-05 09:12:28 | 56436 | 2013-05-24 00:00:00 | 56070.1639930556 | 2012-05-23 03:56:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 7 | AO7 | INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707006010/ | Quick Look | ![]() |
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244 | NEP | 272.7884 | 65.9814 | 272.771336 | 65.967881 | 333.879188 | 88.742697 | 95.75202722 | 28.67554678 | 290.9299 | 53615.6136921296 | 2005-09-02 14:43:43 | 53617.625162037 | 2005-09-04 15:00:14 | 100018010 | 106.2015 | 100 | 106.2015 | 106.2175 | 106.2495 | 106.2255 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 106.125 | 106.125 | 173.5718 | 3 | PROCESSED | 57527.2880092593 | 2016-05-19 06:54:44 | 53705 | 2005-12-01 00:00:00 | 53905.4636921296 | 2006-06-19 11:07:43 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000018 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD background at North Ecliptic Pole | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100018010/ | Quick Look | ![]() |
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245 | BULLET-OFFSET1 | 104.8831 | -55.8434 | 104.638861 | -55.772465 | 130.550899 | -77.176368 | 265.96507608 | -21.0808269 | 287.0003 | 56416.3315277778 | 2013-05-04 07:57:24 | 56419.0787037037 | 2013-05-07 01:53:20 | 808055010 | 102.9172 | 100 | 102.9412 | 102.9172 | 0 | 102.9412 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.4395 | 93.4395 | 237.3167 | 4 | PROCESSED | 57611.2833564815 | 2016-08-11 06:48:02 | 56795 | 2014-05-18 00:00:00 | 56429.7533101852 | 2013-05-17 18:04:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808055010/ | Quick Look | ![]() |
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246 | JUPITER | 103.8407 | 23.1129 | 103.084394 | 23.177707 | 102.712362 | 0.280692 | 192.5219391 | 11.12856775 | 264.3937 | 56762.3891782407 | 2014-04-15 09:20:25 | 56762.7223611111 | 2014-04-15 17:20:12 | 508023020 | 15.4083 | 160 | 15.4083 | 15.4083 | 0 | 15.4083 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.2744 | 12.2744 | 28.7839 | 1 | PROCESSED | 57614.2553819445 | 2016-08-14 06:07:45 | 57212 | 2015-07-09 00:00:00 | 56778.6154166667 | 2014-05-01 14:46:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023020/ | Quick Look | ![]() |
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247 | Crab Nebula | 83.6274 | 22.0192 | 82.875108 | 21.986487 | 84.094124 | -1.29112 | 184.55062413 | -5.78629385 | 86.8663 | 53604.1571412037 | 2005-08-22 03:46:17 | 53604.2501273148 | 2005-08-22 06:00:11 | 100007010 | 1.7229 | 5 | 1.7229 | 1.7229 | 1.7229 | 1.7229 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.808 | 1.808 | 8.034 | 0 | PROCESSED | 57520.7330324074 | 2016-05-12 17:35:34 | 54247 | 2007-05-27 00:00:00 | 54105.2758912037 | 2007-01-05 06:37:17 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Nebula | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007010/ | Quick Look | ![]() |
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248 | Crab nebula | 83.6201 | 22.1854 | 82.866876 | 22.152649 | 84.094711 | -1.124779 | 184.40591259 | -5.70300776 | 86.8631 | 53604.2507175926 | 2005-08-22 06:01:02 | 53604.3889351852 | 2005-08-22 09:20:04 | 100007020 | 3.0531 | 5 | 3.0571 | 3.0531 | 3.0531 | 3.0531 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.1343 | 3.1343 | 11.94 | 1 | PROCESSED | 57520.7416782407 | 2016-05-12 17:48:01 | 54247 | 2007-05-27 00:00:00 | 54105.2987268518 | 2007-01-05 07:10:10 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Nebula | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007020/ | Quick Look | ![]() |
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249 | Crab nebula | 83.4512 | 22.0082 | 82.699013 | 21.974637 | 83.930395 | -1.294795 | 184.47195778 | -5.93010486 | 86.7989 | 53604.489849537 | 2005-08-22 11:45:23 | 53604.5835416667 | 2005-08-22 14:00:18 | 100007040 | 4.2682 | 5 | 4.2682 | 4.2682 | 4.2682 | 4.2682 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4.1392 | 4.1392 | 8.056 | 0 | PROCESSED | 57520.7454513889 | 2016-05-12 17:53:27 | 54247 | 2007-05-27 00:00:00 | 54105.3073726852 | 2007-01-05 07:22:37 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Nebula | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007040/ | Quick Look | ![]() |
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250 | NGC 4945 | 196.3733 | -49.4666 | 195.643253 | -49.198924 | 217.025297 | -38.636782 | 305.27803835 | 13.34111135 | 313.9078 | 53605.101087963 | 2005-08-23 02:25:34 | 53605.1034490741 | 2005-08-23 02:28:58 | 100008020 | 0.1776 | 10 | 0.1815 | 0.1815 | 0.1796 | 0.1776 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 0.2001 | 0.2001 | 0.202 | 0 | PROCESSED | 57526.8486574074 | 2016-05-18 20:22:04 | 54247 | 2007-05-27 00:00:00 | 54034.6891435185 | 2006-10-26 16:32:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000008 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | NGC 4945 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100008020/ | Quick Look | ![]() |
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251 | CYG X-1 | 299.5907 | 35.1892 | 299.120596 | 35.052727 | 313.656273 | 54.237702 | 71.32454904 | 3.06010347 | 276.9898 | 53648.2025347222 | 2005-10-05 04:51:39 | 53648.6335532407 | 2005-10-05 15:12:19 | 100036010 | 18.213 | 20 | 18.213 | 18.213 | 18.213 | 18.213 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18.1457 | 18.1457 | 37.2299 | 0 | PROCESSED | 57527.5598726852 | 2016-05-19 13:26:13 | 54247 | 2007-05-27 00:00:00 | 54037.7278819444 | 2006-10-29 17:28:09 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Cyg X-1 in the low state | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100036010/ | Quick Look | ![]() |
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252 | Sgr_B2 | 266.8775 | -28.4435 | 266.086257 | -28.426412 | 267.234561 | -5.032377 | 0.63628385 | -0.09835114 | 265.3727 | 53653.5194560185 | 2005-10-10 12:28:01 | 53655.2954050926 | 2005-10-12 07:05:23 | 100037060 | 76.5966 | 100 | 76.6286 | 76.6446 | 76.5966 | 76.6286 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.8192 | 70.8192 | 153.4319 | 0 | PROCESSED | 57527.5776041667 | 2016-05-19 13:51:45 | 54247 | 2007-05-27 00:00:00 | 54036.2262731482 | 2006-10-28 05:25:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037060/ | Quick Look | ![]() |
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253 | Sgr_B2_BGD | 267.0943 | -28.1356 | 266.304946 | -28.119568 | 267.419629 | -4.720546 | 0.99854005 | -0.10262599 | 269.0208 | 53655.2988888889 | 2005-10-12 07:10:24 | 53655.4620833333 | 2005-10-12 11:05:24 | 100037070 | 9.1612 | 10 | 9.1612 | 9.1643 | 9.1643 | 9.1632 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.5364 | 9.5364 | 14.092 | 0 | PROCESSED | 57527.5688078704 | 2016-05-19 13:39:05 | 54247 | 2007-05-27 00:00:00 | 54036.0749884259 | 2006-10-28 01:47:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037070/ | Quick Look | ![]() |
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254 | MKN 3 | 93.8839 | 71.0477 | 92.433649 | 71.063052 | 91.875357 | 47.63268 | 143.2836301 | 22.71631463 | 71.8326 | 53665.0848263889 | 2005-10-22 02:02:09 | 53667.2682175926 | 2005-10-24 06:26:14 | 100040010 | 95.0265 | 100 | 95.0265 | 95.0772 | 95.0452 | 95.0345 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 91.3441 | 91.3441 | 188.6299 | 0 | PROCESSED | 57527.6643055556 | 2016-05-19 15:56:36 | 54247 | 2007-05-27 00:00:00 | 53906.4896759259 | 2006-06-20 11:45:08 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | MKN 3 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100040010/ | Quick Look | ![]() |
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255 | RXJ1856.5-3754 | 284.1498 | -37.9103 | 283.298136 | -37.976359 | 281.509901 | -15.033652 | 358.59888263 | -17.21635309 | 269.4259 | 53667.2829976852 | 2005-10-24 06:47:31 | 53669.4793287037 | 2005-10-26 11:30:14 | 100041010 | 76.2548 | 80 | 0 | 76.2548 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 62.6217 | 62.6217 | 189.72 | 3 | PROCESSED | 57527.6811111111 | 2016-05-19 16:20:48 | 54247 | 2007-05-27 00:00:00 | 54037.2294791667 | 2006-10-29 05:30:27 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | LOW ENERGY QE CALIBRATION OF XIS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100041010/ | Quick Look | ![]() |
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256 | RXJ1713-3946_ID3 | 258.1658 | -40.0306 | 257.296734 | -39.971421 | 260.540524 | -16.976597 | 347.01547145 | -0.49239611 | 87.0009 | 55244.1262847222 | 2010-02-17 03:01:51 | 55244.4779398148 | 2010-02-17 11:28:14 | 504029010 | 20.8716 | 20 | 20.9036 | 20.9036 | 0 | 20.8716 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.8868 | 20.8868 | 30.3759 | 0 | PROCESSED | 57550.6116087963 | 2016-06-11 14:40:43 | 55622 | 2011-03-02 00:00:00 | 55256.0720601852 | 2010-03-01 01:43:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504029010/ | Quick Look | ![]() |
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257 | G11.2-0.3 | 272.8676 | 19.433 | 272.324919 | 19.420376 | 273.677117 | 42.836704 | 46.34586116 | 17.29738119 | 77.6432 | 53834.4626041667 | 2006-04-09 11:06:09 | 53835.6634143518 | 2006-04-10 15:55:19 | 401010010 | 43.9846 | 50 | 43.9926 | 43.9846 | 43.9926 | 43.9926 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.3879 | 37.3879 | 83.6799 | 1 | PROCESSED | 57533.4279166667 | 2016-05-25 10:16:12 | 54397 | 2007-10-24 00:00:00 | 53905.4671875 | 2006-06-19 11:12:45 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ASAMI HAYATO | JAP | 1 | AO1 | CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401010010/ | Quick Look | ![]() |
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258 | PSR B1259-63 | 195.6732 | -63.8823 | 194.883764 | -63.613652 | 227.720536 | -50.935927 | 304.17036556 | -1.03761834 | 285.8945 | 54294.6568865741 | 2007-07-13 15:45:55 | 54295.3459953704 | 2007-07-14 08:18:14 | 402014040 | 22.9149 | 20 | 22.9149 | 22.9149 | 0 | 22.9149 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0706 | 21.0706 | 59.4959 | 1 | PROCESSED | 57539.2651273148 | 2016-05-31 06:21:47 | 54709 | 2008-08-31 00:00:00 | 54339.4142592593 | 2007-08-27 09:56:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014040/ | Quick Look | ![]() |
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259 | HOT BLOB 2 | 131.2547 | 53.3234 | 130.330211 | 53.505247 | 118.317658 | 33.861433 | 164.89716269 | 38.20704104 | 284.8982 | 57137.3573842593 | 2015-04-25 08:34:38 | 57139.1293055556 | 2015-04-27 03:06:12 | 509008010 | 46.0224 | 80 | 46.0224 | 77.9795 | 0 | 78.0115 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.041412037 | 2016-08-18 00:59:38 | 57520 | 2016-05-12 00:00:00 | 57154.4516087963 | 2015-05-12 10:50:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090044 | Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIO SEKIYA | JAP | 9 | AO9 | ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509008010/ | Quick Look | ![]() |
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260 | IC 443 | 94.3028 | 22.7465 | 93.545727 | 22.765551 | 93.96971 | -0.635136 | 188.89754986 | 3.10625906 | 259.0005 | 56378.1771527778 | 2013-03-27 04:15:06 | 56379.6668865741 | 2013-03-28 16:00:19 | 507015020 | 59.2712 | 300 | 59.2712 | 59.2712 | 0 | 59.2712 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.2705 | 51.2705 | 128.6878 | 3 | PROCESSED | 57610.9601388889 | 2016-08-10 23:02:36 | 56018 | 2012-04-01 00:00:00 | 56391.749224537 | 2013-04-09 17:58:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015020/ | Quick Look | ![]() |
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261 | MARS-P1 | 102.8773 | 25.1625 | 102.108873 | 25.222717 | 101.648232 | 2.240772 | 190.24974394 | 11.19384085 | 298.0037 | 54559.3414814815 | 2008-04-03 08:11:44 | 54559.4099421296 | 2008-04-03 09:50:19 | 403006010 | 2.9048 | 100 | 2.9048 | 2.9128 | 0 | 2.9128 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.9096 | 2.9096 | 5.9119 | 0 | PROCESSED | 57542.0343981482 | 2016-06-03 00:49:32 | 54953 | 2009-05-02 00:00:00 | 54577.0446875 | 2008-04-21 01:04:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006010/ | Quick Look | ![]() |
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262 | MARS-P4 | 103.0016 | 25.1536 | 102.233284 | 25.214407 | 101.761173 | 2.241936 | 190.30618657 | 11.29219101 | 298.0476 | 54559.5767592593 | 2008-04-03 13:50:32 | 54559.6599421296 | 2008-04-03 15:50:19 | 403006040 | 2.2882 | 100 | 2.2882 | 2.2882 | 0 | 2.2882 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.01 | 2.01 | 7.1839 | 0 | PROCESSED | 57542.0411226852 | 2016-06-03 00:59:13 | 54953 | 2009-05-02 00:00:00 | 54577.0528935185 | 2008-04-21 01:16:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006040/ | Quick Look | ![]() |
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263 | MARS-P15 | 103.4611 | 25.1019 | 102.69331 | 25.164885 | 102.180485 | 2.228357 | 190.53184536 | 11.64832678 | 298.2083 | 54560.4934375 | 2008-04-04 11:50:33 | 54560.5766666667 | 2008-04-04 13:50:24 | 403006150 | 3.831 | 100 | 3.839 | 3.831 | 0 | 3.847 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.1928 | 3.1928 | 7.1839 | 1 | PROCESSED | 57542.0622222222 | 2016-06-03 01:29:36 | 54953 | 2009-05-02 00:00:00 | 54580.5809837963 | 2008-04-24 13:56:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006150/ | Quick Look | ![]() |
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264 | AM HERCULES BGD | 282.0964 | 47.9785 | 281.757583 | 47.920958 | 294.678535 | 70.385314 | 77.40285415 | 20.2844947 | 234.9986 | 54771.3072106482 | 2008-11-01 07:22:23 | 54772.3438310185 | 2008-11-02 08:15:07 | 403008010 | 44.3601 | 40 | 44.3681 | 44.3601 | 0 | 44.3921 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.4115 | 40.4115 | 89.5519 | 1 | PROCESSED | 57544.3170833333 | 2016-06-05 07:36:36 | 55154 | 2009-11-19 00:00:00 | 54788.4288541667 | 2008-11-18 10:17:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | JAP | 3 | AO3 | NON THERMAL EMISSION FROM THE POLAR AM HERCULES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403008010/ | Quick Look | ![]() |
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265 | RXJ0007.0+7302 | 1.8916 | 72.9843 | 1.226338 | 72.706084 | 53.083805 | 60.867639 | 119.68700382 | 10.38954096 | 241.7328 | 55204.6112847222 | 2010-01-08 14:40:15 | 55207.0675231482 | 2010-01-11 01:37:14 | 404011010 | 105.3739 | 100 | 105.3739 | 105.3739 | 0 | 106.9714 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 58.5644 | 58.5644 | 212.2059 | 2 | PROCESSED | 57550.1958564815 | 2016-06-11 04:42:02 | 55587 | 2011-01-26 00:00:00 | 55768.9633333333 | 2011-07-26 23:07:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUMPEI TAKATA | JAP | 4 | AO4 | X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404011010/ | Quick Look | ![]() |
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266 | FO AQR | 334.4646 | -8.2931 | 333.805898 | -8.543636 | 333.309968 | 2.14088 | 53.06192299 | -49.11309098 | 76.4186 | 54987.3437152778 | 2009-06-05 08:14:57 | 54988.5536921296 | 2009-06-06 13:17:19 | 404032010 | 46.0846 | 40 | 46.0846 | 46.0846 | 0 | 46.0846 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.4993 | 33.4993 | 104.5299 | 0 | PROCESSED | 57547.5153356482 | 2016-06-08 12:22:05 | 55366 | 2010-06-19 00:00:00 | 54998.3271064815 | 2009-06-16 07:51:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404032010/ | Quick Look | ![]() |
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267 | LOW_LATITUDE_97-10 | 311.8076 | 60.1112 | 311.52726 | 59.92615 | 0.701483 | 70.601802 | 96.61384914 | 10.40907029 | 101.0346 | 54571.1324652778 | 2008-04-15 03:10:45 | 54572.8890509259 | 2008-04-16 21:20:14 | 503075010 | 79.8119 | 80 | 79.8199 | 79.8279 | 0 | 79.8119 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.8105 | 80.8105 | 151.7498 | 2 | PROCESSED | 57542.342962963 | 2016-06-03 08:13:52 | 54953 | 2009-05-02 00:00:00 | 54581.3271643518 | 2008-04-25 07:51:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOMOTAKA YOSHINO | JAP | 3 | AO3 | RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503075010/ | Quick Look | ![]() |
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268 | IGR J15094-6649 | 227.3484 | -66.8278 | 226.235673 | -66.63712 | 247.091848 | -46.74399 | 315.91945149 | -7.50109233 | 90.4626 | 55588.7031365741 | 2011-01-27 16:52:31 | 55589.5557638889 | 2011-01-28 13:20:18 | 405007010 | 49.4612 | 50 | 49.4832 | 49.4752 | 0 | 49.4612 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.0185 | 48.0185 | 73.6599 | 0 | PROCESSED | 57600.7830092593 | 2016-07-31 18:47:32 | 55990 | 2012-03-04 00:00:00 | 55621.2282291667 | 2011-03-01 05:28:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 5 | AO5 | ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405007010/ | Quick Look | ![]() |
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269 | A2163NW | 243.7926 | -5.9349 | 243.126237 | -5.810502 | 242.931845 | 15.076918 | 6.85972512 | 30.71314923 | 93.93 | 57075.8011574074 | 2015-02-22 19:13:40 | 57077.0558333333 | 2015-02-24 01:20:24 | 809008010 | 48.0634 | 50 | 48.0634 | 49.7339 | 0 | 49.7194 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6490046296 | 2016-08-17 15:34:34 | 57454 | 2016-03-07 00:00:00 | 57087.4664467593 | 2015-03-06 11:11:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809008010/ | Quick Look | ![]() |
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270 | XSS J16537-1905 | 253.8855 | -18.1447 | 253.157456 | -18.065723 | 254.650655 | 4.44189 | 2.56699105 | 15.52634316 | 96.7569 | 55602.7046412037 | 2011-02-10 16:54:41 | 55603.1488657407 | 2011-02-11 03:34:22 | 405032010 | 20.0243 | 20 | 20.0323 | 20.0403 | 0 | 20.0243 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.1528 | 18.1528 | 38.3439 | 0 | PROCESSED | 57600.887337963 | 2016-07-31 21:17:46 | 55983 | 2012-02-26 00:00:00 | 55617.4104282407 | 2011-02-25 09:51:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405032010/ | Quick Look | ![]() |
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271 | VW HYI | 62.3086 | -71.2914 | 62.399129 | -71.420645 | 322.033067 | -79.109175 | 284.88209314 | -38.1323503 | 276.4367 | 55986.5687962963 | 2012-02-29 13:39:04 | 55987.2501273148 | 2012-03-01 06:00:11 | 406009030 | 20.1097 | 20 | 20.1097 | 20.1097 | 0 | 20.1097 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.5712 | 20.5712 | 58.8579 | 1 | PROCESSED | 57604.7590972222 | 2016-08-04 18:13:06 | 56385 | 2013-04-03 00:00:00 | 56018.9417824074 | 2012-04-01 22:36:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009030/ | Quick Look | ![]() |
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272 | AQL X-1 | 287.8264 | 0.5741 | 287.188103 | 0.49034 | 289.387425 | 22.822835 | 35.71314195 | -4.15661165 | 244.5268 | 55855.5357986111 | 2011-10-21 12:51:33 | 55856.4599884259 | 2011-10-22 11:02:23 | 406010020 | 9.9406 | 40 | 10.041 | 9.9406 | 0 | 10.041 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37.8451 | 37.8451 | 79.846 | 1 | PROCESSED | 57603.5073958333 | 2016-08-03 12:10:39 | 56241 | 2012-11-10 00:00:00 | 55873.3025578704 | 2011-11-08 07:15:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUTAKA YAMAOKA | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010020/ | Quick Look | ![]() |
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273 | 4U0114+65 | 19.4873 | 65.3067 | 18.650038 | 65.043652 | 51.171478 | 51.093575 | 125.69846298 | 2.57745686 | 71.642 | 55763.4307291667 | 2011-07-21 10:20:15 | 55764.9453472222 | 2011-07-22 22:41:18 | 406017010 | 106.4925 | 100 | 106.5508 | 106.5588 | 0 | 106.4925 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.5061 | 88.5061 | 130.8219 | 1 | PROCESSED | 57602.6518402778 | 2016-08-02 15:38:39 | 56152 | 2012-08-13 00:00:00 | 55785.0443981482 | 2011-08-12 01:03:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO SASANO | JAP | 6 | AO6 | SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406017010/ | Quick Look | ![]() |
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274 | EUVE J1439 +75.0 | 219.9459 | 75.0823 | 219.98134 | 75.295606 | 130.308915 | 72.229429 | 114.11249059 | 40.13551871 | 340.4897 | 56067.2884722222 | 2012-05-20 06:55:24 | 56067.8599421296 | 2012-05-20 20:38:19 | 407039010 | 29.9613 | 40 | 29.9693 | 29.9693 | 0 | 29.9613 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32.3932 | 32.3932 | 49.3439 | 0 | PROCESSED | 57605.4757523148 | 2016-08-05 11:25:05 | 56442 | 2013-05-30 00:00:00 | 56076.028912037 | 2012-05-29 00:41:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ATSUSHI HARAYAMA | JAP | 7 | AO7 | SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407039010/ | Quick Look | ![]() |
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275 | CRAB PULSAR | 83.6302 | 22.0185 | 82.877911 | 21.9858 | 84.096687 | -1.291934 | 184.55261516 | -5.78447613 | 87.4628 | 56551.703599537 | 2013-09-16 16:53:11 | 56552.187650463 | 2013-09-17 04:30:13 | 408008010 | 0.2483 | 20 | 0.2483 | 0.2483 | 0 | 0.2483 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.312 | 16.312 | 41.8179 | 1 | PROCESSED | 57612.6349421296 | 2016-08-12 15:14:19 | 56956 | 2014-10-26 00:00:00 | 56588.603599537 | 2013-10-23 14:29:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080026 | We hereby submit a proposal for Suzaku/HXD observations of the Crab pulsar' hard X-ray pulses, which will be coordinated with simultaneous detection of giant radio pulses at ground radio telescopes. With these observations, we will get a statistically significant confirmation (or denial) of the existence of correlation between X-ray intensity and giant radio pulses, which has been found, with a marginal significance, during our trial observations of the Crab pulsar in which we utilized the calibration data of the HXD. If this correlation is confirmed, a new insight into the physics of pulsars' magnetospheres can be obtained. | GALACTIC POINT SOURCES | 4 | C | TOSHIO TERASAWA | JAP | 8 | AO8 | CORRELATION STUDY OF X-RAY PULSES AND GIANT RADIO PULSES FROM CRAB PULSAR WITH SUZAKU/HXD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408008010/ | Quick Look | ![]() |
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276 | ETA CARINAE | 161.2758 | -59.6779 | 160.789133 | -59.414544 | 202.149273 | -58.913486 | 287.59865979 | -0.62113788 | 295.3343 | 56479.0480439815 | 2013-07-06 01:09:11 | 56481.2890509259 | 2013-07-08 06:56:14 | 408018020 | 83.9685 | 180 | 83.9685 | 83.9685 | 0 | 83.9685 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.7786 | 75.7786 | 193.6058 | 3 | PROCESSED | 57611.7548263889 | 2016-08-11 18:06:57 | 56861 | 2014-07-23 00:00:00 | 56492.6867361111 | 2013-07-19 16:28:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080081 | Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms. | GALACTIC POINT SOURCES | 4 | B | TAKAYUKI YUASA | JAP | 8 | AO8 | DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018020/ | Quick Look | ![]() |
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277 | 1RXSJ174559.6-370055 | 266.4961 | -37.0139 | 265.645982 | -36.994815 | 267.112271 | -13.607714 | 353.13065719 | -4.26083799 | 95.2535 | 57115.2722106482 | 2015-04-03 06:31:59 | 57115.6653240741 | 2015-04-03 15:58:04 | 409017010 | 14.2473 | 15 | 14.2473 | 14.2473 | 0 | 14.2633 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9002777778 | 2016-08-17 21:36:24 | 57493 | 2016-04-15 00:00:00 | 57126.4170949074 | 2015-04-14 10:00:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 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 | B | HIDEYUKI MORI | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409017010/ | Quick Look | ![]() |
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278 | GK PER | 52.7957 | 43.9123 | 51.943474 | 43.742358 | 61.502929 | 24.084705 | 150.94865814 | -10.09942696 | 88.9617 | 56876.7092708333 | 2014-08-07 17:01:21 | 56879.871712963 | 2014-08-10 20:55:16 | 409018010 | 109.7612 | 140 | 109.7612 | 114.4242 | 0 | 114.4722 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4851157407 | 2016-08-16 11:38:34 | 57468 | 2016-03-21 00:00:00 | 56902.7320023148 | 2014-09-02 17:34:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090055 | A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI YUASA | JAP | 9 | AO9 | CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409018010/ | Quick Look | ![]() |
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279 | IC 443 | 94.2972 | 22.4797 | 93.541644 | 22.498727 | 93.972502 | -0.901975 | 189.13057055 | 2.97563306 | 274.0001 | 54166.5158680556 | 2007-03-07 12:22:51 | 54167.612025463 | 2007-03-08 14:41:19 | 501006020 | 44.0135 | 40 | 44.0135 | 44.0375 | 0 | 44.0215 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.3209 | 36.3209 | 94.6999 | 1 | PROCESSED | 57537.6255324074 | 2016-05-29 15:00:46 | 54736 | 2008-09-27 00:00:00 | 54172.2247800926 | 2007-03-13 05:23:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASANOBU OZAKI | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006020/ | Quick Look | ![]() |
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280 | 1RXJ0603 OFFSET | 92.2783 | 42.2687 | 91.384795 | 42.277603 | 91.783385 | 18.842189 | 170.6889541 | 10.70559867 | 80.0991 | 56214.8308564815 | 2012-10-14 19:56:26 | 56215.5314236111 | 2012-10-15 12:45:15 | 807002010 | 26.8334 | 30 | 26.8334 | 26.8574 | 0 | 26.8414 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.3531 | 28.3531 | 60.5159 | 1 | PROCESSED | 57607.7719907407 | 2016-08-07 18:31:40 | 56690 | 2014-02-02 00:00:00 | 56323.4936574074 | 2013-01-31 11:50:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070025 | We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HIROKI AKAMATSU | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807002010/ | Quick Look | ![]() |
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281 | CENA LOBE BGD1 | 205.3783 | -39.3349 | 204.641576 | -39.082547 | 218.514411 | -26.72025 | 313.38854271 | 22.51794697 | 286.0001 | 56122.4603125 | 2012-07-14 11:02:51 | 56123.1043634259 | 2012-07-15 02:30:17 | 807042010 | 22.2455 | 20 | 22.2455 | 22.2455 | 0 | 22.2455 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8556 | 18.8556 | 55.616 | 1 | PROCESSED | 57606.6151157407 | 2016-08-06 14:45:46 | 56018 | 2012-04-01 00:00:00 | 56142.2381597222 | 2012-08-03 05:42:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807042010/ | Quick Look | ![]() |
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282 | SN1006 NE BG | 226.7036 | -41.3998 | 225.886024 | -41.207391 | 236.037501 | -22.925171 | 328.51405135 | 14.65073262 | 293.6503 | 53617.7018865741 | 2005-09-04 16:50:43 | 53622.1668287037 | 2005-09-09 04:00:14 | 100019010 | 44.7503 | 50 | 44.7543 | 44.7543 | 44.7543 | 44.7503 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.3883 | 37.3883 | 385.6018 | 5 | PROCESSED | 57527.2923148148 | 2016-05-19 07:00:56 | 54247 | 2007-05-27 00:00:00 | 54035.4224768518 | 2006-10-27 10:08:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | SN1006 observation with XIS and HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019010/ | Quick Look | ![]() |
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283 | VICINITY OF LMC X-3 | 83.4844 | -63.8863 | 83.408578 | -63.918105 | 41.435206 | -86.187449 | 273.3865557 | -32.64248934 | 284.6189 | 53811.6008333333 | 2006-03-17 14:25:12 | 53813.9168055556 | 2006-03-19 22:00:12 | 500031010 | 82.0185 | 80 | 82.0265 | 82.0185 | 82.0265 | 82.0265 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74.6148 | 74.6148 | 200.0639 | 2 | PROCESSED | 57533.2849537037 | 2016-05-25 06:50:20 | 54247 | 2007-05-27 00:00:00 | 54056.4806828704 | 2006-11-17 11:32:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | VICINITY OF LMC X-3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500031010/ | Quick Look | ![]() |
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284 | IC 443 | 94.2975 | 22.7757 | 93.54026 | 22.794725 | 93.963954 | -0.606095 | 188.8694635 | 3.11574616 | 274.0004 | 54165.4446643518 | 2007-03-06 10:40:19 | 54166.5154398148 | 2007-03-07 12:22:14 | 501006010 | 42.0113 | 40 | 42.0113 | 42.0129 | 0 | 42.0209 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6934 | 34.6934 | 92.5099 | 2 | PROCESSED | 57537.6197337963 | 2016-05-29 14:52:25 | 54736 | 2008-09-27 00:00:00 | 54174.6613541667 | 2007-03-15 15:52:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASANOBU OZAKI | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006010/ | Quick Look | ![]() |
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285 | CYGNUS_LOOP_P1 | 313.519 | 31.9657 | 313.004288 | 31.774919 | 328.788742 | 46.92673 | 75.41990185 | -8.25713566 | 240 | 54417.6059259259 | 2007-11-13 14:32:32 | 54418.0904976852 | 2007-11-14 02:10:19 | 501012010 | 16.7385 | 10 | 16.7385 | 16.7489 | 0 | 16.7425 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.7758 | 15.7758 | 41.86 | 1 | PROCESSED | 57540.5110648148 | 2016-06-01 12:15:56 | 54798 | 2008-11-28 00:00:00 | 54430.2159375 | 2007-11-26 05:10:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501012010/ | Quick Look | ![]() |
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286 | CYGNUS_LOOP_P4 | 312.8083 | 31.361 | 312.292075 | 31.17275 | 327.627486 | 46.612051 | 74.56035476 | -8.16867105 | 239.9997 | 54418.9382291667 | 2007-11-14 22:31:03 | 54419.3196643518 | 2007-11-15 07:40:19 | 501015010 | 18.279 | 15 | 18.287 | 18.279 | 0 | 18.287 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.286 | 14.286 | 32.9439 | 0 | PROCESSED | 57540.5253935185 | 2016-06-01 12:36:34 | 54798 | 2008-11-28 00:00:00 | 54430.2398726852 | 2007-11-26 05:45:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501015010/ | Quick Look | ![]() |
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287 | CYGNUS_LOOP_P5 | 312.5567 | 31.1701 | 312.040041 | 30.982753 | 327.230821 | 46.520779 | 74.2739834 | -8.12038976 | 239.9995 | 54419.3201388889 | 2007-11-15 07:41:00 | 54420.0627777778 | 2007-11-16 01:30:24 | 501016010 | 28.4062 | 22 | 28.4062 | 28.4062 | 0 | 28.4062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.37 | 25.37 | 64.1559 | 1 | PROCESSED | 57540.538900463 | 2016-06-01 12:56:01 | 54798 | 2008-11-28 00:00:00 | 54430.4318865741 | 2007-11-26 10:21:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501016010/ | Quick Look | ![]() |
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288 | CYGNUS_LOOP_P6 | 312.3057 | 30.9823 | 311.788615 | 30.795857 | 326.837045 | 46.431585 | 73.99029438 | -8.06939848 | 240.0003 | 54415.3923032407 | 2007-11-11 09:24:55 | 54416.1668287037 | 2007-11-12 04:00:14 | 501017010 | 28.7049 | 22 | 28.7049 | 28.7049 | 0 | 28.7049 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.8878 | 26.8878 | 66.9119 | 0 | PROCESSED | 57540.490474537 | 2016-06-01 11:46:17 | 54798 | 2008-11-28 00:00:00 | 54430.18875 | 2007-11-26 04:31:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501017010/ | Quick Look | ![]() |
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289 | CYGNUS_LOOP_P16 | 312.737 | 30.4592 | 312.216541 | 30.271212 | 327.037451 | 45.805605 | 73.81069789 | -8.68546284 | 61.9998 | 53877.1905439815 | 2006-05-22 04:34:23 | 53877.7605671296 | 2006-05-22 18:15:13 | 501033010 | 23.3375 | 22 | 23.3695 | 23.3375 | 23.3695 | 23.3695 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.1184 | 20.1184 | 49.2439 | 2 | PROCESSED | 57534.3873611111 | 2016-05-26 09:17:48 | 54398 | 2007-10-25 00:00:00 | 53926.8416319445 | 2006-07-10 20:11:57 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501033010/ | Quick Look | ![]() |
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290 | GC_SGR_B_NORTH | 266.6955 | -28.3829 | 265.90467 | -28.36493 | 267.072555 | -4.975375 | 0.60514127 | 0.06995468 | 271.4417 | 54002.2105555556 | 2006-09-24 05:03:12 | 54003.2919444444 | 2006-09-25 07:00:24 | 501040020 | 44.8295 | 38 | 44.8455 | 44.8295 | 44.8375 | 44.8535 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.9705 | 39.9705 | 93.4319 | 1 | PROCESSED | 57535.678125 | 2016-05-27 16:16:30 | 54744 | 2008-10-05 00:00:00 | 54021.2868055556 | 2006-10-13 06:53:00 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040020/ | Quick Look | ![]() |
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291 | HESS J1614-518 | 243.5851 | -51.743 | 242.630135 | -51.617031 | 251.446035 | -29.987821 | 331.574855 | -0.5276897 | 283.402 | 53993.6672222222 | 2006-09-15 16:00:48 | 53994.4571064815 | 2006-09-16 10:58:14 | 501042010 | 40.1777 | 50 | 40.1857 | 40.1777 | 40.1857 | 40.1857 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.5607 | 43.5607 | 68.2279 | 0 | PROCESSED | 57535.5776967593 | 2016-05-27 13:51:53 | 54526 | 2008-03-01 00:00:00 | 54020.8545833333 | 2006-10-12 20:30:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501042010/ | Quick Look | ![]() |
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292 | HESS J1614-518 BG | 242.0174 | -52.4329 | 241.059171 | -52.300176 | 250.522759 | -30.865237 | 330.3996927 | -0.37656553 | 291.2192 | 53994.4597569444 | 2006-09-16 11:02:03 | 53995.3015509259 | 2006-09-17 07:14:14 | 501043010 | 43.5554 | 50 | 43.5634 | 43.5634 | 43.5554 | 43.5634 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 50.5922 | 50.5922 | 72.7039 | 1 | PROCESSED | 57535.5823726852 | 2016-05-27 13:58:37 | 54526 | 2008-03-01 00:00:00 | 54020.8662268518 | 2006-10-12 20:47:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501043010/ | Quick Look | ![]() |
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293 | GALACTIC CENTER GC3 | 265.5781 | -29.4684 | 264.780645 | -29.444998 | 266.119721 | -6.086772 | 359.1684549 | 0.33584661 | 108.8001 | 54170.7951273148 | 2007-03-11 19:04:59 | 54171.3397453704 | 2007-03-12 08:09:14 | 501048010 | 27.4546 | 25 | 27.4786 | 27.4546 | 0 | 27.4786 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.0548 | 24.0548 | 47.0479 | 1 | PROCESSED | 57537.6483333333 | 2016-05-29 15:33:36 | 54736 | 2008-09-27 00:00:00 | 54182.2788425926 | 2007-03-23 06:41:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501048010/ | Quick Look | ![]() |
294 | GALACTIC CENTER | 265.9089 | -29.649 | 265.11021 | -29.627197 | 266.414403 | -6.258746 | 359.16615355 | -0.00387238 | 269 | 54017.0975115741 | 2006-10-09 02:20:25 | 54017.5690277778 | 2006-10-09 13:39:24 | 501050010 | 22.0477 | 20 | 22.0477 | 22.0477 | 22.0477 | 22.0477 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18.6256 | 18.6256 | 40.7359 | 0 | PROCESSED | 57535.8013194445 | 2016-05-27 19:13:54 | 54735 | 2008-09-26 00:00:00 | 54053.4127777778 | 2006-11-14 09:54:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501050010/ | Quick Look | ![]() |
295 | GALACTIC CENTER | 265.2994 | -30.4982 | 264.495374 | -30.473432 | 265.90984 | -7.123709 | 358.16648703 | -0.00302139 | 269.0003 | 54018.8881828704 | 2006-10-10 21:18:59 | 54019.4209953704 | 2006-10-11 10:06:14 | 501053010 | 21.9086 | 20 | 21.9086 | 21.9321 | 21.9166 | 21.9166 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.948 | 19.948 | 46.0319 | 0 | PROCESSED | 57535.8190393518 | 2016-05-27 19:39:25 | 54735 | 2008-09-26 00:00:00 | 54053.5019675926 | 2006-11-14 12:02:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501053010/ | Quick Look | ![]() |
296 | GC SGR D EAST | 267.2856 | -27.6502 | 266.49923 | -27.635104 | 267.579665 | -4.231943 | 1.50163715 | 0.00269695 | 108.7997 | 54176.2132407407 | 2007-03-17 05:07:04 | 54177.8737731482 | 2007-03-18 20:58:14 | 501060010 | 64.7953 | 63 | 64.7953 | 64.8267 | 0 | 64.8113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.6297 | 54.6297 | 143.4659 | 1 | PROCESSED | 57537.7151851852 | 2016-05-29 17:09:52 | 54736 | 2008-09-27 00:00:00 | 54185.4429050926 | 2007-03-26 10:37:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501060010/ | Quick Look | ![]() |
297 | RXJ1713-3946 | 258.5524 | -39.4291 | 257.687827 | -39.37177 | 260.79719 | -16.352329 | 347.6770378 | -0.38034705 | 267.9999 | 53997.5713773148 | 2006-09-19 13:42:47 | 53997.9140509259 | 2006-09-19 21:56:14 | 501069010 | 18.375 | 20 | 18.375 | 18.375 | 18.375 | 18.375 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14.2767 | 14.2767 | 29.5999 | 0 | PROCESSED | 57535.6332060185 | 2016-05-27 15:11:49 | 54526 | 2008-03-01 00:00:00 | 54021.1502546296 | 2006-10-13 03:36:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501069010/ | Quick Look | ![]() |
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298 | RXJ1713-3946 | 258.9408 | -39.7267 | 258.073523 | -39.671212 | 261.133474 | -16.624716 | 347.60984156 | -0.7970823 | 268.0009 | 54013.3138541667 | 2006-10-05 07:31:57 | 54013.877974537 | 2006-10-05 21:04:17 | 501072010 | 19.9817 | 20 | 19.9817 | 19.9817 | 19.9817 | 19.9817 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.2997 | 16.2997 | 48.718 | 1 | PROCESSED | 57535.7676736111 | 2016-05-27 18:25:27 | 54526 | 2008-03-01 00:00:00 | 54021.6599652778 | 2006-10-13 15:50:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501072010/ | Quick Look | ![]() |
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299 | U SCO | 245.6292 | -17.8133 | 244.907482 | -17.696814 | 246.808074 | 3.687304 | 357.72295453 | 21.91020567 | 93.2753 | 55239.299224537 | 2010-02-12 07:10:53 | 55239.8259027778 | 2010-02-12 19:49:18 | 404018030 | 26.826 | 20 | 26.826 | 26.826 | 0 | 26.826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.9037 | 24.9037 | 45.472 | 1 | PROCESSED | 57550.5610763889 | 2016-06-11 13:27:57 | 55619 | 2011-02-27 00:00:00 | 55253.1155671296 | 2010-02-26 02:46:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | DAI TAKEI | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018030/ | Quick Look | ![]() |
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300 | GC18 | 266.183 | -28.6222 | 265.39077 | -28.601742 | 266.626489 | -5.225763 | 0.16630142 | 0.32982124 | 260.5302 | 54384.4819560185 | 2007-10-11 11:34:01 | 54384.9633564815 | 2007-10-11 23:07:14 | 502006010 | 22.6311 | 20 | 22.6311 | 22.6413 | 0 | 22.6351 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.6702 | 21.6702 | 41.5841 | 1 | PROCESSED | 57540.2503356482 | 2016-06-01 06:00:29 | 54771 | 2008-11-01 00:00:00 | 54402.6632291667 | 2007-10-29 15:55:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502006010/ | Quick Look | ![]() |
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301 | GC21 | 267.484 | -27.3686 | 266.699338 | -27.354471 | 267.750913 | -3.947195 | 1.83363899 | -0.00346152 | 261.5433 | 54385.9113888889 | 2007-10-12 21:52:24 | 54386.3127199074 | 2007-10-13 07:30:19 | 502009010 | 20.8615 | 20 | 20.8615 | 20.8615 | 0 | 20.8615 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.6483 | 19.6483 | 34.6639 | 1 | PROCESSED | 57540.2599189815 | 2016-06-01 06:14:17 | 54771 | 2008-11-01 00:00:00 | 54402.5769444444 | 2007-10-29 13:50:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502009010/ | Quick Look | ![]() |
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302 | GC22 | 266.3806 | -28.337 | 265.590118 | -28.317504 | 266.793387 | -4.936169 | 0.50023196 | 0.3305092 | 262.5049 | 54386.3138888889 | 2007-10-13 07:32:00 | 54386.785 | 2007-10-13 18:50:24 | 502010010 | 21.6214 | 20 | 21.6214 | 21.6214 | 0 | 21.6214 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1944 | 21.1944 | 40.662 | 1 | PROCESSED | 57540.2655439815 | 2016-06-01 06:22:23 | 54771 | 2008-11-01 00:00:00 | 54402.6900231482 | 2007-10-29 16:33:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502010010/ | Quick Look | ![]() |
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303 | HESS J1745-303 3 | 266.0567 | -30.2413 | 265.254155 | -30.220204 | 266.559978 | -6.847208 | 358.72882707 | -0.42335991 | 69.0003 | 54533.6682523148 | 2008-03-08 16:02:17 | 54535.8752199074 | 2008-03-10 21:00:19 | 502018010 | 79.0162 | 67 | 79.0162 | 79.0402 | 0 | 79.0242 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.201 | 70.201 | 190.658 | 2 | PROCESSED | 57541.8566898148 | 2016-06-02 20:33:38 | 54919 | 2009-03-29 00:00:00 | 54550.3420601852 | 2008-03-25 08:12:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502018010/ | Quick Look | ![]() |
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304 | A478 OFFSET A | 63.4449 | 10.2053 | 62.759891 | 10.079352 | 63.389046 | -10.816509 | 182.72704568 | -28.38203256 | 259.1008 | 55600.4642361111 | 2011-02-08 11:08:30 | 55601.5488194444 | 2011-02-09 13:10:18 | 805001010 | 44.3964 | 45 | 44.3964 | 44.3964 | 0 | 44.3964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.2374 | 35.2374 | 93.6998 | 1 | PROCESSED | 57600.8998148148 | 2016-07-31 21:35:44 | 55983 | 2012-02-26 00:00:00 | 55617.4093981482 | 2011-02-25 09:49:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | ANDREW FABIAN | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805001010/ | Quick Look | ![]() |
305 | VELA JR P7 | 133.7759 | -45.5828 | 133.340558 | -45.390922 | 159.660843 | -58.904253 | 266.02998701 | -0.32446592 | 347.0033 | 54286.9870023148 | 2007-07-05 23:41:17 | 54287.3023032407 | 2007-07-06 07:15:19 | 502029010 | 14.5838 | 10 | 14.5838 | 14.5838 | 0 | 14.5838 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.605 | 12.605 | 27.2399 | 0 | PROCESSED | 57539.1100810185 | 2016-05-31 02:38:31 | 54696 | 2008-08-18 00:00:00 | 54328.4686111111 | 2007-08-16 11:14:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502029010/ | Quick Look | ![]() |
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306 | THE MOON | 337.3918 | -5.9294 | 336.739564 | -6.185815 | 336.879419 | 3.286876 | 58.6068568 | -50.1809823 | 252.3009 | 56990.3496643518 | 2014-11-29 08:23:31 | 56990.483587963 | 2014-11-29 11:36:22 | 809001320 | 6.3868 | 45 | 6.3868 | 6.3868 | 0 | 6.3868 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4101851852 | 2016-08-17 09:50:40 | 57415 | 2016-01-28 00:00:00 | 57006.395 | 2014-12-15 09:28:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001320/ | Quick Look | ![]() |
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307 | XB1323-619 | 201.6454 | -62.1418 | 200.814994 | -61.88221 | 229.562797 | -47.947963 | 307.02498182 | 0.45033402 | 99.5731 | 54109.4794907407 | 2007-01-09 11:30:28 | 54110.9168402778 | 2007-01-10 22:00:15 | 401002010 | 55.9368 | 50 | 55.9368 | 55.9368 | 0 | 55.9368 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.8173 | 81.8173 | 124.1769 | 1 | PROCESSED | 57536.8666087963 | 2016-05-28 20:47:55 | 54735 | 2008-09-26 00:00:00 | 54133.0271759259 | 2007-02-02 00:39:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYASU DOTANI | JAP | 1 | AO1 | BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401002010/ | Quick Look | ![]() |
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308 | VELA JR P10 | 132.9993 | -45.7656 | 132.567919 | -45.576468 | 158.955645 | -59.347984 | 265.8217159 | -0.85784968 | 347.0018 | 54287.9522337963 | 2007-07-06 22:51:13 | 54288.2308564815 | 2007-07-07 05:32:26 | 502032010 | 13.04 | 10 | 13.048 | 13.04 | 0 | 13.056 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6988 | 10.6988 | 24.0679 | 0 | PROCESSED | 57539.1146527778 | 2016-05-31 02:45:06 | 54703 | 2008-08-25 00:00:00 | 54333.4328240741 | 2007-08-21 10:23:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502032010/ | Quick Look | ![]() |
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309 | VELA JR P14 | 131.9312 | -46.3861 | 131.508056 | -46.200795 | 158.369308 | -60.268301 | 265.83284327 | -1.824218 | 347.0017 | 54290.4416087963 | 2007-07-09 10:35:55 | 54290.675150463 | 2007-07-09 16:12:13 | 502036010 | 11.034 | 10 | 11.034 | 11.042 | 0 | 11.042 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.1391 | 11.1391 | 20.1679 | 0 | PROCESSED | 57539.1311226852 | 2016-05-31 03:08:49 | 54696 | 2008-08-18 00:00:00 | 54328.4740277778 | 2007-08-16 11:22:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502036010/ | Quick Look | ![]() |
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310 | VELA JR P15 | 132.3334 | -46.3288 | 131.908455 | -46.142044 | 158.77835 | -60.071 | 265.96324441 | -1.57253381 | 347.0016 | 54291.1946064815 | 2007-07-10 04:40:14 | 54291.46 | 2007-07-10 11:02:24 | 502037010 | 8.876 | 10 | 8.876 | 8.876 | 0 | 8.876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.3411 | 7.3411 | 22.9121 | 1 | PROCESSED | 57539.1396990741 | 2016-05-31 03:21:10 | 54696 | 2008-08-18 00:00:00 | 54328.472962963 | 2007-08-16 11:21:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502037010/ | Quick Look | ![]() |
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311 | 47 TUCANAE | 6.2112 | -71.9961 | 5.659821 | -72.273106 | 311.457534 | -62.358991 | 305.8317488 | -44.9821189 | 65.5967 | 54261.1765162037 | 2007-06-10 04:14:11 | 54263.5404976852 | 2007-06-12 12:58:19 | 502048010 | 132.1052 | 133 | 132.1452 | 132.1052 | 0 | 132.1372 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.9042 | 132.9042 | 204.2319 | 1 | PROCESSED | 57538.9491666667 | 2016-05-30 22:46:48 | 54745 | 2008-10-06 00:00:00 | 54271.5258796296 | 2007-06-20 12:37:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 2 | AO2 | OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502048010/ | Quick Look | ![]() |
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312 | M17 EAST BKG | 275.6441 | -15.5803 | 274.925967 | -15.60595 | 275.476675 | 7.75309 | 15.81995827 | -0.84785909 | 271.9998 | 54380.0947800926 | 2007-10-07 02:16:29 | 54381.7571064815 | 2007-10-08 18:10:14 | 502053010 | 71.494 | 67 | 71.494 | 71.5085 | 0 | 71.502 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62.5549 | 62.5549 | 143.61 | 1 | PROCESSED | 57540.2032175926 | 2016-06-01 04:52:38 | 54771 | 2008-11-01 00:00:00 | 54403.2344791667 | 2007-10-30 05:37:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAHIRO TSUJIMOTO | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502053010/ | Quick Look | ![]() |
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313 | GALACTIC BULGE | 268.3774 | -29.9651 | 267.576244 | -29.955267 | 268.575567 | -6.53206 | 359.99980668 | -2.0020922 | 279.4328 | 54372.0700347222 | 2007-09-29 01:40:51 | 54375.590462963 | 2007-10-02 14:10:16 | 502059010 | 136.824 | 133 | 136.824 | 136.824 | 0 | 136.824 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.5156 | 110.5156 | 304.1306 | 2 | PROCESSED | 57540.2260185185 | 2016-06-01 05:25:28 | 54770 | 2008-10-31 00:00:00 | 54402.653275463 | 2007-10-29 15:40:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502059010/ | Quick Look | ![]() |
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314 | HD45314 | 96.8131 | 14.89 | 96.098891 | 14.921299 | 96.656857 | -8.393671 | 196.95740391 | 1.52274638 | 93.5296 | 56935.6339814815 | 2014-10-05 15:12:56 | 56937.7981134259 | 2014-10-07 19:09:17 | 409019010 | 82.0799 | 80 | 82.0879 | 82.0879 | 0 | 82.0799 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6300115741 | 2016-08-16 15:07:13 | 57355 | 2015-11-29 00:00:00 | 56989.5080208333 | 2014-11-28 12:11:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090079 | We propose a Suzaku observation of a newly-found Gamma Cas analogue HD45314. The Gamma Cas analogues constitute a small but distinctive group showing anomalously hard X-ray spectra. We propose a Suzaku observation of HD45314 and compare it with the XMM data taken previously (Rauw et al. 2013) to reveal an expected change in the X-ray spectra. This will give us a clue to understand the X-ray production mechanism of this source and the gamma Cas analogues. | GALACTIC POINT SOURCES | 4 | B | MASAHIRO TSUJIMOTO | JAP | 9 | AO9 | INVESTIGATION OF A GAMMA CAS ANALOGUES USING SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409019010/ | Quick Look | ![]() |
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315 | Crab Nebula | 83.6622 | 21.1838 | 82.914561 | 21.151265 | 84.089646 | -2.127158 | 185.27784655 | -6.20565133 | 88.1125 | 53628.0468055556 | 2005-09-15 01:07:24 | 53628.2988194444 | 2005-09-15 07:10:18 | 100022010 | 12.881 | 10 | 12.881 | 12.881 | 12.881 | 12.881 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12.241 | 12.241 | 21.7679 | 0 | PROCESSED | 57527.323275463 | 2016-05-19 07:45:31 | 54247 | 2007-05-27 00:00:00 | 54109.2599768518 | 2007-01-09 06:14:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000022 | Crab at 50arcmin off from the XIS aimpoint to study stray light. | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab at 50 arcmin off | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022010/ | Quick Look | ![]() |
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316 | A133_N | 15.6732 | -21.6726 | 15.062059 | -21.941094 | 5.322246 | -26.023104 | 148.68503798 | -83.97324559 | 44.9987 | 55352.9000347222 | 2010-06-05 21:36:03 | 55354.0974768518 | 2010-06-07 02:20:22 | 805020010 | 50.2334 | 50 | 50.2334 | 50.2334 | 0 | 50.2334 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44.176 | 44.176 | 103.416 | 1 | PROCESSED | 57551.8040740741 | 2016-06-12 19:17:52 | 55765 | 2011-07-23 00:00:00 | 55393.4422916667 | 2010-07-16 10:36:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805020010/ | Quick Look | ![]() |
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317 | ANTICENTER2 | 12.9862 | 62.9112 | 12.227424 | 62.639587 | 45.279185 | 50.910305 | 122.98962226 | 0.03950805 | 69.9598 | 54679.0120717593 | 2008-08-01 00:17:23 | 54680.8411921296 | 2008-08-02 20:11:19 | 503006010 | 86.1101 | 80 | 86.123 | 86.123 | 0 | 86.1101 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.785 | 106.785 | 158.0198 | 1 | PROCESSED | 57543.2173726852 | 2016-06-04 05:13:01 | 55070 | 2009-08-27 00:00:00 | 54693.3237847222 | 2008-08-15 07:46:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KENSUKE MASUI | JAP | 3 | AO3 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503006010/ | Quick Look | ![]() |
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318 | GC_LARGEPROJECT2 | 266.7785 | -29.1292 | 265.982946 | -29.111621 | 267.162656 | -5.719811 | 0.00479668 | -0.37932142 | 260.8763 | 54712.9538078704 | 2008-09-03 22:53:29 | 54714.2891087963 | 2008-09-05 06:56:19 | 503008010 | 53.6388 | 50 | 53.6548 | 53.6388 | 0 | 53.6548 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8111 | 42.8111 | 115.3338 | 0 | PROCESSED | 57543.7762615741 | 2016-06-04 18:37:49 | 54557 | 2008-04-01 00:00:00 | 54780.4880092593 | 2008-11-10 11:42:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503008010/ | Quick Look | ![]() |
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319 | GC_LARGEPROJECT3 | 266.4525 | -29.3384 | 265.655678 | -29.319237 | 266.881748 | -5.935661 | 359.67825031 | -0.24492188 | 260.8779 | 54714.2896759259 | 2008-09-05 06:57:08 | 54715.6634722222 | 2008-09-06 15:55:24 | 503009010 | 52.3975 | 50 | 52.4055 | 52.3975 | 0 | 52.4114 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2691 | 40.2691 | 118.6778 | 2 | PROCESSED | 57543.769375 | 2016-06-04 18:27:54 | 54557 | 2008-04-01 00:00:00 | 54780.6767476852 | 2008-11-10 16:14:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503009010/ | Quick Look | ![]() |
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320 | GC_LARGEPROJECT5 | 265.9469 | -29.8331 | 265.147019 | -29.811478 | 266.45285 | -6.44183 | 359.02671432 | -0.12852462 | 265.43 | 54717.3806597222 | 2008-09-08 09:08:09 | 54718.8981365741 | 2008-09-09 21:33:19 | 503011010 | 57.6334 | 50 | 57.6334 | 57.6334 | 0 | 57.6334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1555 | 40.1555 | 131.0998 | 1 | PROCESSED | 57543.8408449074 | 2016-06-04 20:10:49 | 54557 | 2008-04-01 00:00:00 | 54780.6683912037 | 2008-11-10 16:02:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503011010/ | Quick Look | ![]() |
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321 | GC_LARGEPROJECT9 | 265.0297 | -30.9626 | 264.222709 | -30.936519 | 265.692051 | -7.595667 | 357.64981902 | -0.05267713 | 269.1132 | 54728.3146412037 | 2008-09-19 07:33:05 | 54729.4140393518 | 2008-09-20 09:56:13 | 503015010 | 56.7716 | 50 | 56.7796 | 56.7716 | 0 | 56.7876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.8454 | 52.8454 | 94.9759 | 0 | PROCESSED | 57543.8851041667 | 2016-06-04 21:14:33 | 54557 | 2008-04-01 00:00:00 | 54780.4933564815 | 2008-11-10 11:50:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503015010/ | Quick Look | ![]() |
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322 | GC_LARGEPROJECT12 | 264.5606 | -31.5967 | 263.749555 | -31.56834 | 265.310874 | -8.24393 | 356.89961278 | -0.05143068 | 268.4538 | 54742.7536226852 | 2008-10-03 18:05:13 | 54743.154375 | 2008-10-04 03:42:18 | 503018020 | 12.2466 | 10 | 12.2466 | 12.2466 | 0 | 12.2466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.232 | 10.232 | 34.6179 | 1 | PROCESSED | 57544.0096527778 | 2016-06-05 00:13:54 | 54557 | 2008-04-01 00:00:00 | 54780.5624652778 | 2008-11-10 13:29:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018020/ | Quick Look | ![]() |
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323 | HESS J1825-137 | 276.5024 | -13.9965 | 275.79256 | -14.02632 | 276.383198 | 9.300131 | 17.60816681 | -0.84042551 | 271.0002 | 54754.9096064815 | 2008-10-15 21:49:50 | 54756.458599537 | 2008-10-17 11:00:23 | 503028010 | 57.2104 | 50 | 57.2104 | 57.2104 | 0 | 57.2104 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.5485 | 51.5485 | 133.7938 | 1 | PROCESSED | 57544.1955324074 | 2016-06-05 04:41:34 | 55148 | 2009-11-13 00:00:00 | 54780.7053703704 | 2008-11-10 16:55:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAAKI TANAKA | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503028010/ | Quick Look | ![]() |
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324 | VELA JR P24 | 132.0303 | -46.6729 | 131.609003 | -46.487232 | 158.79782 | -60.473277 | 266.0989339 | -1.95139979 | 347.001 | 54652.7719328704 | 2008-07-05 18:31:35 | 54653.1668865741 | 2008-07-06 04:00:19 | 503036010 | 12.3735 | 10 | 12.3735 | 12.3735 | 0 | 12.3735 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2548 | 12.2548 | 34.12 | 1 | PROCESSED | 57542.9791203704 | 2016-06-03 23:29:56 | 55048 | 2009-08-05 00:00:00 | 54679.3185763889 | 2008-08-01 07:38:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503036010/ | Quick Look | ![]() |
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325 | VELA JR P28 | 133.7109 | -46.6037 | 133.283226 | -46.412037 | 160.667114 | -59.788002 | 266.78076878 | -1.01777641 | 347.0004 | 54654.1674537037 | 2008-07-07 04:01:08 | 54654.4259143518 | 2008-07-07 10:13:19 | 503040010 | 13.093 | 10 | 13.101 | 13.093 | 0 | 13.101 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.054 | 12.054 | 22.296 | 0 | PROCESSED | 57542.9904282407 | 2016-06-03 23:46:13 | 55048 | 2009-08-05 00:00:00 | 54679.3674421296 | 2008-08-01 08:49:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503040010/ | Quick Look | ![]() |
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326 | VELA JR P29 | 134.0711 | -46.43 | 133.640871 | -46.237075 | 160.890422 | -59.507166 | 266.80859879 | -0.71638658 | 347 | 54654.4264814815 | 2008-07-07 10:14:08 | 54654.7203703704 | 2008-07-07 17:17:20 | 503041010 | 11.3685 | 10 | 11.3802 | 11.3685 | 0 | 11.3802 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.2225 | 8.2225 | 25.3679 | 0 | PROCESSED | 57542.9909606482 | 2016-06-03 23:46:59 | 55048 | 2009-08-05 00:00:00 | 54679.3958217593 | 2008-08-01 09:29:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503041010/ | Quick Look | ![]() |
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327 | VELA JR P38 | 132.2003 | -47.2308 | 131.782721 | -47.04451 | 159.617188 | -60.877835 | 266.60579829 | -2.21244802 | 347.0003 | 54657.2423958333 | 2008-07-10 05:49:03 | 54657.5209953704 | 2008-07-10 12:30:14 | 503050010 | 14.0436 | 10 | 14.0436 | 14.0436 | 0 | 14.0596 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.426 | 11.426 | 24.0639 | 0 | PROCESSED | 57543.0197800926 | 2016-06-04 00:28:29 | 55037 | 2009-07-25 00:00:00 | 54670.2561111111 | 2008-07-23 06:08:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503050010/ | Quick Look | ![]() |
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328 | RCW 38 | 134.7638 | -47.5154 | 134.339139 | -47.320051 | 162.870038 | -60.148721 | 267.93999829 | -1.06526988 | 109.8553 | 54788.5064351852 | 2008-11-18 12:09:16 | 54790.699525463 | 2008-11-20 16:47:19 | 503054010 | 81.5377 | 80 | 81.5495 | 81.5377 | 0 | 81.5415 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.9281 | 60.9281 | 189.4597 | 1 | PROCESSED | 57544.5092013889 | 2016-06-05 12:13:15 | 55171 | 2009-12-06 00:00:00 | 54811.741099537 | 2008-12-11 17:47:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROKAZU ODAKA | JAP | 3 | AO3 | SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503054010/ | Quick Look | ![]() |
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329 | CYGNUS LOOP (P21) | 313.196 | 32.4197 | 312.684204 | 32.23006 | 328.688835 | 47.452326 | 75.60030214 | -7.75821821 | 61.9243 | 54619.9401967593 | 2008-06-02 22:33:53 | 54620.2975 | 2008-06-03 07:08:24 | 503057010 | 16.1703 | 15 | 16.1783 | 16.1703 | 0 | 16.1783 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.8903 | 12.8903 | 30.8639 | 0 | PROCESSED | 57542.700474537 | 2016-06-03 16:48:41 | 55003 | 2009-06-21 00:00:00 | 54636.2238078704 | 2008-06-19 05:22:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503057010/ | Quick Look | ![]() |
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330 | RABBIT | 214.6544 | -60.9713 | 213.733054 | -60.740946 | 236.398817 | -43.82174 | 313.31134091 | 0.131367 | 105.7763 | 54876.850787037 | 2009-02-14 20:25:08 | 54877.5224421296 | 2009-02-15 12:32:19 | 503071010 | 21.274 | 20 | 21.282 | 21.274 | 0 | 21.29 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.0126 | 18.0126 | 57.984 | 0 | PROCESSED | 57545.5405439815 | 2016-06-06 12:58:23 | 55330 | 2010-05-14 00:00:00 | 54892.945162037 | 2009-03-02 22:41:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TETSUICHI KISHISHITA | JAP | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503071010/ | Quick Look | ![]() |
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331 | HESS_J1809-193_N | 272.4044 | -19.3551 | 271.665869 | -19.36499 | 272.264534 | 4.066746 | 11.02929838 | 0.07166066 | 112.001 | 54556.5874421296 | 2008-03-31 14:05:55 | 54557.6877662037 | 2008-04-01 16:30:23 | 503078010 | 51.5309 | 40 | 51.5389 | 51.5309 | 0 | 51.5461 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8186 | 34.8186 | 95.0518 | 2 | PROCESSED | 57542.0290740741 | 2016-06-03 00:41:52 | 54950 | 2009-04-29 00:00:00 | 54571.3638888889 | 2008-04-15 08:44:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYASU ANADA | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503078010/ | Quick Look | ![]() |
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332 | VICINITY_OF_PKS_2155-1 | 329.2367 | -30.5281 | 328.510685 | -30.766467 | 320.669664 | -16.905257 | 17.16872193 | -51.86657338 | 55.8337 | 54585.7726736111 | 2008-04-29 18:32:39 | 54588.3542592593 | 2008-05-02 08:30:08 | 503082010 | 90.1812 | 80 | 90.1812 | 90.1812 | 0 | 90.1812 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.7921 | 76.7921 | 223.0237 | 4 | PROCESSED | 57542.4840277778 | 2016-06-03 11:37:00 | 54975 | 2009-05-24 00:00:00 | 54608.3373726852 | 2008-05-22 08:05:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHISHIGE HAGIHARA | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503082010/ | Quick Look | ![]() |
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333 | SGR_B2 | 266.8788 | -28.4436 | 266.087557 | -28.426518 | 267.23571 | -5.032452 | 0.63679 | -0.09938091 | 266.4718 | 55096.836412037 | 2009-09-22 20:04:26 | 55102.6667592593 | 2009-09-28 16:00:08 | 504004020 | 202.0945 | 200 | 202.0945 | 202.1025 | 0 | 202.0945 | 3 | 4 | 0 | 3 | 1 | 0 | 0 | 178.2831 | 178.2831 | 303.5437 | 4 | PROCESSED | 57548.82125 | 2016-06-09 19:42:36 | 55500 | 2010-10-31 00:00:00 | 55133.4505092593 | 2009-10-29 10:48:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAYOSHI NOBUKAWA | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004020/ | Quick Look | ![]() |
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334 | BLOWOUT1 | 312.2225 | 31.7347 | 311.709294 | 31.548551 | 327.170903 | 47.151978 | 74.53998499 | -7.54540267 | 244.0864 | 55158.2754166667 | 2009-11-23 06:36:36 | 55158.9655555556 | 2009-11-23 23:10:24 | 504011010 | 24.1854 | 23 | 24.2014 | 24.1854 | 0 | 24.1934 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4768 | 19.4768 | 59.6039 | 1 | PROCESSED | 57549.5243055556 | 2016-06-10 12:35:00 | 55545 | 2010-12-15 00:00:00 | 55176.2112731482 | 2009-12-11 05:04:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504011010/ | Quick Look | ![]() |
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335 | BLOWOUT3 | 311.7021 | 31.3134 | 311.187829 | 31.12914 | 326.330215 | 46.937186 | 73.92913651 | -7.4588166 | 242.4356 | 55160.1363888889 | 2009-11-25 03:16:24 | 55160.4723611111 | 2009-11-25 11:20:12 | 504013010 | 16.1599 | 16 | 16.1599 | 16.1599 | 0 | 16.1599 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.8101 | 11.8101 | 29.0219 | 0 | PROCESSED | 57549.5443634259 | 2016-06-10 13:03:53 | 55545 | 2010-12-15 00:00:00 | 55176.2365740741 | 2009-12-11 05:40:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504013010/ | Quick Look | ![]() |
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336 | FESI1 | 313.4345 | 30.6099 | 312.913405 | 30.419428 | 327.914732 | 45.71047 | 74.31119672 | -9.05841998 | 226.3696 | 55182.5546180556 | 2009-12-17 13:18:39 | 55183.3334837963 | 2009-12-18 08:00:13 | 504017010 | 32.2876 | 24 | 32.2876 | 32.2876 | 0 | 32.2876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.2129 | 27.2129 | 67.2859 | 0 | PROCESSED | 57549.881099537 | 2016-06-10 21:08:47 | 55575 | 2011-01-14 00:00:00 | 55204.4679976852 | 2010-01-08 11:13:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504017010/ | Quick Look | ![]() |
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337 | HESS J1731-347 N | 262.8483 | -34.6425 | 262.016963 | -34.605825 | 263.993904 | -11.350062 | 353.56257635 | -0.49517094 | 91.6366 | 55244.8937037037 | 2010-02-17 21:26:56 | 55245.7189699074 | 2010-02-18 17:15:19 | 504032010 | 41.5263 | 40 | 41.5263 | 41.5263 | 0 | 41.5263 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.8653 | 32.8653 | 71.2719 | 0 | PROCESSED | 57550.6405555556 | 2016-06-11 15:22:24 | 55623 | 2011-03-03 00:00:00 | 55257.0108449074 | 2010-03-02 00:15:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504032010/ | Quick Look | ![]() |
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338 | GALACTICDISC3-1 | 15.309 | 67.9759 | 14.492554 | 67.706941 | 51.801719 | 54.210388 | 123.85392042 | 5.12169353 | 244.2747 | 55214.8348148148 | 2010-01-18 20:02:08 | 55216.0225 | 2010-01-20 00:32:24 | 504038010 | 55.2279 | 50 | 55.2279 | 55.2279 | 0 | 55.2279 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3329 | 43.3329 | 102.5998 | 2 | PROCESSED | 57550.2600231482 | 2016-06-11 06:14:26 | 55594 | 2011-02-02 00:00:00 | 55228.2005092593 | 2010-02-01 04:48:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHUNSUKE KIMURA | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504038010/ | Quick Look | ![]() |
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339 | ASO0505 | 339.5988 | 59.0734 | 339.120995 | 58.812928 | 20.160721 | 59.131044 | 106.55945745 | 0.49758229 | 62.7751 | 55001.185775463 | 2009-06-19 04:27:31 | 55001.7494675926 | 2009-06-19 17:59:14 | 504048010 | 26.3616 | 20 | 26.3696 | 26.3616 | 0 | 26.3776 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8416 | 23.8416 | 48.6959 | 1 | PROCESSED | 57547.5983449074 | 2016-06-08 14:21:37 | 55381 | 2010-07-04 00:00:00 | 55015.2523148148 | 2009-07-03 06:03:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504048010/ | Quick Look | ![]() |
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340 | ASO0418 | 279.775 | -5.7085 | 279.106672 | -5.754175 | 280.186655 | 17.387028 | 26.44714681 | 0.13153934 | 86.843 | 54934.6472800926 | 2009-04-13 15:32:05 | 54935.7578587963 | 2009-04-14 18:11:19 | 504052010 | 41.0684 | 40 | 41.0802 | 41.0844 | 0 | 41.0684 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.5258 | 33.5258 | 95.9378 | 0 | PROCESSED | 57546.1671296296 | 2016-06-07 04:00:40 | 55324 | 2010-05-08 00:00:00 | 54949.5662268518 | 2009-04-28 13:35:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504052010/ | Quick Look | ![]() |
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341 | FJ1145+6430 | 176.4302 | 64.5188 | 175.749504 | 64.796472 | 138.22089 | 54.839324 | 134.11889935 | 51.15827028 | 157.0241 | 56940.8652199074 | 2014-10-10 20:45:55 | 56941.847337963 | 2014-10-11 20:20:10 | 809036010 | 44.5555 | 45 | 44.5555 | 44.9155 | 0 | 44.9235 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6416435185 | 2016-08-16 15:23:58 | 57345 | 2015-11-19 00:00:00 | 56979.4120949074 | 2014-11-18 09:53:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809036010/ | Quick Look | ![]() |
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342 | ASO0215 | 154.6836 | -58.9426 | 154.241353 | -58.691332 | 196.521873 | -60.887637 | 284.32918046 | -1.70077172 | 314.5017 | 55019.3141782407 | 2009-07-07 07:32:25 | 55020.3404976852 | 2009-07-08 08:10:19 | 504053010 | 40.0868 | 40 | 40.0868 | 40.0868 | 0 | 40.0868 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.4782 | 35.4782 | 88.6598 | 0 | PROCESSED | 57547.8126851852 | 2016-06-08 19:30:16 | 55399 | 2010-07-22 00:00:00 | 55029.2468055556 | 2009-07-17 05:55:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504053010/ | Quick Look | ![]() |
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343 | ASO0319 | 224.8822 | -60.8823 | 223.89321 | -60.683278 | 242.498215 | -41.674426 | 317.89227503 | -1.78687667 | 277.7774 | 55049.7078125 | 2009-08-06 16:59:15 | 55051.0238425926 | 2009-08-08 00:34:20 | 504055010 | 42.3613 | 40 | 42.3613 | 42.3668 | 0 | 42.3773 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.5233 | 37.5233 | 113.6859 | 0 | PROCESSED | 57548.1027083333 | 2016-06-09 02:27:54 | 55430 | 2010-08-22 00:00:00 | 55062.2941782407 | 2009-08-19 07:03:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504055010/ | Quick Look | ![]() |
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344 | 3C_391 | 282.3812 | -0.9417 | 281.735823 | -0.99987 | 283.351934 | 21.926784 | 31.87573789 | -0.00377867 | 261.9952 | 55491.0759722222 | 2010-10-22 01:49:24 | 55493.8224537037 | 2010-10-24 19:44:20 | 505007010 | 99.3887 | 100 | 99.4607 | 99.3887 | 0 | 99.4687 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.374 | 89.374 | 237.2779 | 2 | PROCESSED | 57553.8698032407 | 2016-06-14 20:52:31 | 55287 | 2010-04-01 00:00:00 | 55502.3356597222 | 2010-11-02 08:03:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505007010/ | Quick Look | ![]() |
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345 | CYGNUS LOOP 1 | 313.2462 | 32.1399 | 312.732912 | 31.950084 | 328.580357 | 47.179033 | 75.40840203 | -7.96786776 | 81.7816 | 55300.7096759259 | 2010-04-14 17:01:56 | 55301.0293402778 | 2010-04-15 00:42:15 | 505009010 | 15.9992 | 13 | 15.9992 | 15.9992 | 0 | 15.9992 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.242 | 12.242 | 27.612 | 0 | PROCESSED | 57551.2105787037 | 2016-06-12 05:03:14 | 55287 | 2010-04-01 00:00:00 | 55362.3098726852 | 2010-06-15 07:26:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505009010/ | Quick Look | ![]() |
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346 | CYGNUS LOOP 2 | 312.7259 | 32.1633 | 312.213805 | 31.975338 | 327.998937 | 47.37656 | 75.14683323 | -7.61088939 | 81.0273 | 55301.0300925926 | 2010-04-15 00:43:20 | 55301.2897569444 | 2010-04-15 06:57:15 | 505010010 | 12.932 | 10 | 12.932 | 12.932 | 0 | 12.932 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.924 | 11.924 | 22.4319 | 0 | PROCESSED | 57551.2143402778 | 2016-06-12 05:08:39 | 55287 | 2010-04-01 00:00:00 | 55362.2959375 | 2010-06-15 07:06:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505010010/ | Quick Look | ![]() |
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347 | CYGNUS LOOP 3 | 312.9529 | 31.9301 | 312.439181 | 31.741329 | 328.122092 | 47.08601 | 75.08571271 | -7.90709143 | 81.0389 | 55301.2902777778 | 2010-04-15 06:58:00 | 55301.6209953704 | 2010-04-15 14:54:14 | 505011010 | 13.4448 | 12 | 13.4448 | 13.4448 | 0 | 13.4448 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.427 | 10.427 | 28.5719 | 0 | PROCESSED | 57551.2233333333 | 2016-06-12 05:21:36 | 55287 | 2010-04-01 00:00:00 | 55362.3557060185 | 2010-06-15 08:32:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505011010/ | Quick Look | ![]() |
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348 | CYGNUS LOOP 10 | 314.1171 | 30.7461 | 313.595298 | 30.553225 | 328.763604 | 45.604555 | 74.79486269 | -9.42625359 | 82.0017 | 55328.2812152778 | 2010-05-12 06:44:57 | 55328.6981134259 | 2010-05-12 16:45:17 | 505018010 | 16.268 | 16 | 16.276 | 16.276 | 0 | 16.268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6551 | 12.6551 | 36.012 | 0 | PROCESSED | 57551.4785069444 | 2016-06-12 11:29:03 | 55287 | 2010-04-01 00:00:00 | 55393.3335069445 | 2010-07-16 08:00:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505018010/ | Quick Look | ![]() |
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349 | G22.0+0.0 | 277.823 | -9.7151 | 277.134886 | -9.751345 | 277.921132 | 13.510599 | 22.00005623 | 0.00370699 | 89.3658 | 55302.6023842593 | 2010-04-16 14:27:26 | 55303.7272222222 | 2010-04-17 17:27:12 | 505025010 | 50.5294 | 50 | 50.5294 | 50.5294 | 0 | 50.5294 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.6208 | 44.6208 | 97.1598 | 0 | PROCESSED | 57551.270775463 | 2016-06-12 06:29:55 | 55737 | 2011-06-25 00:00:00 | 55375.7533101852 | 2010-06-28 18:04:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505025010/ | Quick Look | ![]() |
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350 | G37.0-0.1 | 284.8009 | 3.5813 | 284.176842 | 3.511637 | 286.494967 | 26.178305 | 37.00394757 | -0.09218404 | 68.6266 | 55303.7327893518 | 2010-04-17 17:35:13 | 55304.8814583333 | 2010-04-18 21:09:18 | 505027010 | 50.9694 | 50 | 50.9774 | 50.9774 | 0 | 50.9694 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.3361 | 45.3361 | 99.23 | 1 | PROCESSED | 57551.2689699074 | 2016-06-12 06:27:19 | 55693 | 2011-05-12 00:00:00 | 55326.2903125 | 2010-05-10 06:58:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505027010/ | Quick Look | ![]() |
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351 | SGR_C | 266.2461 | -29.3903 | 265.44899 | -29.370135 | 266.702279 | -5.992122 | 359.54016882 | -0.1184914 | 267.0744 | 55464.5256481482 | 2010-09-25 12:36:56 | 55466.608599537 | 2010-09-27 14:36:23 | 505031010 | 99.916 | 100 | 99.9561 | 99.916 | 0 | 99.956 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 89.0712 | 89.0712 | 179.9499 | 2 | PROCESSED | 57553.5757175926 | 2016-06-14 13:49:02 | 55853 | 2011-10-19 00:00:00 | 55484.3402777778 | 2010-10-15 08:10:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAYOSHI NOBUKAWA | JAP | 5 | AO5 | THE SAGITTARIUS C COMPLEX A ROSETTA STONE OF THE PAST ACTIVITY OF SAGITTARIUS A* | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505031010/ | Quick Look | ![]() |
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352 | BLOWOUT SHELL 1 | 311.9978 | 28.9736 | 311.471635 | 28.788286 | 325.391021 | 44.676168 | 72.22846422 | -9.10440661 | 48.7676 | 55360.0953587963 | 2010-06-13 02:17:19 | 55361.2627546296 | 2010-06-14 06:18:22 | 505055010 | 52.1945 | 50 | 52.2185 | 52.1945 | 0 | 52.2185 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43.6927 | 43.6927 | 100.8559 | 1 | PROCESSED | 57552.0261226852 | 2016-06-13 00:37:37 | 55741 | 2011-06-29 00:00:00 | 55375.7594907407 | 2010-06-28 18:13:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505055010/ | Quick Look | ![]() |
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353 | HD110432 | 190.599 | -63.0744 | 189.861553 | -62.800339 | 224.074847 | -51.705731 | 301.908501 | -0.22062002 | 344.9423 | 54718.9065740741 | 2008-09-09 21:45:28 | 54719.7050231482 | 2008-09-10 16:55:14 | 403002010 | 25.3332 | 25 | 25.3332 | 25.3332 | 0 | 25.3332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.3436 | 21.3436 | 68.9779 | 0 | PROCESSED | 57543.8037615741 | 2016-06-04 19:17:25 | 55148 | 2009-11-13 00:00:00 | 54780.4451736111 | 2008-11-10 10:41:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUNICHIRO MIURA | JAP | 3 | AO3 | SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403002010/ | Quick Look | ![]() |
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354 | BLOWOUT SHELL 2 | 312.2035 | 28.7297 | 311.67582 | 28.543644 | 325.497444 | 44.382569 | 72.14669544 | -9.39669734 | 48.0881 | 55361.263599537 | 2010-06-14 06:19:35 | 55362.5155439815 | 2010-06-15 12:22:23 | 505056010 | 52.0698 | 50 | 52.0698 | 52.0698 | 0 | 52.0698 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0827 | 46.0827 | 108.1558 | 1 | PROCESSED | 57552.3493634259 | 2016-06-13 08:23:05 | 55741 | 2011-06-29 00:00:00 | 55375.7627893518 | 2010-06-28 18:18:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505056010/ | Quick Look | ![]() |
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355 | HE FOCUSING CONE | 49.5928 | 10.9507 | 48.911727 | 10.768982 | 50.111751 | -7.072007 | 170.97872575 | -37.85410489 | 253.7002 | 55591.1307291667 | 2011-01-30 03:08:15 | 55593.7710763889 | 2011-02-01 18:30:21 | 505062010 | 100.1678 | 100 | 100.1678 | 100.1678 | 0 | 100.1678 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.7852 | 82.7852 | 228.1037 | 2 | PROCESSED | 57600.8639351852 | 2016-07-31 20:44:04 | 55973 | 2012-02-16 00:00:00 | 55607.305462963 | 2011-02-15 07:19:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI YOSHITAKE | JAP | 5 | AO5 | OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505062010/ | Quick Look | ![]() |
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356 | BD+43 3654 | 308.4185 | 44.0658 | 307.988834 | 43.893641 | 331.745866 | 59.550103 | 82.48241574 | 2.36274642 | 104.8287 | 55655.0785416667 | 2011-04-04 01:53:06 | 55657.0925231482 | 2011-04-06 02:13:14 | 506004010 | 97.0478 | 100 | 98.9638 | 97.0478 | 0 | 98.9638 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 88.9256 | 88.9256 | 173.9877 | 0 | PROCESSED | 57601.4465972222 | 2016-08-01 10:43:06 | 56037 | 2012-04-20 00:00:00 | 55670.3073842593 | 2011-04-19 07:22:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF NON-THERMAL EMISSION FROM A BOW SHOCK REGION OF A RUNAWAY STAR, BD+43 3654 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506004010/ | Quick Look | ![]() |
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357 | JUPITER | 28.9811 | 10.6021 | 28.315769 | 10.357786 | 30.678261 | -1.183373 | 147.5984875 | -49.15640747 | 249.1843 | 55937.2038773148 | 2012-01-11 04:53:35 | 55938.208599537 | 2012-01-12 05:00:23 | 506006030 | 34.8942 | 160 | 34.9022 | 34.9102 | 0 | 34.8942 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.2081 | 32.2081 | 86.7918 | 2 | PROCESSED | 57604.3101273148 | 2016-08-04 07:26:35 | 56319 | 2013-01-27 00:00:00 | 55952.170787037 | 2012-01-26 04:05:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006030/ | Quick Look | ![]() |
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358 | CYGNUS LOOP W-B-S | 311.1967 | 30.3719 | 310.678738 | 30.189494 | 325.222144 | 46.233696 | 72.9110541 | -7.69596159 | 71.021 | 55693.7715277778 | 2011-05-12 18:31:00 | 55694.9794212963 | 2011-05-13 23:30:22 | 506008010 | 55.6499 | 56 | 55.6499 | 55.6499 | 0 | 55.6499 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.8516 | 49.8516 | 104.3259 | 1 | PROCESSED | 57602.0472916667 | 2016-08-02 01:08:06 | 56072 | 2012-05-25 00:00:00 | 55705.1847800926 | 2011-05-24 04:26:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 6 | AO6 | HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506008010/ | Quick Look | ![]() |
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359 | HESSJ1857-B | 284.5485 | 2.7494 | 283.920534 | 2.680934 | 286.113501 | 25.379812 | 36.14879968 | -0.24805898 | 252.48 | 55866.7917592593 | 2011-11-01 19:00:08 | 55867.6946990741 | 2011-11-02 16:40:22 | 506020010 | 40.6869 | 40 | 40.6869 | 40.6949 | 0 | 40.6949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.0513 | 40.0513 | 78.0119 | 0 | PROCESSED | 57603.6841435185 | 2016-08-03 16:25:10 | 56246 | 2012-11-15 00:00:00 | 55879.1725 | 2011-11-14 04:08:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506020010/ | Quick Look | ![]() |
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360 | NGC 7618 | 349.8326 | 42.9144 | 349.23867 | 42.640678 | 11.92237 | 42.546584 | 105.51742003 | -16.82119292 | 269.9991 | 55911.4056828704 | 2011-12-16 09:44:11 | 55913.6161458333 | 2011-12-18 14:47:15 | 506027010 | 101.1772 | 100 | 101.1852 | 101.1772 | 0 | 101.1852 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.774 | 95.774 | 190.9399 | 0 | PROCESSED | 57604.196712963 | 2016-08-04 04:43:16 | 56289 | 2012-12-28 00:00:00 | 55922.1112847222 | 2011-12-27 02:40:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUHIRO HAYASHI | JAP | 6 | AO6 | OBSERVATION OF NEARBY MERGING GALAXY GROUP NGC 7618 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506027010/ | Quick Look | ![]() |
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361 | FERMI_BUBBLE_N2 | 234.4045 | 4.1242 | 233.780349 | 4.287466 | 230.936286 | 22.866796 | 10.25580888 | 44.20015183 | 287.5 | 56145.3990740741 | 2012-08-06 09:34:40 | 56145.971099537 | 2012-08-06 23:18:23 | 507002010 | 22.491 | 20 | 22.491 | 22.491 | 0 | 22.491 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.5 | 22.5 | 49.4059 | 0 | PROCESSED | 57606.7805555556 | 2016-08-06 18:44:00 | 56630 | 2013-12-04 00:00:00 | 56264.5602662037 | 2012-12-03 13:26:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507002010/ | Quick Look | ![]() |
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362 | FERMI_BUBBLE_N3 | 234.0339 | 6.0902 | 233.417441 | 6.254904 | 230.000126 | 24.67426 | 12.27048516 | 45.60209416 | 287.4996 | 56145.9724537037 | 2012-08-06 23:20:20 | 56146.4377893518 | 2012-08-07 10:30:25 | 507003010 | 22.4846 | 20 | 22.4846 | 22.5086 | 0 | 22.4926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.836 | 19.836 | 40.1959 | 0 | PROCESSED | 57606.7866782407 | 2016-08-06 18:52:49 | 56535 | 2013-08-31 00:00:00 | 56169.009837963 | 2012-08-30 00:14:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507003010/ | Quick Look | ![]() |
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363 | FERMI_BUBBLE_N6 | 233.4001 | 9.0706 | 232.795243 | 9.23775 | 228.456067 | 27.38567 | 15.47217439 | 47.71191257 | 287.5008 | 56147.4330324074 | 2012-08-08 10:23:34 | 56147.9606134259 | 2012-08-08 23:03:17 | 507006010 | 20.607 | 20 | 20.607 | 20.6246 | 0 | 20.619 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.3045 | 20.3045 | 45.58 | 0 | PROCESSED | 57606.8039467593 | 2016-08-06 19:17:41 | 56626 | 2013-11-30 00:00:00 | 56260.4951851852 | 2012-11-29 11:53:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507006010/ | Quick Look | ![]() |
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364 | FERMI_BUBBLE_S6 | 326.677 | -46.8481 | 325.870677 | -47.079705 | 311.980005 | -31.325121 | 351.64382858 | -48.94656928 | 44.0056 | 56037.1166087963 | 2012-04-20 02:47:55 | 56037.6009027778 | 2012-04-20 14:25:18 | 507014010 | 19.6439 | 20 | 19.6519 | 19.6439 | 0 | 19.6599 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.1827 | 14.1827 | 41.8399 | 1 | PROCESSED | 57605.2222916667 | 2016-08-05 05:20:06 | 56420 | 2013-05-08 00:00:00 | 56054.1845833333 | 2012-05-07 04:25:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507014010/ | Quick Look | ![]() |
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365 | GC_SOUTH_2 | 268.3751 | -29.7084 | 267.575601 | -29.69856 | 268.570633 | -6.275404 | 0.22024801 | -1.8703349 | 273.7998 | 56192.7899421296 | 2012-09-22 18:57:31 | 56194.081412037 | 2012-09-24 01:57:14 | 507029010 | 52.4469 | 50 | 52.4629 | 52.4469 | 0 | 52.4549 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45.2307 | 45.2307 | 111.5759 | 1 | PROCESSED | 57607.1634259259 | 2016-08-07 03:55:20 | 56689 | 2014-02-01 00:00:00 | 56321.5121875 | 2013-01-29 12:17:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507029010/ | Quick Look | ![]() |
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366 | G298.6-0.0 | 183.3873 | -62.6234 | 182.718198 | -62.34531 | 219.474963 | -53.500968 | 298.59191859 | -0.0713547 | 133.8706 | 56341.7597222222 | 2013-02-18 18:14:00 | 56342.6981712963 | 2013-02-19 16:45:22 | 507037020 | 39.7247 | 35 | 39.7247 | 39.7247 | 0 | 39.7247 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 36.2621 | 36.2621 | 81.0699 | 0 | PROCESSED | 57610.644849537 | 2016-08-10 15:28:35 | 56721 | 2014-03-05 00:00:00 | 56362.8029861111 | 2013-03-11 19:16:18 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037020/ | Quick Look | ![]() |
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367 | MSH15-56_SW | 238.0528 | -56.3239 | 237.060386 | -56.174494 | 248.949341 | -35.191477 | 326.11105465 | -1.81589779 | 86.2015 | 56326.3325 | 2013-02-03 07:58:48 | 56327.8577314815 | 2013-02-04 20:35:08 | 507039010 | 86.0122 | 100 | 86.0122 | 86.0122 | 0 | 86.0122 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.3912 | 88.3912 | 131.7719 | 2 | PROCESSED | 57610.534849537 | 2016-08-10 12:50:11 | 56714 | 2014-02-26 00:00:00 | 56345.5312847222 | 2013-02-22 12:45:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOICHI YATSU | JAP | 7 | AO7 | A STUDY OF PARTICLE ACCELERATION BASED ON THE THERMAL PLASMA BEHIND THE SHOCK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507039010/ | Quick Look | ![]() |
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368 | VELA PWN N1 | 128.8231 | -44.9507 | 128.399065 | -44.776941 | 153.1311 | -60.168643 | 263.36545364 | -2.659461 | 324.0013 | 56108.9552083333 | 2012-06-30 22:55:30 | 56109.3487962963 | 2012-07-01 08:22:16 | 507048010 | 17.8014 | 15 | 17.8094 | 17.8014 | 0 | 17.8094 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.2047 | 19.2047 | 33.9999 | 1 | PROCESSED | 57606.5230439815 | 2016-08-06 12:33:11 | 56592 | 2013-10-27 00:00:00 | 56226.6327083333 | 2012-10-26 15:11:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507048010/ | Quick Look | ![]() |
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369 | VELA PWN N2 | 128.845 | -44.6374 | 128.418547 | -44.463562 | 152.844801 | -59.889474 | 263.12360018 | -2.45940596 | 325.4993 | 56109.3500115741 | 2012-07-01 08:24:01 | 56109.7210185185 | 2012-07-01 17:18:16 | 507049010 | 18.4118 | 15 | 18.4198 | 18.4118 | 0 | 18.4198 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.7623 | 18.7623 | 32.024 | 0 | PROCESSED | 57606.5242939815 | 2016-08-06 12:34:59 | 56493 | 2013-07-20 00:00:00 | 56127.0941319444 | 2012-07-19 02:15:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507049010/ | Quick Look | ![]() |
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370 | VELA PWN N3 | 128.8419 | -44.3423 | 128.413265 | -44.168478 | 152.550585 | -59.63427 | 262.88578161 | -2.28439697 | 325.9006 | 56109.7216782407 | 2012-07-01 17:19:13 | 56110.0161574074 | 2012-07-02 00:23:16 | 507050010 | 12.3984 | 15 | 12.3984 | 12.3984 | 0 | 12.3984 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2454 | 13.2454 | 25.4319 | 1 | PROCESSED | 57606.5311805556 | 2016-08-06 12:44:54 | 56493 | 2013-07-20 00:00:00 | 56127.104849537 | 2012-07-19 02:30:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507050010/ | Quick Look | ![]() |
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371 | VELA PWN N6 | 128.8205 | -43.4604 | 128.385504 | -43.286672 | 151.68228 | -58.872108 | 262.17003306 | -1.76832201 | 122.021 | 56258.4379050926 | 2012-11-27 10:30:35 | 56258.805625 | 2012-11-27 19:20:06 | 507053010 | 15.3401 | 15 | 15.3481 | 15.3481 | 0 | 15.3401 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.9013 | 13.9013 | 31.7599 | 0 | PROCESSED | 57608.0978819444 | 2016-08-08 02:20:57 | 56641 | 2013-12-15 00:00:00 | 56275.6586111111 | 2012-12-14 15:48:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507053010/ | Quick Look | ![]() |
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372 | 3C 397 | 286.9092 | 7.1226 | 286.301586 | 7.04303 | 289.342559 | 29.434869 | 41.11337729 | -0.33398163 | 251.9939 | 56595.6848611111 | 2013-10-30 16:26:12 | 56597.9106828704 | 2013-11-01 21:51:23 | 508001010 | 103.5157 | 100 | 103.5157 | 103.5157 | 0 | 103.5157 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.6753 | 98.6753 | 192.2937 | 2 | PROCESSED | 57613.2313425926 | 2016-08-13 05:33:08 | 57012 | 2014-12-21 00:00:00 | 56645.6863541667 | 2013-12-19 16:28:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080011 | 3C 397 is a Galactic Supernova remnant (SNR) ,whose X-ray spectrum has prominent Fe K line emission. We analyzed Suzaku AO5 data, it resulted in finding of Fe Lya Line. This is a symptomatic of over-ionized (recombining) plasma. On the other hand, the Fe K line center indicates under-ionized (ionizing) plasma. This means that 3C 397 may consisting of two opposite type of plasma: ionizing and recombining. Such a strange state of plasma is not discovered in any SNR.This discovery will be a key to uncovering a mystery of the origin of recombining plasma. However, we still not detect Fe Radiative recombination continuum (RRC),which is a evidence of recombining plasma. To detect the Fe RRC, we propose 150 ks additional observation of 3C 397. | GALACTIC DIFFUSE EMISSION | 5 | C | RYUSUKE SUGAWARA | JAP | 8 | AO8 | THE INDICATION OF RECOMBINING PLASMA COEXISTING WITH IONIZING PLASMA IN 3C 397 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508001010/ | Quick Look | ![]() |
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373 | W44_EAST | 284.1459 | 1.2991 | 283.51111 | 1.232548 | 285.500202 | 23.981686 | 34.67473844 | -0.5521979 | 254.9985 | 56583.3375231482 | 2013-10-18 08:06:02 | 56584.8897337963 | 2013-10-19 21:21:13 | 508004010 | 58.2965 | 60 | 58.3045 | 58.2965 | 0 | 58.3149 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 52.7276 | 52.7276 | 134.0958 | 2 | PROCESSED | 57613.0782407407 | 2016-08-13 01:52:40 | 57004 | 2014-12-13 00:00:00 | 56637.6520949074 | 2013-12-11 15:39:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508004010/ | Quick Look | ![]() |
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374 | NW_SRC | 221.7499 | -1.3162 | 221.105287 | -1.10746 | 219.72393 | 14.106437 | 351.9522425 | 50.22344256 | 289.0003 | 56499.3402430556 | 2013-07-26 08:09:57 | 56499.8412037037 | 2013-07-26 20:11:20 | 508007010 | 23.554 | 20 | 23.554 | 23.5554 | 0 | 23.554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.103 | 24.103 | 43.274 | 0 | PROCESSED | 57612.0357986111 | 2016-08-12 00:51:33 | 56955 | 2014-10-25 00:00:00 | 56587.4553819444 | 2013-10-22 10:55:45 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508007010/ | Quick Look | ![]() |
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375 | SE_SRC | 287.3947 | -27.2493 | 286.61657 | -27.330736 | 285.457559 | -4.737737 | 9.97288902 | -15.74410072 | 84.5985 | 56404.7026967593 | 2013-04-22 16:51:53 | 56405.330775463 | 2013-04-23 07:56:19 | 508009010 | 20.3287 | 20 | 20.3287 | 20.3287 | 0 | 20.3287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.5938 | 17.5938 | 54.2639 | 1 | PROCESSED | 57611.1595833333 | 2016-08-11 03:49:48 | 56792 | 2014-05-15 00:00:00 | 56425.5555092593 | 2013-05-13 13:19:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508009010/ | Quick Look | ![]() |
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376 | SE_BGD | 288.7458 | -25.773 | 287.977196 | -25.860714 | 286.843449 | -3.422342 | 11.87589948 | -16.28754896 | 81.8427 | 56405.3324537037 | 2013-04-23 07:58:44 | 56405.8329050926 | 2013-04-23 19:59:23 | 508010010 | 20.9653 | 20 | 20.9693 | 20.9653 | 0 | 20.9733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.7626 | 18.7626 | 43.234 | 0 | PROCESSED | 57618.7907291667 | 2016-08-18 18:58:39 | 56792 | 2014-05-15 00:00:00 | 56425.5426851852 | 2013-05-13 13:01:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508010010/ | Quick Look | ![]() |
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377 | HESS J1534-571 2 | 233.1754 | -57.1 | 232.193457 | -56.931173 | 246.039407 | -36.679353 | 323.50919975 | -0.81659232 | 295.9986 | 56544.0219212963 | 2013-09-09 00:31:34 | 56544.6695949074 | 2013-09-09 16:04:13 | 508014010 | 38.9186 | 40 | 38.9426 | 38.9186 | 0 | 38.9506 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.8565 | 36.8565 | 55.9539 | 0 | PROCESSED | 57612.5722916667 | 2016-08-12 13:44:06 | 56990 | 2014-11-29 00:00:00 | 56622.6062268518 | 2013-11-26 14:32:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | 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 J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target 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 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508014010/ | Quick Look | ![]() |
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378 | HESSJ1858-B | 284.4324 | 2.2013 | 283.801854 | 2.133387 | 285.919657 | 24.847772 | 35.60820996 | -0.39516335 | 251.7997 | 56593.9763310185 | 2013-10-28 23:25:55 | 56595.1313541667 | 2013-10-30 03:09:09 | 508022010 | 52.595 | 50 | 52.619 | 52.611 | 0 | 52.595 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49.9941 | 49.9941 | 99.7858 | 2 | PROCESSED | 57613.1665393518 | 2016-08-13 03:59:49 | 56975 | 2014-11-14 00:00:00 | 56608.7129166667 | 2013-11-12 17:06:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080052 | 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 | B | HIRONORI MATSUMOTO | JAP | 8 | AO8 | DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508022010/ | Quick Look | ![]() |
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379 | JUPITER | 104.0103 | 23.0994 | 103.254149 | 23.165009 | 102.868934 | 0.282188 | 192.60135744 | 11.26438783 | 264.454 | 56763.7225 | 2014-04-16 17:20:24 | 56764.0627083333 | 2014-04-17 01:30:18 | 508023060 | 8.8696 | 160 | 8.8776 | 8.8696 | 0 | 8.8856 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9524652778 | 2016-08-14 22:51:33 | 57212 | 2015-07-09 00:00:00 | 56846.5928472222 | 2014-07-08 14:13:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023060/ | Quick Look | ![]() |
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380 | JUPITER | 104.4171 | 23.0664 | 103.66133 | 23.133929 | 103.244601 | 0.2859 | 192.79210183 | 11.59024455 | 264.5983 | 56766.7815972222 | 2014-04-19 18:45:30 | 56767.1147916667 | 2014-04-20 02:45:18 | 508023100 | 9.3759 | 160 | 9.3839 | 9.3919 | 0 | 9.3759 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9623263889 | 2016-08-14 23:05:45 | 57212 | 2015-07-09 00:00:00 | 56782.4942824074 | 2014-05-05 11:51:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023100/ | Quick Look | ![]() |
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381 | VELA JR WEST3 | 131.773 | -46.2743 | 131.349543 | -46.08957 | 158.06279 | -60.232297 | 265.67717372 | -1.83917649 | 116.21 | 56620.0804861111 | 2013-11-24 01:55:54 | 56620.7320949074 | 2013-11-24 17:34:13 | 508038010 | 34.9611 | 30 | 34.9911 | 34.9611 | 0 | 34.9611 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.4434 | 40.4434 | 56.2959 | 0 | PROCESSED | 57613.4017708333 | 2016-08-13 09:38:33 | 56995 | 2014-12-04 00:00:00 | 56629.6399421296 | 2013-12-03 15:21:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDETOSHI SANO | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508038010/ | Quick Look | ![]() |
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382 | CIZA J1358.9-4750 | 209.651 | -47.7758 | 208.860998 | -47.532845 | 225.745985 | -33.169178 | 314.45332941 | 13.58776424 | 104.5762 | 56313.755 | 2013-01-21 18:07:12 | 56315.4835648148 | 2013-01-23 11:36:20 | 807037010 | 61.6899 | 60 | 61.7299 | 61.6899 | 0 | 61.731 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.9497 | 58.9497 | 149.3318 | 1 | PROCESSED | 57608.595162037 | 2016-08-08 14:17:02 | 56718 | 2014-03-02 00:00:00 | 56351.6358680556 | 2013-02-28 15:15:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070101 | We propose a Suzaku observation of newly found merging cluster in the Zone of Avoidance, CIZA J1358.9-4750. The cluster has double core, and apparently in an early phase of merging. Targets with this phase is rare. With this observation, we want to obtain the temperature map of the bridge region and identify the existence of heating, to understand the merging phase of this cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TERUKAZU NISHIDA | JAP | 7 | AO7 | OBSERVATION OF THE NEWLY DISCOVERED MERGING CLUSTER NEAR THE GALACTIC DISC; CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807037010/ | Quick Look | ![]() |
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383 | VELA PWN W5 | 126.0444 | -45.2057 | 125.630533 | -45.042674 | 149.898743 | -61.36183 | 262.42223435 | -4.39970467 | 94.9992 | 56591.8819560185 | 2013-10-26 21:10:01 | 56592.3202777778 | 2013-10-27 07:41:12 | 508046010 | 15.8569 | 15 | 15.8729 | 15.8569 | 0 | 15.8809 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.7358 | 12.7358 | 37.8639 | 0 | PROCESSED | 57613.1438657407 | 2016-08-13 03:27:10 | 57009 | 2014-12-18 00:00:00 | 56643.6567824074 | 2013-12-17 15:45:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, 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 western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508046010/ | Quick Look | ![]() |
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384 | VELA PWN W6 | 125.6171 | -45.2116 | 125.2045 | -45.05026 | 149.354915 | -61.513653 | 262.25511101 | -4.65051542 | 95.0008 | 56592.3208912037 | 2013-10-27 07:42:05 | 56592.8209722222 | 2013-10-27 19:42:12 | 508047010 | 17.2398 | 15 | 17.2478 | 17.2398 | 0 | 17.2398 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.2299 | 16.2299 | 43.1999 | 0 | PROCESSED | 57613.1284606482 | 2016-08-13 03:04:59 | 57011 | 2014-12-20 00:00:00 | 56645.5849421296 | 2013-12-19 14:02:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, 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 western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508047010/ | Quick Look | ![]() |
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385 | W49B | 287.7839 | 9.1153 | 287.185543 | 9.031646 | 290.654077 | 31.289696 | 43.2808507 | -0.18308455 | 82.0062 | 57122.7467013889 | 2015-04-10 17:55:15 | 57125.7127777778 | 2015-04-13 17:06:24 | 509001010 | 81.4763 | 400 | 81.4763 | 113.9098 | 0 | 113.9162 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.986724537 | 2016-08-17 23:40:53 | 56748 | 2014-04-01 00:00:00 | 57136.5735300926 | 2015-04-24 13:45:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001010/ | Quick Look | ![]() |
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386 | W49B | 287.7843 | 9.1147 | 287.18594 | 9.031044 | 290.654435 | 31.289046 | 43.28050127 | -0.18371216 | 82.0064 | 57128.6891203704 | 2015-04-16 16:32:20 | 57131.6619328704 | 2015-04-19 15:53:11 | 509001030 | 100.9959 | 400 | 100.9959 | 106.4207 | 0 | 106.3967 | 4 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0043518518 | 2016-08-18 00:06:16 | 56748 | 2014-04-01 00:00:00 | 57220.3809722222 | 2015-07-17 09:08:36 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001030/ | Quick Look | ![]() |
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387 | G1.9+0.3 | 267.1939 | -27.1714 | 266.410492 | -27.155866 | 267.488865 | -3.754805 | 1.87009843 | 0.31910459 | 104.2133 | 57099.6072569445 | 2015-03-18 14:34:27 | 57101.7854976852 | 2015-03-20 18:51:07 | 509003010 | 92.0313 | 100 | 92.0313 | 97.0859 | 0 | 97.0699 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8499189815 | 2016-08-17 20:23:53 | 57527 | 2016-05-19 00:00:00 | 57160.6404861111 | 2015-05-18 15:22:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090030 | We propose a Suzaku observations of the youngest supernova remnant (SNR) G1.9+0.3. We aim to detect flux increase and spectral hardening of synchrotron X-rays since 2011 when the previous Suzaku observation was performed. The measurement should provide us with important information about the maximum acceleration energy attainable by diffusive shock acceleration in SNRs. Suzaku XIS is the most suitable detector since it has the large effective area even in the hard band up to 10 keV. If X-ray flux increase is significantly larger than that measured in the radio band, we can conclude that maximum acceleration energy is becoming higher at present. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAAKI TANAKA | YASUNOBU UCHIYAMA | JAP | 9 | AO9 | MEASUREMENT OF TIME VARIABILITY OF SYNCHROTRON X-RAYS FROM THE YOUNGEST SUPERNOVA REMNANT G1.9+0.3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509003010/ | Quick Look | ![]() |
388 | VELA PWN GEV5 | 128.1777 | -45.5057 | 127.759875 | -45.334391 | 152.900781 | -60.876983 | 263.54099229 | -3.35509044 | 120.3003 | 56987.5594328704 | 2014-11-26 13:25:35 | 56987.9009490741 | 2014-11-26 21:37:22 | 509015010 | 16.1889 | 15 | 16.1889 | 16.2127 | 0 | 16.1969 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.822025463 | 2016-08-16 19:43:43 | 57368 | 2015-12-12 00:00:00 | 57002.4333564815 | 2014-12-11 10:24:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509015010/ | Quick Look | ![]() |
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389 | G166.0+4.3_SE | 81.6718 | 42.6436 | 80.778042 | 42.601144 | 83.516564 | 19.390604 | 166.37682371 | 4.1455421 | 266.8508 | 57094.5870486111 | 2015-03-13 14:05:21 | 57095.305 | 2015-03-14 07:19:12 | 509024020 | 26.0329 | 27 | 26.0329 | 27.3929 | 0 | 27.3929 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.780625 | 2016-08-17 18:44:06 | 57478 | 2016-03-31 00:00:00 | 57108.4092939815 | 2015-03-27 09:49:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024020/ | Quick Look | ![]() |
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390 | CIZA J1358.9-4750_NE | 209.8984 | -47.6059 | 209.108141 | -47.363535 | 225.843523 | -32.945776 | 314.66509294 | 13.70714471 | 293.0012 | 56879.8864467593 | 2014-08-10 21:16:29 | 56880.8606481482 | 2014-08-11 20:39:20 | 509025010 | 40.2748 | 40 | 40.2828 | 40.2828 | 0 | 40.2748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.7468 | 7.7468 | 19.736 | 0 | PROCESSED | 57616.4833333333 | 2016-08-16 11:36:00 | 57270 | 2015-09-05 00:00:00 | 56902.1990972222 | 2014-09-02 04:46:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509025010/ | Quick Look | ![]() |
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391 | VERJ2019_P2 | 305.0647 | 36.873 | 304.594845 | 36.714007 | 321.75914 | 54.196272 | 75.14540231 | 0.26023113 | 251.4317 | 56970.0347453704 | 2014-11-09 00:50:02 | 56971.0419097222 | 2014-11-10 01:00:21 | 509029010 | 40.4941 | 40 | 40.4941 | 40.5021 | 0 | 40.5021 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7544791667 | 2016-08-16 18:06:27 | 57436 | 2016-02-18 00:00:00 | 57071.4171527778 | 2015-02-18 10:00:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090120 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 9 | AO9 | SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509029010/ | Quick Look | ![]() |
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392 | CENTAURUS CLUSTER N | 192.2138 | -40.9141 | 191.523743 | -40.64159 | 208.863601 | -32.495572 | 302.40583252 | 21.95501054 | 115.2417 | 55961.0060763889 | 2012-02-04 00:08:45 | 55962.6667939815 | 2012-02-05 16:00:11 | 806011010 | 54.0496 | 50 | 54.0496 | 54.0496 | 0 | 54.0496 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.6109 | 48.6109 | 143.4758 | 2 | PROCESSED | 57604.5565972222 | 2016-08-04 13:21:30 | 56360 | 2013-03-09 00:00:00 | 55992.1577546296 | 2012-03-06 03:47:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060035 | We propose to observe two fields at 0.1-0.2r180 of the Centaurus cluster for total 90 ks exposures with Suzaku. The purpose of the observations is to determine Mg and Fe distributions of the intracluster medium up to 0.2 r180 and to study origin of metals in the intracluster medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 6 | AO6 | MG AND FE ABUNDANCES OF THE ICM IN THE CENTAURUS CLUSTER UP TO 0.2R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806011010/ | Quick Look | ![]() |
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393 | PKS 0558-504 | 89.9335 | -50.4395 | 89.62999 | -50.44058 | 89.864093 | -73.881363 | 257.95137808 | -28.57681508 | 212.4401 | 54121.9091203704 | 2007-01-21 21:49:08 | 54122.3529976852 | 2007-01-22 08:28:19 | 701011050 | 19.5154 | 20 | 19.5314 | 19.5154 | 0 | 19.5314 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.1236 | 16.1236 | 38.312 | 0 | PROCESSED | 57536.8983217593 | 2016-05-28 21:33:35 | 54735 | 2008-09-26 00:00:00 | 54137.0453240741 | 2007-02-06 01:05:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011050/ | Quick Look | ![]() |
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394 | SWIFT J0350.1-5019 | 57.6662 | -50.2998 | 57.309175 | -50.449494 | 28.967165 | -67.019674 | 259.65657878 | -48.95336771 | 180.7044 | 54062.0888078704 | 2006-11-23 02:07:53 | 54062.5647453704 | 2006-11-23 13:33:14 | 701017020 | 19.271 | 23 | 19.271 | 19.271 | 0 | 19.271 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.74 | 16.74 | 41.097 | 0 | PROCESSED | 57536.1549768518 | 2016-05-28 03:43:10 | 54750 | 2008-10-11 00:00:00 | 54088.5939583333 | 2006-12-19 14:15:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017020/ | Quick Look | ![]() |
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395 | OJ 287 FLARE | 133.7115 | 20.1695 | 132.996174 | 20.360602 | 130.493887 | 2.661227 | 206.74425687 | 35.84822718 | 98.7868 | 54411.475 | 2007-11-07 11:24:00 | 54413.896099537 | 2007-11-09 21:30:23 | 702008010 | 112.044 | 100 | 112.052 | 112.06 | 0 | 112.044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.9238 | 102.9238 | 209.1519 | 3 | PROCESSED | 57540.5116087963 | 2016-06-01 12:16:43 | 54791 | 2008-11-21 00:00:00 | 54423.3848032407 | 2007-11-19 09:14:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 2 | AO2-TOO | MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702008010/ | Quick Look | ![]() |
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396 | IC 3639 | 190.1935 | -36.8078 | 189.517353 | -36.533453 | 205.04698 | -29.556314 | 300.55692841 | 26.01476797 | 293.9494 | 54293.1966435185 | 2007-07-12 04:43:10 | 54294.4133564815 | 2007-07-13 09:55:14 | 702011010 | 53.3912 | 50 | 53.3912 | 53.3912 | 0 | 53.3912 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.4852 | 48.4852 | 105.11 | 1 | PROCESSED | 57539.1904050926 | 2016-05-31 04:34:11 | 54709 | 2008-08-31 00:00:00 | 54339.5331365741 | 2007-08-27 12:47:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702011010/ | Quick Look | ![]() |
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397 | PKS2126-15 | 322.2988 | -15.6437 | 321.609655 | -15.862975 | 319.629627 | -0.752825 | 35.92993079 | -41.86589251 | 72.3882 | 54576.0912384259 | 2008-04-20 02:11:23 | 54578.4238310185 | 2008-04-22 10:10:19 | 703001010 | 81.9214 | 80 | 81.9214 | 81.9364 | 0 | 81.9454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.5414 | 71.5414 | 201.5279 | 3 | PROCESSED | 57542.3941087963 | 2016-06-03 09:27:31 | 54961 | 2009-05-10 00:00:00 | 54594.3427777778 | 2008-05-08 08:13:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 3 | AO3 | UNVEILING NEW-TYPE "PRIMITIVE" BLAZARS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703001010/ | Quick Look | ![]() |
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398 | SWIFT J2009.0-6103 | 302.158 | -61.0495 | 301.087298 | -61.195509 | 289.575526 | -39.777943 | 335.84532046 | -32.77756596 | 73.0628 | 54563.6948148148 | 2008-04-07 16:40:32 | 54564.600775463 | 2008-04-08 14:25:07 | 703015010 | 43.7268 | 40 | 43.7268 | 43.7268 | 0 | 43.7268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.1996 | 36.1996 | 78.268 | 1 | PROCESSED | 57542.2661342593 | 2016-06-03 06:23:14 | 54953 | 2009-05-02 00:00:00 | 54580.2454976852 | 2008-04-24 05:53:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703015010/ | Quick Look | ![]() |
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399 | 1739+518 | 264.9784 | 52.1719 | 264.694846 | 52.196929 | 257.680013 | 75.396251 | 79.52646168 | 31.85370007 | 22.9152 | 54985.7571759259 | 2009-06-03 18:10:20 | 54986.3641087963 | 2009-06-04 08:44:19 | 704008010 | 22.4868 | 20 | 22.4948 | 22.4948 | 0 | 22.4868 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.2378 | 28.2378 | 52.4319 | 0 | PROCESSED | 57547.4536458333 | 2016-06-08 10:53:15 | 55367 | 2010-06-20 00:00:00 | 54998.1968634259 | 2009-06-16 04:43:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704008010/ | Quick Look | ![]() |
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400 | CENTAURUS_A | 201.3322 | -43.0688 | 200.598815 | -42.808768 | 217.137097 | -31.383435 | 309.48334217 | 19.37141452 | 298.7164 | 55048.3079513889 | 2009-08-05 07:23:27 | 55049.7029398148 | 2009-08-06 16:52:14 | 704018020 | 51.2787 | 50 | 51.2787 | 51.2947 | 0 | 51.2867 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7332 | 43.7332 | 120.5059 | 1 | PROCESSED | 57548.0839699074 | 2016-06-09 02:00:55 | 55430 | 2010-08-22 00:00:00 | 55062.3520023148 | 2009-08-19 08:26:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018020/ | Quick Look | ![]() |
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401 | PBC J0216.1+5124 | 34.0954 | 51.5104 | 33.261431 | 51.278784 | 50.779826 | 35.406451 | 136.13174863 | -9.17115539 | 78.3815 | 55421.9728356482 | 2010-08-13 23:20:53 | 55423.4168171296 | 2010-08-15 10:00:13 | 705006010 | 72.7733 | 80 | 72.7964 | 72.7733 | 0 | 72.7964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.5582 | 73.5582 | 124.7258 | 3 | PROCESSED | 57553.114375 | 2016-06-14 02:44:42 | 55804 | 2011-08-31 00:00:00 | 55435.2980092593 | 2010-08-27 07:09:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 5 | AO5 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705006010/ | Quick Look | ![]() |
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402 | EMS1164 | 265.9438 | -76.3446 | 264.162094 | -76.320567 | 268.39939 | -52.925114 | 317.07818058 | -22.45515073 | 114.3984 | 55300.0111689815 | 2010-04-14 00:16:05 | 55300.6980439815 | 2010-04-14 16:45:11 | 705013010 | 42.3783 | 40 | 42.3836 | 42.3783 | 0 | 42.389 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.0487 | 39.0487 | 59.3439 | 1 | PROCESSED | 57551.2223958333 | 2016-06-12 05:20:15 | 55675 | 2011-04-24 00:00:00 | 55309.1947453704 | 2010-04-23 04:40:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705013010/ | Quick Look | ![]() |
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403 | EMS1395 | 310.8148 | 17.1786 | 310.239098 | 16.997696 | 318.830842 | 33.961912 | 61.89528011 | -15.30299533 | 74.9546 | 55319.8076736111 | 2010-05-03 19:23:03 | 55320.4342476852 | 2010-05-04 10:25:19 | 705015010 | 23.3002 | 20 | 23.3002 | 23.3002 | 0 | 23.3002 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4944 | 19.4944 | 54.1299 | 0 | PROCESSED | 57551.3813773148 | 2016-06-12 09:09:11 | 55696 | 2011-05-15 00:00:00 | 55330.2005208333 | 2010-05-14 04:48:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705015010/ | Quick Look | ![]() |
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404 | MRK 509 | 311.0469 | -10.7401 | 310.365769 | -10.921688 | 310.545768 | 7.110758 | 35.95684044 | -29.86794514 | 252.3716 | 55521.595625 | 2010-11-21 14:17:42 | 55523.8155092593 | 2010-11-23 19:34:20 | 705025010 | 102.1205 | 100 | 102.1285 | 102.1285 | 0 | 102.1205 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.0625 | 92.0625 | 191.7697 | 0 | PROCESSED | 57554.2039930556 | 2016-06-15 04:53:45 | 55916 | 2011-12-21 00:00:00 | 55550.2628356482 | 2010-12-20 06:18:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROFUMI NODA | JAP | 5 | AO5 | VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705025010/ | Quick Look | ![]() |
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405 | NGC6251_LOBE_BGD2 | 245.2973 | 82.3586 | 246.565183 | 82.472103 | 101.108878 | 73.211894 | 115.82251183 | 31.60630628 | 26.9772 | 55667.4343981482 | 2011-04-16 10:25:32 | 55667.8230902778 | 2011-04-16 19:45:15 | 706005010 | 12.0103 | 20 | 12.0183 | 12.0103 | 0 | 12.0263 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.5851 | 17.5851 | 33.5759 | 0 | PROCESSED | 57601.5154976852 | 2016-08-01 12:22:19 | 56058 | 2012-05-11 00:00:00 | 55690.9834490741 | 2011-05-09 23:36:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005010/ | Quick Look | ![]() |
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406 | IC 4518A | 224.419 | -43.1269 | 223.597719 | -42.926611 | 234.851401 | -25.085272 | 326.11466585 | 13.99053707 | 102.9822 | 55959.1723263889 | 2012-02-02 04:08:09 | 55961.0002777778 | 2012-02-04 00:00:24 | 706012010 | 64.3986 | 60 | 64.3986 | 64.3986 | 0 | 64.3986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.2381 | 57.2381 | 157.9058 | 1 | PROCESSED | 57604.5692708333 | 2016-08-04 13:39:45 | 56434 | 2013-05-22 00:00:00 | 56068.6321064815 | 2012-05-21 15:10:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA HIRATA | 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 | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706012010/ | Quick Look | ![]() |
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407 | RX J1633+4718 | 248.3303 | 47.3072 | 247.970126 | 47.410772 | 228.761848 | 67.666439 | 73.53738657 | 42.62611906 | 329.4078 | 55743.8204050926 | 2011-07-01 19:41:23 | 55744.8460069444 | 2011-07-02 20:18:15 | 706027010 | 39.9916 | 40 | 39.9916 | 39.9916 | 0 | 39.9916 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.6531 | 39.6531 | 88.6059 | 1 | PROCESSED | 57602.4692013889 | 2016-08-02 11:15:39 | 56144 | 2012-08-05 00:00:00 | 55775.3057407407 | 2011-08-02 07:20:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027010/ | Quick Look | ![]() |
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408 | 3C 236 WEST LOBE | 151.329 | 34.9949 | 150.593371 | 35.23826 | 140.67974 | 21.703249 | 189.91194492 | 53.83302535 | 299.9981 | 56053.9465740741 | 2012-05-06 22:43:04 | 56055.7862384259 | 2012-05-08 18:52:11 | 707005010 | 83.9935 | 80 | 83.9935 | 83.9935 | 0 | 83.9935 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.4248 | 80.4248 | 158.9318 | 2 | PROCESSED | 57605.4100925926 | 2016-08-05 09:50:32 | 56436 | 2013-05-24 00:00:00 | 56070.2690856482 | 2012-05-23 06:27:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 7 | AO7 | INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707005010/ | Quick Look | ![]() |
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409 | 2FGL J0037.8+1238 | 9.4591 | 12.6426 | 8.808625 | 12.367737 | 13.671851 | 7.875917 | 117.75617703 | -50.09241086 | 67.2998 | 56108.005787037 | 2012-06-30 00:08:20 | 56108.9432523148 | 2012-06-30 22:38:17 | 707010010 | 28.6039 | 30 | 28.6039 | 28.6039 | 0 | 28.6039 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0977 | 30.0977 | 80.972 | 1 | PROCESSED | 57606.5224768518 | 2016-08-06 12:32:22 | 56493 | 2013-07-20 00:00:00 | 56127.1415625 | 2012-07-19 03:23:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707010010/ | Quick Look | ![]() |
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410 | NGC1365 | 53.4072 | -36.1471 | 52.929884 | -36.314043 | 36.805891 | -53.04754 | 237.96723255 | -54.59318142 | 57.2979 | 56125.3876273148 | 2012-07-17 09:18:11 | 56125.896087963 | 2012-07-17 21:30:22 | 707017030 | 26.7672 | 30 | 26.7672 | 26.7672 | 0 | 26.7672 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2112 | 25.2112 | 43.9239 | 1 | PROCESSED | 57606.6299537037 | 2016-08-06 15:07:08 | 56582 | 2013-10-17 00:00:00 | 56212.7663194444 | 2012-10-12 18:23:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017030/ | Quick Look | ![]() |
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411 | NGC 3516 | 166.6556 | 72.561 | 165.802341 | 72.831319 | 123.361761 | 57.969661 | 133.25565935 | 42.40250412 | 335.7404 | 56391.9675925926 | 2013-04-09 23:13:20 | 56393.0460185185 | 2013-04-11 01:06:16 | 708006010 | 51.386 | 50 | 51.402 | 51.386 | 0 | 51.402 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.1015 | 49.1015 | 93.1638 | 1 | PROCESSED | 57611.0515856482 | 2016-08-11 01:14:17 | 56383 | 2013-04-01 00:00:00 | 56421.6947106482 | 2013-05-09 16:40:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006010/ | Quick Look | ![]() |
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412 | NGC 3516 | 166.6684 | 72.5566 | 165.815394 | 72.826934 | 123.372761 | 57.969452 | 133.25443095 | 42.40827092 | 314.5458 | 56409.0119560185 | 2013-04-27 00:17:13 | 56409.446087963 | 2013-04-27 10:42:22 | 708006020 | 19.103 | 50 | 19.119 | 19.103 | 0 | 19.119 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2121 | 20.2121 | 30.7239 | 0 | PROCESSED | 57611.1744907407 | 2016-08-11 04:11:16 | 56383 | 2013-04-01 00:00:00 | 56457.6034375 | 2013-06-14 14:28:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006020/ | Quick Look | ![]() |
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413 | NGC 3516 | 166.6764 | 72.5574 | 165.823506 | 72.827743 | 123.374751 | 57.971749 | 133.25110438 | 42.40886909 | 307.603 | 56424.0155555556 | 2013-05-12 00:22:24 | 56425.1044328704 | 2013-05-13 02:30:23 | 708006030 | 50.4283 | 50 | 50.4283 | 50.4283 | 0 | 50.4283 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 57.2275 | 57.2275 | 94.076 | 0 | PROCESSED | 57611.3108680556 | 2016-08-11 07:27:39 | 56383 | 2013-04-01 00:00:00 | 56436.6511805556 | 2013-05-24 15:37:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006030/ | Quick Look | ![]() |
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414 | NGC6552 | 270.0757 | 66.6036 | 270.078264 | 66.603205 | 60.706525 | 89.950181 | 96.43339546 | 29.78135373 | 217.6129 | 56610.8399884259 | 2013-11-14 20:09:35 | 56613.0126851852 | 2013-11-17 00:18:16 | 708014010 | 105.7767 | 100 | 105.7767 | 105.7767 | 0 | 105.7767 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.2797 | 102.2797 | 187.7079 | 1 | PROCESSED | 57613.3907060185 | 2016-08-13 09:22:37 | 57019 | 2014-12-28 00:00:00 | 56653.7413078704 | 2013-12-27 17:47:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080092 | We propose to observe the interesting Seyfert 2 galaxy NGC6552, which has multi fluorescence lines in the X-ray band. There ara only three objects, including NGC6552, which has multi fluorescence lines in the X-ray band. We aim to detect emission lines finely and study the chemical evolution of the galaxy. We also aim measurements of hard X-ray continuum to constrain the reflection component and other nonthermal emission asscciated with jet or starburst activity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAKAFUMI KAWANO | JAP | 8 | AO8 | OBSERVATION OF THE MULTI EMISSION LINES FROM SEYFERT 2 GALAXY: NGC6552 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708014010/ | Quick Look | ![]() |
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415 | SN 2006JD | 120.5317 | 0.8109 | 119.887421 | 0.950976 | 122.551734 | -19.245465 | 220.45479917 | 16.05743863 | 101.8795 | 56954.8286458333 | 2014-10-24 19:53:15 | 56958.31125 | 2014-10-28 07:28:12 | 709001010 | 144.4894 | 150 | 144.4894 | 151.0361 | 0 | 151.0521 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7014351852 | 2016-08-16 16:50:04 | 57435 | 2016-02-17 00:00:00 | 57066.4298032407 | 2015-02-13 10:18:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090005 | We propose a 150 ks observation of a supernova (SN) 2006jd, a bright SN IIn discovered on October 12, 2006. It is a rare SN that remains bright in X-rays over several years, hence provides us with a rare opportunity to study the dense medium that was ejected by the progenitor star before the SN explosion. Our analysis of archival data taken by Suzaku in 2008 and XMM-Newton in 2009 has indicated interesting spectral evolution, i.e., spectral softening and an increasing centroid of Fe-K lines complex. Our proposed observation will show much clearer spectral variation than that seen in the previous Suzaku and XMM-Newton data, allowing us to understand the details of spectral evolution. The dataset will become a reference for the study of late-time X-ray spectroscopy of SN IIn. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SATORU KATSUDA | JAP | 9 | AO9 | PROBING LATE-TIME X-RAY SPECTRUM OF SN 2006JD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709001010/ | Quick Look | ![]() |
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416 | NGC 2655 | 133.9038 | 78.2094 | 132.281402 | 78.399558 | 105.125039 | 57.091904 | 134.93858201 | 32.69360092 | 275.5561 | 56789.4281828704 | 2014-05-12 10:16:35 | 56791.0731712963 | 2014-05-14 01:45:22 | 709003010 | 76.8371 | 80 | 76.8371 | 76.8371 | 0 | 76.8371 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 2.1539 | 0 | PROCESSED | 57615.0904398148 | 2016-08-15 02:10:14 | 57173 | 2015-05-31 00:00:00 | 56807.6198726852 | 2014-05-30 14:52:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090017 | 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. 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. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709003010/ | Quick Look | ![]() |
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417 | ARP318 | 32.3792 | -10.1586 | 31.765368 | -10.394539 | 26.44249 | -21.810803 | 173.95964772 | -64.97329044 | 75.9989 | 56873.8890509259 | 2014-08-04 21:20:14 | 56875.8252662037 | 2014-08-06 19:48:23 | 709009010 | 80.2195 | 80 | 80.2195 | 80.2195 | 0 | 80.222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.3811 | 15.3811 | 43.076 | 0 | PROCESSED | 57616.4808217593 | 2016-08-16 11:32:23 | 57267 | 2015-09-02 00:00:00 | 56898.4603703704 | 2014-08-29 11:02:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090037 | We propose Suzaku/XIS and PIN observations of nearby two radio-quiet AGNs with very weak mid-infrared emission, which might represent a new class of hot dust free AGNs. We found hot dust free AGN candidates by combining the Swift/BAT hard X-ray all-sky AGN catalog with mid-infrared (MIR) all-sky surveys. Three out of 503 sources are not detected in their MIR bands, even in the high sensitivity of WISE. One source is radio-loud AGNs and the other two radio-quiet sources are also observed in 2-10 keV band with Swift/XRT, and no significant Fe Ka line emission is detected. The scientific goal of this proposal is to obtain the first Fe Ka detection or strong constraints of the emission, which will give us a direct evidence that these sources have very small amount or even lack of torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KOHEI ICHIKAWA | JAP | 9 | AO9 | THE FIRST BROADBAND X-RAY OBSERVATIONS OF HOT DUST FREE AGNS IN THE LOCAL UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709009010/ | Quick Look | ![]() |
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418 | A2104W | 234.9146 | -3.2969 | 234.261116 | -3.135581 | 233.381893 | 15.795133 | 2.73337641 | 39.30878407 | 117.9077 | 54121.3401388889 | 2007-01-21 08:09:48 | 54121.8960532407 | 2007-01-21 21:30:19 | 801001010 | 19.9269 | 20 | 19.9269 | 19.9269 | 0 | 19.9269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.2001 | 17.2001 | 48.0079 | 2 | PROCESSED | 57536.8971875 | 2016-05-28 21:31:57 | 54735 | 2008-09-26 00:00:00 | 54137.0936805556 | 2007-02-06 02:14:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801001010/ | Quick Look | ![]() |
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419 | RX J1347.5-1145 | 206.8558 | -11.8095 | 206.189394 | -11.560383 | 209.147012 | -0.679812 | 323.97878779 | 48.76095676 | 291.7151 | 53931.2858333333 | 2006-07-15 06:51:36 | 53933.2551388889 | 2006-07-17 06:07:24 | 801013020 | 79.1105 | 75 | 79.1265 | 79.1105 | 79.1265 | 79.1345 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 69.567 | 69.567 | 170.1098 | 2 | PROCESSED | 57534.9865393518 | 2016-05-26 23:40:37 | 54394 | 2007-10-21 00:00:00 | 53942.463587963 | 2006-07-26 11:07:34 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOMI OTA | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013020/ | Quick Look | ![]() |
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420 | OPHIUCHUS CLUSTER 0 | 258.0174 | -23.3865 | 257.259196 | -23.326891 | 259.005066 | -0.401441 | 0.50702706 | 9.33401192 | 88.8366 | 54183.0313078704 | 2007-03-24 00:45:05 | 54183.5648726852 | 2007-03-24 13:33:25 | 801021010 | 16.6411 | 15 | 16.6411 | 16.6411 | 0 | 16.6411 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.5209 | 13.5209 | 46.0959 | 0 | PROCESSED | 57537.9746643518 | 2016-05-29 23:23:31 | 54736 | 2008-09-27 00:00:00 | 54209.5175462963 | 2007-04-19 12:25:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801021010/ | Quick Look | ![]() |
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421 | OPHIUCHUS CLUSTER 8 | 258.0175 | -23.6665 | 257.257716 | -23.606887 | 259.028283 | -0.680466 | 0.2749393 | 9.17298979 | 88.8988 | 54182.4897337963 | 2007-03-23 11:45:13 | 54183.0308333333 | 2007-03-24 00:44:24 | 801029010 | 23.7389 | 15 | 23.7469 | 23.7389 | 0 | 23.7469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.678 | 21.678 | 46.746 | 0 | PROCESSED | 57537.9753240741 | 2016-05-29 23:24:28 | 54736 | 2008-09-27 00:00:00 | 54209.5725231482 | 2007-04-19 13:44:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801029010/ | Quick Look | ![]() |
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422 | M87 50' SE | 188.2678 | 11.8367 | 187.635305 | 12.112401 | 182.806232 | 14.132107 | 286.30035277 | 74.11241529 | 119.899 | 54071.127650463 | 2006-12-02 03:03:49 | 54072.312037037 | 2006-12-03 07:29:20 | 801039010 | 53.6374 | 50 | 53.6374 | 53.6581 | 0 | 53.6454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1394 | 46.1394 | 102.309 | 1 | PROCESSED | 57536.2354861111 | 2016-05-28 05:39:06 | 54735 | 2008-09-26 00:00:00 | 54088.5776736111 | 2006-12-19 13:51:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801039010/ | Quick Look | ![]() |
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423 | PERSEUS CL OFFSET | 49.2788 | 41.3719 | 48.454118 | 41.188803 | 58.04223 | 22.344257 | 150.2212005 | -13.65398882 | 65.9966 | 53980.7676273148 | 2006-09-02 18:25:23 | 53981.4543287037 | 2006-09-03 10:54:14 | 801049020 | 32.4646 | 30 | 32.4806 | 32.4646 | 32.4966 | 32.4886 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 28.2912 | 28.2912 | 59.3199 | 1 | PROCESSED | 57535.422025463 | 2016-05-27 10:07:43 | 54526 | 2008-03-01 00:00:00 | 54021.2712731482 | 2006-10-13 06:30:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049020/ | Quick Look | ![]() |
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424 | ABELL 2199 OFFSET 4 | 247.0296 | 39.3161 | 246.598828 | 39.425672 | 233.044127 | 59.841273 | 62.60481799 | 43.78660639 | 250.4756 | 54012.6800462963 | 2006-10-04 16:19:16 | 54013.3044444444 | 2006-10-05 07:18:24 | 801060010 | 24.4546 | 25 | 24.4706 | 24.4626 | 24.4546 | 24.4775 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.811 | 25.811 | 53.9399 | 0 | PROCESSED | 57535.7612615741 | 2016-05-27 18:16:13 | 54735 | 2008-09-26 00:00:00 | 54024.6738888889 | 2006-10-16 16:10:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801060010/ | Quick Look | ![]() |
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425 | VELA JR SE3 | 133.7724 | -47.2478 | 133.349347 | -47.055911 | 161.448089 | -60.302336 | 267.30006641 | -1.40128647 | 110.0008 | 56629.9618055556 | 2013-12-03 23:05:00 | 56630.5806828704 | 2013-12-04 13:56:11 | 508062010 | 27.3638 | 25 | 27.3644 | 27.3638 | 0 | 27.3658 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.7141 | 21.7141 | 53.4599 | 1 | PROCESSED | 57613.4843055556 | 2016-08-13 11:37:24 | 57005 | 2014-12-14 00:00:00 | 56639.5938888889 | 2013-12-13 14:15:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 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) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | TARO FUKUYAMA | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508062010/ | Quick Look | ![]() |
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426 | CEN45 | 192.5119 | -41.3865 | 191.819775 | -41.11429 | 209.359018 | -32.811033 | 302.65166747 | 21.4844922 | 104.7288 | 54458.1467939815 | 2007-12-24 03:31:23 | 54459.2294444444 | 2007-12-25 05:30:24 | 802008010 | 58.2226 | 53 | 58.2226 | 58.2365 | 0 | 58.2306 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.5171 | 64.5171 | 93.5218 | 2 | PROCESSED | 57540.9525810185 | 2016-06-01 22:51:43 | 54854 | 2009-01-23 00:00:00 | 54486.1941087963 | 2008-01-21 04:39:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOMI OTA | JAP | 2 | AO2 | MEASURING GAS MOTIONS OF THE INFALLING SUBCLUSTER CEN45 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802008010/ | Quick Look | ![]() |
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427 | A963N | 154.2645 | 39.1732 | 153.523641 | 39.42315 | 141.268932 | 26.461753 | 182.34163859 | 55.82043448 | 108.9136 | 54428.4751041667 | 2007-11-24 11:24:09 | 54429.0522453704 | 2007-11-25 01:15:14 | 802010010 | 29.1318 | 25 | 29.1318 | 29.1413 | 0 | 29.1358 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.8843 | 27.8843 | 49.8381 | 0 | PROCESSED | 57540.5914351852 | 2016-06-01 14:11:40 | 54804 | 2008-12-04 00:00:00 | 54434.2199305556 | 2007-11-30 05:16:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802010010/ | Quick Look | ![]() |
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428 | FORNAX_GALACTIC_1 | 48.2958 | -37.68 | 47.815673 | -37.866142 | 29.586545 | -52.740717 | 241.51144521 | -58.49700193 | 45.4419 | 54279.8103240741 | 2007-06-28 19:26:52 | 54280.3335532407 | 2007-06-29 08:00:19 | 802037010 | 20.4175 | 20 | 20.4175 | 20.4175 | 0 | 20.4175 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.1912 | 16.1912 | 45.184 | 0 | PROCESSED | 57539.0539814815 | 2016-05-31 01:17:44 | 54695 | 2008-08-17 00:00:00 | 54322.4346064815 | 2007-08-10 10:25:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802037010/ | Quick Look | ![]() |
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429 | OPHIUCHUS CLUSTER | 258.1093 | -23.379 | 257.351096 | -23.319827 | 259.088514 | -0.387026 | 0.56233145 | 9.26925896 | 277.7852 | 54367.8835069444 | 2007-09-24 21:12:15 | 54370.5939351852 | 2007-09-27 14:15:16 | 802046010 | 100.525 | 100 | 100.525 | 100.525 | 0 | 100.525 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.9495 | 82.9495 | 234.1619 | 3 | PROCESSED | 57540.1576041667 | 2016-06-01 03:46:57 | 54770 | 2008-10-31 00:00:00 | 54402.5613194444 | 2007-10-29 13:28:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AKIHIRO FURUZAWA | JAP | 2 | AO2 | APPROCHING RESONANCE SCATTERING/NI-OVERABUNDANCE PROBLEM IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802046010/ | Quick Look | ![]() |
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430 | COMA_60OFF | 194.0251 | 27.4252 | 193.418894 | 27.695609 | 180.937501 | 30.537759 | 49.19228369 | 88.92228234 | 126.7582 | 54438.1998726852 | 2007-12-04 04:47:49 | 54439.1946990741 | 2007-12-05 04:40:22 | 802048010 | 36.6669 | 30 | 36.6669 | 36.6669 | 0 | 36.6669 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.6962 | 31.6962 | 85.9219 | 1 | PROCESSED | 57540.8231365741 | 2016-06-01 19:45:19 | 54814 | 2008-12-14 00:00:00 | 54445.3011689815 | 2007-12-11 07:13:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SUSUMU INOUE | JAP | 2 | AO2 | EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802048010/ | Quick Look | ![]() |
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431 | FILAMENT JUNCTION 1 | 204.175 | 43.8307 | 203.643106 | 44.085146 | 179.610846 | 48.837733 | 97.2080472 | 70.96687365 | 328.3601 | 55706.688900463 | 2011-05-25 16:32:01 | 55707.984224537 | 2011-05-26 23:37:17 | 806003010 | 52.5091 | 60 | 52.5091 | 52.5171 | 0 | 52.5171 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.1339 | 50.1339 | 111.8899 | 0 | PROCESSED | 57602.1515509259 | 2016-08-02 03:38:14 | 56093 | 2012-06-15 00:00:00 | 55725.311412037 | 2011-06-13 07:28:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806003010/ | Quick Look | ![]() |
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432 | IKT25 | 16.5704 | -72.153 | 16.175469 | -72.420209 | 314.528049 | -65.245772 | 301.32642461 | -44.92895011 | 33.6181 | 54601.2130208333 | 2008-05-15 05:06:45 | 54603.3675810185 | 2008-05-17 08:49:19 | 803002010 | 107.3223 | 100 | 107.3303 | 107.3303 | 0 | 107.3223 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124.1064 | 124.1064 | 186.1339 | 1 | PROCESSED | 57542.58375 | 2016-06-03 14:00:36 | 54981 | 2009-05-30 00:00:00 | 54613.1905439815 | 2008-05-27 04:34:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030016 | In order for the white dwarf, the progenitor of SN Ia, to increase its mass to the Chandrasekhar limit, stellar wind driven by Fe contained in the accreting matter needs to be strong enough. For this reason, SN Ia is difficult to take place in the galaxy with low metallicity. We propose the observation on IKT 25, a type Ia SNR candidate in SMC, in order to decide its origin. Since the Fe abundance of SMC (0.2 solar) is lower than that of any other galaxys where SN Ia (or its remnant) had already been discovered, this observation will give the strongest restriction to the theory of the white dwarf evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYA YAMAGUCHI | JAP | 3 | AO3 | IKT25: TYPE IA SNR CANDIDATE IN SMALL MAGELLANIC CLOUD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803002010/ | Quick Look | ![]() |
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433 | ZWCL_0823_FILAMENT-1 | 126.4596 | 4.2515 | 125.801978 | 4.415646 | 127.752151 | -14.538767 | 220.17063425 | 22.90045491 | 284.0603 | 54603.3781944444 | 2008-05-17 09:04:36 | 54604.4551388889 | 2008-05-18 10:55:24 | 803009010 | 41.3573 | 40 | 41.3573 | 41.3619 | 0 | 41.3619 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.9369 | 35.9369 | 93.0059 | 1 | PROCESSED | 57542.5603472222 | 2016-06-03 13:26:54 | 54979 | 2009-05-28 00:00:00 | 54613.0757060185 | 2008-05-27 01:49:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030039 | We propose Suzaku X-ray follow-up observations of dark matter (DM) halo "sub-clumps" detected by the Subaru weak-lens survey. The sub-clumps we are interested in are the smaller DM halo associated with large scale structures. According to the CDM hierarchical structure formation scenario, they are the elemental component of the universe. Since the barion component associated to the clumps are supposed to be very faint, the X-ray follow-up requires the highest sensitivity for diffuse sources, i.e. the Suzaku XIS detectors. Our aim is to detect barion signals and reveal the history/nature of these sub-clumps. A total of four pointing, two aiming at A222/223 filament and another two at ZwCl0823--A664 filament are proposed. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO NAKAZAWA | JAP | 3 | AO3 | SUZAKU X-RAY FOLLOW-UP OF DARK MATTER SUB-CLUMPS DETECTED WITH SUBARU WEAK-LENS SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803009010/ | Quick Look | ![]() |
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434 | DEM L 205 | 82.0576 | -67.4229 | 82.080975 | -67.461346 | 340.764256 | -86.78514 | 277.64219696 | -32.8462006 | 9.9744 | 55005.3430092593 | 2009-06-23 08:13:56 | 55006.4578472222 | 2009-06-24 10:59:18 | 804010010 | 41.3433 | 40 | 41.3492 | 41.3492 | 0 | 41.3433 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3829 | 37.3829 | 96.3078 | 3 | PROCESSED | 57547.6717361111 | 2016-06-08 16:07:18 | 55381 | 2010-07-04 00:00:00 | 55015.1437268518 | 2009-07-03 03:26:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040009 | The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYA YAMAGUCHI | JAP | 4 | AO4 | DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804010010/ | Quick Look | ![]() |
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435 | A2390 | 328.3984 | 17.7035 | 327.804289 | 17.467151 | 337.435653 | 28.529496 | 73.96308198 | -27.80512015 | 79.9886 | 54955.5395486111 | 2009-05-04 12:56:57 | 54957.6939583333 | 2009-05-06 16:39:18 | 804012010 | 96.4645 | 90 | 96.4645 | 96.473 | 0 | 96.4725 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 85.5386 | 85.5386 | 186.1119 | 1 | PROCESSED | 57546.5371990741 | 2016-06-07 12:53:34 | 55343 | 2010-05-27 00:00:00 | 54976.1695023148 | 2009-05-25 04:04:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040011 | We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAOMI OTA | JAP | 4 | AO4 | SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804012010/ | Quick Look | ![]() |
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436 | FERMI_0265 | 187.8001 | -14.1665 | 187.150388 | -13.890445 | 192.786887 | -9.914495 | 295.53023761 | 48.41419063 | 294.2648 | 55020.9540277778 | 2009-07-08 22:53:48 | 55021.5418981482 | 2009-07-09 13:00:20 | 804017010 | 26.3115 | 80 | 26.3115 | 26.3115 | 0 | 26.3115 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.8463 | 22.8463 | 50.7879 | 1 | PROCESSED | 57547.7938773148 | 2016-06-08 19:03:11 | 55422 | 2010-08-14 00:00:00 | 55034.2333217593 | 2009-07-22 05:35:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804017010/ | Quick Look | ![]() |
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437 | FERMI_0459 | 304.3461 | 6.0496 | 303.729476 | 5.893761 | 308.253181 | 25.044638 | 48.6197877 | -16.02859504 | 257.4741 | 55131.4269097222 | 2009-10-27 10:14:45 | 55132.2224189815 | 2009-10-28 05:20:17 | 804020010 | 32.8128 | 30 | 32.8128 | 32.8128 | 0 | 32.8128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.6251 | 28.6251 | 68.7259 | 0 | PROCESSED | 57549.0265046296 | 2016-06-10 00:38:10 | 55513 | 2010-11-13 00:00:00 | 55149.4269791667 | 2009-11-14 10:14:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804020010/ | Quick Look | ![]() |
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438 | W51SW | 290.8908 | 14.1062 | 290.315286 | 14.008227 | 295.206632 | 35.736826 | 49.1149541 | -0.54215584 | 104.3698 | 55285.3081944444 | 2010-03-30 07:23:48 | 55286.3752314815 | 2010-03-31 09:00:20 | 504067010 | 43.7287 | 40 | 43.7287 | 43.7287 | 0 | 43.7287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.8137 | 9.8137 | 92.1799 | 0 | PROCESSED | 57551.0856597222 | 2016-06-12 02:03:21 | 55671 | 2011-04-20 00:00:00 | 55302.2468055556 | 2010-04-16 05:55:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEAKI KATAGIRI | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504067010/ | Quick Look | ![]() |
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439 | SGR1806-20 | 272.1595 | -20.349 | 271.415501 | -20.357687 | 272.017973 | 3.076639 | 10.0481975 | -0.20823053 | 88.7483 | 54189.6305555556 | 2007-03-30 15:08:00 | 54190.0627199074 | 2007-03-31 01:30:19 | 401021010 | 19.2889 | 20 | 19.2889 | 19.595 | 0 | 19.3563 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.5071 | 16.5071 | 37.3279 | 1 | PROCESSED | 57538.0253587963 | 2016-05-30 00:36:31 | 54561 | 2008-04-05 00:00:00 | 54209.5169212963 | 2007-04-19 12:24:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUJIN NAKAGAWA | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401021010/ | Quick Look | ![]() |
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440 | A2029_4 | 228.0053 | 5.6496 | 227.385284 | 5.836972 | 223.833276 | 22.612919 | 6.60771448 | 50.27207577 | 112.9543 | 55225.6146180556 | 2010-01-29 14:45:03 | 55226.2501388889 | 2010-01-30 06:00:12 | 804024040 | 25.6584 | 22 | 25.6584 | 25.6824 | 0 | 25.6664 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.446 | 19.446 | 54.9019 | 0 | PROCESSED | 57550.4263657407 | 2016-06-11 10:13:58 | 55637 | 2011-03-17 00:00:00 | 55271.0446064815 | 2010-03-16 01:04:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024040/ | Quick Look | ![]() |
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441 | A478 OFFSET C | 63.6328 | 10.5074 | 62.946361 | 10.382264 | 63.629527 | -10.552687 | 182.59008129 | -28.04907037 | 259.6787 | 55604.2488888889 | 2011-02-12 05:58:24 | 55605.3522685185 | 2011-02-13 08:27:16 | 805003010 | 47.1486 | 45 | 47.1646 | 47.1486 | 0 | 47.1646 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.9898 | 39.9898 | 95.3198 | 2 | PROCESSED | 57600.9430671296 | 2016-07-31 22:38:01 | 55983 | 2012-02-26 00:00:00 | 55617.4134490741 | 2011-02-25 09:55:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | ANDREW FABIAN | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805003010/ | Quick Look | ![]() |
442 | Crab nebula | 83.2708 | 21.9976 | 82.518718 | 21.963167 | 83.762776 | -1.29769 | 184.39063256 | -6.07689385 | 86.7331 | 53607.7165162037 | 2005-08-25 17:11:47 | 53607.9167361111 | 2005-08-25 22:00:06 | 100010050 | 9.3469 | 5 | 9.3469 | 9.3469 | 9.3469 | 9.3469 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6.653 | 6.653 | 17.2879 | 0 | PROCESSED | 57526.9 | 2016-05-18 21:36:00 | 54247 | 2007-05-27 00:00:00 | 54122.4223611111 | 2007-01-22 10:08:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Offset 1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010050/ | Quick Look | ![]() |
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443 | RXCJ0013.2-4905 | 3.3206 | -49.1017 | 2.696864 | -49.379799 | 337.855034 | -45.122753 | 318.93482177 | -66.82406097 | 263.5597 | 55565.2569328704 | 2011-01-04 06:09:59 | 55565.4036689815 | 2011-01-04 09:41:17 | 805023010 | 8.432 | 10 | 8.432 | 8.432 | 0 | 8.432 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57600.5421875 | 2016-07-31 13:00:45 | 56016 | 2012-03-30 00:00:00 | 55627.5157638889 | 2011-03-07 12:22:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050021 | We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 5 | AO5 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805023010/ | Quick Look | ![]() |
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444 | A2199 EAST OFFSET | 246.7666 | 40.2374 | 246.342386 | 40.34813 | 232.073247 | 60.652123 | 63.87682573 | 44.00920476 | 240.0015 | 55458.2941666667 | 2010-09-19 07:03:36 | 55459.7155324074 | 2010-09-20 17:10:22 | 805042010 | 58.4398 | 60 | 58.4399 | 58.4398 | 0 | 58.4398 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52.5076 | 52.5076 | 122.7919 | 1 | PROCESSED | 57553.4778935185 | 2016-06-14 11:28:10 | 55836 | 2011-10-02 00:00:00 | 55470.1049884259 | 2010-10-01 02:31:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050081 | We propose to observe the virial radius region of the cluster of galaxies A2199 (z=0.0309) over the virial radius. This cluster lies in the Great Wall, and a cosmic filament runs from north to south. We aim to explore possible influence from the filament gives onto the formation process of the cluster, by comparing the hot-gas density and temperature around the virial radius in parallel and vertical directions to the filament. With the high sensitivity of XIS to faint extended emission, we expect to detect denser and hotter gas in the filement even outside the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROKI AKAMATSU | JAP | 5 | AO5 | TEMPERATURE OVER THE VIRIAL RADIUS OF ABELL 2199, AND INFLUENCE OF THE LARGE-SCALE STRUCTURE. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805042010/ | Quick Look | ![]() |
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445 | VIRGOHI 21 | 184.472 | 14.7597 | 183.83671 | 15.037342 | 178.086194 | 15.290258 | 268.97789082 | 75.3718003 | 123.3105 | 55535.5218518518 | 2010-12-05 12:31:28 | 55537.7911574074 | 2010-12-07 18:59:16 | 805054010 | 103.1915 | 100 | 103.3995 | 103.1915 | 0 | 103.3995 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.9209 | 81.9209 | 196.0168 | 4 | PROCESSED | 57554.4175694444 | 2016-06-15 10:01:18 | 55916 | 2011-12-21 00:00:00 | 55550.3035185185 | 2010-12-20 07:17:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050114 | We propose a 100 ksec observation of "VIRGOHI 21" in the Virgo galaxy cluster. VIRGOHI 21 with no optical counterpart, is called a "dark galaxy" from the presence of velocity informed gas clouds with 21-cm observations somewhat like a disk galaxy. Origins are said to be traces of density fluctuation at cluster birth, or gas stripped from galaxies, but nothing clear is yet not introduced. Using the energy resolution of the XIS, we would like to explain the origin, deciding heavy element abundances of VIRGOHI 21. Extremely low abundance will give us the first "dark galaxy". Discovery of a "dark galaxy" with its information of prehistoric universe, will lead us to not just galaxy evolution, but also mighty mechanisms to understand cosmology, giving great impact to astrophysics itself. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RYO IIZUKA | JAP | 5 | AO5 | X-RAY SEARCH FOR A DARK GALAXY IN THE VIRGO CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805054010/ | Quick Look | ![]() |
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446 | GC_SGR_B_NORTH | 266.6958 | -28.383 | 265.90497 | -28.365031 | 267.072823 | -4.975469 | 0.60519276 | 0.06967717 | 271.4415 | 53999.7284837963 | 2006-09-21 17:29:01 | 54001.2863425926 | 2006-09-23 06:52:20 | 501040010 | 61.3753 | 62 | 61.3913 | 61.3753 | 61.3833 | 61.3913 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.867 | 53.867 | 134.5818 | 2 | PROCESSED | 57535.7042361111 | 2016-05-27 16:54:06 | 54735 | 2008-09-26 00:00:00 | 54021.2828472222 | 2006-10-13 06:47:18 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040010/ | Quick Look | ![]() |
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447 | EX HYA | 193.0706 | -29.2994 | 192.395685 | -29.027802 | 203.848452 | -21.746269 | 303.15288952 | 33.57198642 | 300.0004 | 54299.8912152778 | 2007-07-18 21:23:21 | 54302.4377199074 | 2007-07-21 10:30:19 | 402001010 | 100.5157 | 100 | 100.5237 | 100.5157 | 0 | 100.5237 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.1135 | 91.1135 | 219.9599 | 1 | PROCESSED | 57539.3319097222 | 2016-05-31 07:57:57 | 54707 | 2008-08-29 00:00:00 | 54339.5139467593 | 2007-08-27 12:20:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MANABU ISHIDA | JAP | 2 | AO2 | MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402001010/ | Quick Look | ![]() |
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448 | SNR B0532-675 | 83.0766 | -67.535 | 83.105131 | -67.568522 | 336.894388 | -87.135778 | 277.71335978 | -32.44457154 | 140.0497 | 55871.6295601852 | 2011-11-06 15:06:34 | 55874.1570601852 | 2011-11-09 03:46:10 | 806007010 | 82.4909 | 80 | 82.4909 | 82.4909 | 0 | 82.4909 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.4573 | 77.4573 | 218.3547 | 4 | PROCESSED | 57603.7734027778 | 2016-08-03 18:33:42 | 56257 | 2012-11-26 00:00:00 | 55890.6997337963 | 2011-11-25 16:47:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060025 | Interstellar medium (ISM) heated by a forward shock of supernova remnants (SNRs) gives us a unique opportunity to study local metal abundance and density. Systematic study of the shock-heated ISM in a galaxy unveils its overall metal distribution and provides a key to understand its chemical evolution. On the basis of this idea, we have performed observations of SNRs in the Large Magellanic Cloud (LMC). We here propose to observe the LMC SNR B0532-675 for 80 ks. Since it locates near the star formation region LH76, we expect that we can study the process of metal diffusion from a star forming region by utilizing the result from another SNR DEM L241 near LH76 already observed. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KENTARO SOMEYA | JAP | 6 | AO6 | STUDY OF CHEMICAL EVOLUTION OF THE LARGE MAGELLANIC CLOUD WITH SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806007010/ | Quick Look | ![]() |
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449 | XMMU 2235.3-2557 | 338.8435 | -25.9657 | 338.152793 | -26.224773 | 330.62189 | -15.821353 | 27.27021923 | -59.64080614 | 244.5944 | 55878.6378125 | 2011-11-13 15:18:27 | 55881.5577777778 | 2011-11-16 13:23:12 | 806013010 | 101.1227 | 100 | 101.1227 | 101.1227 | 0 | 101.1227 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.6244 | 90.6244 | 252.2417 | 4 | PROCESSED | 57603.8656481482 | 2016-08-03 20:46:32 | 56257 | 2012-11-26 00:00:00 | 55890.7014583333 | 2011-11-25 16:50:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060038 | Galaxy clusters at high redshift are useful as a cosmological probe that have a potential to constrain the inflation theory via its mass function. A massive cluster, XMMU 2235.3-2557 found at z=1.4 is especially important because the presence itself should be quite rare if the standard theory with the Gaussian random field is correct. However, there can be a lot of systematic errors of the mass estimates, that is, the temperature measurement of the cluster. Hence, we propose an independent measurement of X-ray spectroscopic temperature by SUZAKU. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HAJIME KAWAHARA | JAP | 6 | AO6 | TEMPERATURE MEASUREMENT OF A MASSIVE HIGH-Z CLUSTER XMMU 2235.3-2557 BY SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806013010/ | Quick Look | ![]() |
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450 | COMA OUTSKIRTS1 | 196.4834 | 28.9037 | 195.885803 | 29.171019 | 182.42683 | 32.834582 | 62.80265316 | 86.34142243 | 115.9997 | 55900.1880092593 | 2011-12-05 04:30:44 | 55901.4341203704 | 2011-12-06 10:25:08 | 806020010 | 48.334 | 50 | 48.334 | 48.334 | 0 | 48.334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.2514 | 42.2514 | 107.6538 | 0 | PROCESSED | 57604.0541898148 | 2016-08-04 01:18:02 | 56282 | 2012-12-21 00:00:00 | 55914.2892013889 | 2011-12-19 06:56:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806020010/ | Quick Look | ![]() |
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451 | COMA OUTSKIRTS4 | 193.3444 | 28.9037 | 192.738609 | 29.174872 | 179.533604 | 31.586326 | 109.48887466 | 88.17367696 | 116.0002 | 55902.7178125 | 2011-12-07 17:13:39 | 55903.9105324074 | 2011-12-08 21:51:10 | 806023010 | 51.6563 | 50 | 51.6643 | 51.6563 | 0 | 51.6713 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.0198 | 49.0198 | 103.0419 | 1 | PROCESSED | 57604.0840972222 | 2016-08-04 02:01:06 | 56284 | 2012-12-23 00:00:00 | 55915.2433449074 | 2011-12-20 05:50:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806023010/ | Quick Look | ![]() |
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452 | VELA SOUTHWEST 1 | 126.2671 | -48.2152 | 125.877652 | -48.051248 | 153.532268 | -63.870386 | 264.99036518 | -5.99332729 | 119.5649 | 55164.9700925926 | 2009-11-29 23:16:56 | 55165.818900463 | 2009-11-30 19:39:13 | 504063010 | 32.7331 | 30 | 32.7492 | 32.7331 | 0 | 32.7411 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23.7674 | 23.7674 | 73.3099 | 0 | PROCESSED | 57549.6219791667 | 2016-06-10 14:55:39 | 55546 | 2010-12-16 00:00:00 | 55179.268587963 | 2009-12-14 06:26:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUNKO HIRAGA | JAP | 4 | AO4 | X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504063010/ | Quick Look | ![]() |
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453 | A3581_CEN | 211.9083 | -27.0199 | 211.193684 | -26.782616 | 219.008869 | -13.266139 | 323.17769244 | 32.83870198 | 117.8993 | 56308.5541782407 | 2013-01-16 13:18:01 | 56310.7078356482 | 2013-01-18 16:59:17 | 807026010 | 80.408 | 80 | 80.416 | 80.416 | 0 | 80.408 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.1715 | 70.1715 | 186.0419 | 1 | PROCESSED | 57608.5784259259 | 2016-08-08 13:52:56 | 56711 | 2014-02-23 00:00:00 | 56345.6637384259 | 2013-02-22 15:55:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070064 | We propose to study the metallicity of Abell 3581 to the outer region beyond 0.5 r180. Abell 3581 is a very useful system for investigating the history of the chemical evolution of groups and clusters, because the temperature of the intra-cluster medium is about 1.7 keV, which is intermediate between groups and clusters of galaxies. Suzaku will enable us to measure for the first time the metal distributions to such outer regions of the clusters, because of the significantly lower background level and higher sensitivity below ~1 keV. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 7 | AO7 | SEARCH FOR THE METALLICITY OF ABELL 3581 TO THE OUTER REGION BEYOND 0.5 R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807026010/ | Quick Look | ![]() |
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454 | A2061_2 | 230.6122 | 30.8661 | 230.100044 | 31.043682 | 216.595507 | 47.269453 | 48.57175305 | 56.92431824 | 121.1842 | 56307.485625 | 2013-01-15 11:39:18 | 56308.5460185185 | 2013-01-16 13:06:16 | 807030010 | 41.788 | 40 | 41.788 | 41.788 | 0 | 41.788 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7529 | 37.7529 | 91.6018 | 1 | PROCESSED | 57608.5263888889 | 2016-08-08 12:38:00 | 56707 | 2014-02-19 00:00:00 | 56338.5482291667 | 2013-02-15 13:09:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070070 | We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO OKABE | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807030010/ | Quick Look | ![]() |
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455 | NGC 5044 NORTH 30' | 199.0992 | -15.8941 | 198.433238 | -15.630477 | 203.627041 | -7.241957 | 311.67530339 | 46.55349501 | 110.0017 | 55220.5889814815 | 2010-01-24 14:08:08 | 55222.2571064815 | 2010-01-26 06:10:14 | 804013010 | 62.8482 | 60 | 62.8562 | 62.8482 | 0 | 62.8562 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.5926 | 44.5926 | 144.0998 | 1 | PROCESSED | 57550.396099537 | 2016-06-11 09:30:23 | 55602 | 2011-02-10 00:00:00 | 55235.338587963 | 2010-02-08 08:07:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040013 | Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804013010/ | Quick Look | ![]() |
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456 | A401EAST | 45.0348 | 13.3366 | 44.348124 | 13.13869 | 46.452106 | -3.5684 | 164.66710088 | -38.88860633 | 71.9996 | 56530.5043055556 | 2013-08-26 12:06:12 | 56531.6841782407 | 2013-08-27 16:25:13 | 808006010 | 51.6628 | 50 | 51.6868 | 51.6628 | 0 | 51.6868 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.8099 | 47.8099 | 101.9238 | 1 | PROCESSED | 57612.4270138889 | 2016-08-12 10:14:54 | 56956 | 2014-10-26 00:00:00 | 56587.515474537 | 2013-10-22 12:22:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHITAKA ISHISAKI | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808006010/ | Quick Look | ![]() |
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457 | COMA SUBHALO3 | 193.9804 | 27.7549 | 193.374568 | 28.025359 | 180.724315 | 30.814588 | 65.39722549 | 88.82429581 | 314.9967 | 56453.0272569444 | 2013-06-10 00:39:15 | 56453.5912384259 | 2013-06-10 14:11:23 | 808021010 | 24.0441 | 20 | 24.0521 | 24.0441 | 0 | 24.0521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.5334 | 25.5334 | 48.6979 | 0 | PROCESSED | 57611.5202199074 | 2016-08-11 12:29:07 | 56872 | 2014-08-03 00:00:00 | 56506.7633101852 | 2013-08-02 18:19:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808021010/ | Quick Look | ![]() |
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458 | A2255_NW | 258.0206 | 64.3236 | 257.946874 | 64.381524 | 198.635574 | 84.547798 | 94.26240936 | 34.95584628 | 200.0017 | 56613.0157060185 | 2013-11-17 00:22:37 | 56613.9467476852 | 2013-11-17 22:43:19 | 808039010 | 43.7688 | 40 | 43.7688 | 43.7688 | 0 | 43.7688 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8557 | 41.8557 | 80.4121 | 0 | PROCESSED | 57613.3414814815 | 2016-08-13 08:11:44 | 56991 | 2014-11-30 00:00:00 | 56625.6806481482 | 2013-11-29 16:20:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080047 | We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROKO YOSHIDA | JAP | 8 | AO8 | MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808039010/ | Quick Look | ![]() |
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459 | BULLET-OFFSET2 | 104.4232 | -55.8309 | 104.179615 | -55.762127 | 129.485135 | -77.282926 | 265.86935635 | -21.32349548 | 287.0017 | 56419.6209722222 | 2013-05-07 14:54:12 | 56422.4605439815 | 2013-05-10 11:03:11 | 808056010 | 101.3855 | 100 | 101.3935 | 101.3935 | 0 | 101.3855 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.6767 | 93.6767 | 245.3058 | 2 | PROCESSED | 57611.3171643518 | 2016-08-11 07:36:43 | 56799 | 2014-05-22 00:00:00 | 56433.6998958333 | 2013-05-21 16:47:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808056010/ | Quick Look | ![]() |
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460 | (L,B)=(-20,0) | 276.6688 | -11.87 | 275.969796 | -11.90065 | 276.648122 | 11.416809 | 19.56512772 | 0.0074406 | 263.6004 | 56215.5456944444 | 2012-10-15 13:05:48 | 56219.7479861111 | 2012-10-19 17:57:06 | 507044010 | 171.8231 | 200 | 171.8231 | 171.8231 | 0 | 171.8231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 147.1192 | 147.1192 | 363.0377 | 4 | PROCESSED | 57607.9036342593 | 2016-08-07 21:41:14 | 56602 | 2013-11-06 00:00:00 | 56238.7999884259 | 2012-11-07 19:11:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEKI UCHIYAMA | JAP | 7 | AO7 | SUZAKU STUDY OF SPATIAL AND TEMPORAL FLUCTUATIONS IN THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507044010/ | Quick Look | ![]() |
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461 | MCG-6-30-15 | 203.9795 | -34.2919 | 203.263096 | -34.036775 | 215.177217 | -22.538878 | 313.29805273 | 27.68293005 | 295.971 | 53599.6735300926 | 2005-08-17 16:09:53 | 53601.1459027778 | 2005-08-19 03:30:06 | 100004010 | 46.6987 | 40 | 46.7009 | 50.9169 | 46.6987 | 46.7254 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 46.4846 | 46.4846 | 127.0999 | 0 | PROCESSED | 57520.7326388889 | 2016-05-12 17:35:00 | 54247 | 2007-05-27 00:00:00 | 54035.7991782407 | 2006-10-27 19:10:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000004 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | MCG-60-30-15 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100004010/ | Quick Look | ![]() |
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462 | PSR B1259-63 | 195.6782 | -63.8867 | 194.888688 | -63.618059 | 227.727553 | -50.938083 | 304.17237227 | -1.04211039 | 282.6534 | 54290.6852083333 | 2007-07-09 16:26:42 | 54291.1876041667 | 2007-07-10 04:30:09 | 402014020 | 19.4817 | 20 | 19.4817 | 19.4817 | 0 | 19.4817 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.9111 | 26.9111 | 43.378 | 1 | PROCESSED | 57539.1396759259 | 2016-05-31 03:21:08 | 54696 | 2008-08-18 00:00:00 | 54328.5032060185 | 2007-08-16 12:04:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014020/ | Quick Look | ![]() |
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463 | PSR B1259-63 | 195.6089 | -63.8685 | 194.820162 | -63.599771 | 227.67155 | -50.942181 | 304.14267075 | -1.0226082 | 321.9333 | 54348.2308449074 | 2007-09-05 05:32:25 | 54348.6043287037 | 2007-09-05 14:30:14 | 402014080 | 18.3327 | 20 | 18.3407 | 18.3487 | 0 | 18.3327 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.3513 | 22.3513 | 32.26 | 0 | PROCESSED | 57539.9271412037 | 2016-05-31 22:15:05 | 54724 | 2008-09-15 00:00:00 | 54356.1999537037 | 2007-09-13 04:47:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014080/ | Quick Look | ![]() |
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464 | THE MOON | 142.9426 | 9.1926 | 142.274308 | 9.413777 | 142.279358 | -5.167487 | 223.99367078 | 39.68355518 | 285.4008 | 56784.5840162037 | 2014-05-07 14:00:59 | 56784.7155555556 | 2014-05-07 17:10:24 | 809001090 | 4.7558 | 45 | 4.7558 | 4.7558 | 0 | 4.7558 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.6674 | 4.6674 | 11.358 | 0 | PROCESSED | 57615.0740277778 | 2016-08-15 01:46:36 | 57162 | 2015-05-20 00:00:00 | 56796.5977546296 | 2014-05-19 14:20:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001090/ | Quick Look | ![]() |
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465 | THE MOON | 29.2087 | 11.3221 | 28.541439 | 11.078317 | 31.138176 | -0.585907 | 147.49986562 | -48.40533826 | 73.8007 | 56857.4028472222 | 2014-07-19 09:40:06 | 56857.5265856482 | 2014-07-19 12:38:17 | 809001170 | 5.6621 | 45 | 5.6701 | 5.6621 | 0 | 5.6701 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4102314815 | 2016-08-15 09:50:44 | 57239 | 2015-08-05 00:00:00 | 56869.612974537 | 2014-07-31 14:42:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001170/ | Quick Look | ![]() |
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466 | THE MOON | 30.7597 | 12.0224 | 30.089346 | 11.782342 | 32.8056 | -0.451848 | 149.17525918 | -47.16814979 | 73.8003 | 56857.5278009259 | 2014-07-19 12:40:02 | 56857.5974189815 | 2014-07-19 14:20:17 | 809001180 | 3.4386 | 45 | 3.4466 | 3.4386 | 0 | 3.4546 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4120601852 | 2016-08-15 09:53:22 | 57239 | 2015-08-05 00:00:00 | 56869.6134953704 | 2014-07-31 14:43:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001180/ | Quick Look | ![]() |
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467 | THE MOON | 138.5418 | 11.2369 | 137.863994 | 11.444435 | 137.511885 | -4.561937 | 219.19555273 | 36.72863641 | 105.699 | 56975.1999768518 | 2014-11-14 04:47:58 | 56975.3237615741 | 2014-11-14 07:46:13 | 809001200 | 3.3796 | 45 | 3.3796 | 3.3796 | 0 | 3.3796 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7701041667 | 2016-08-16 18:28:57 | 57358 | 2015-12-02 00:00:00 | 56992.4114699074 | 2014-12-01 09:52:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001200/ | Quick Look | ![]() |
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468 | THE MOON | 141.4013 | 10.2837 | 140.728619 | 10.500242 | 140.487309 | -4.611146 | 221.84323525 | 38.83162783 | 105.6986 | 56975.4499305556 | 2014-11-14 10:47:54 | 56975.5834143518 | 2014-11-14 14:00:07 | 809001220 | 4.2552 | 45 | 4.2552 | 4.2632 | 0 | 4.2632 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7742592593 | 2016-08-16 18:34:56 | 57358 | 2015-12-02 00:00:00 | 56992.4140625 | 2014-12-01 09:56:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001220/ | Quick Look | ![]() |
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469 | THE MOON | 145.8331 | 9.4283 | 145.16599 | 9.657722 | 144.909334 | -4.019227 | 225.49397113 | 42.31232043 | 105.6985 | 56975.8485300926 | 2014-11-14 20:21:53 | 56975.9376388889 | 2014-11-14 22:30:12 | 809001250 | 4.244 | 45 | 4.244 | 4.308 | 0 | 4.324 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7786574074 | 2016-08-16 18:41:16 | 57358 | 2015-12-02 00:00:00 | 56992.4181828704 | 2014-12-01 10:02:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001250/ | Quick Look | ![]() |
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470 | THE MOON | 335.3702 | -6.281 | 334.716283 | -6.533427 | 334.875812 | 3.693556 | 56.37004308 | -48.74864005 | 248.3898 | 56990.2098148148 | 2014-11-29 05:02:08 | 56990.3474768518 | 2014-11-29 08:20:22 | 809001310 | 6.2242 | 45 | 6.2242 | 6.2242 | 0 | 6.2242 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4106481482 | 2016-08-17 09:51:20 | 57415 | 2016-01-28 00:00:00 | 57002.4438541667 | 2014-12-11 10:39:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001310/ | Quick Look | ![]() |
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471 | THE MOON | 340.8235 | -5.0226 | 340.1744 | -5.285051 | 340.39289 | 2.857324 | 63.09935011 | -52.32405661 | 251.0714 | 56990.6104513889 | 2014-11-29 14:39:03 | 56990.733587963 | 2014-11-29 17:36:22 | 809001340 | 6.3566 | 45 | 6.3566 | 6.3566 | 0 | 6.3566 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4124537037 | 2016-08-17 09:53:56 | 57415 | 2016-01-28 00:00:00 | 57007.4026041667 | 2014-12-16 09:39:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001340/ | Quick Look | ![]() |
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472 | THE MOON | 342.4216 | -4.2139 | 341.77438 | -4.478841 | 342.17578 | 3.00393 | 65.81829296 | -53.01188957 | 247.9474 | 56990.7354513889 | 2014-11-29 17:39:03 | 56990.8683101852 | 2014-11-29 20:50:22 | 809001350 | 6.3196 | 45 | 6.3196 | 6.3196 | 0 | 6.3196 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4131018518 | 2016-08-17 09:54:52 | 57415 | 2016-01-28 00:00:00 | 57006.4014699074 | 2014-12-15 09:38:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001350/ | Quick Look | ![]() |
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473 | FORNAX A WEST LOBE | 50.4184 | -37.1645 | 49.940428 | -37.342839 | 32.47574 | -52.998531 | 240.1258488 | -56.89722719 | 219.7525 | 54092.8700462963 | 2006-12-23 20:52:52 | 54095.6113888889 | 2006-12-26 14:40:24 | 801014010 | 93.3093 | 100 | 93.3093 | 93.3093 | 0 | 93.3093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.3716 | 96.3716 | 236.8358 | 5 | PROCESSED | 57536.4597569444 | 2016-05-28 11:02:03 | 54735 | 2008-09-26 00:00:00 | 54111.6821875 | 2007-01-11 16:22:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO TASHIRO | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801014010/ | Quick Look | ![]() |
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474 | A3112BG | 50.3198 | -44.6958 | 49.891219 | -44.874421 | 26.077848 | -59.651808 | 253.38706356 | -55.37551095 | 204.9994 | 57009.69125 | 2014-12-18 16:35:24 | 57010.2550462963 | 2014-12-19 06:07:16 | 809028020 | 18.3545 | 15 | 18.3545 | 18.3545 | 0 | 18.3545 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5354166667 | 2016-08-17 12:51:00 | 57394 | 2016-01-07 00:00:00 | 57027.3975 | 2015-01-05 09:32:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809028020/ | Quick Look | ![]() |
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475 | PKS 0558-504 VIC 1 | 90.9582 | -50.6414 | 90.657059 | -50.637494 | 92.232149 | -74.075703 | 258.29690544 | -27.96668923 | 6.4262 | 56825.0805208333 | 2014-06-17 01:55:57 | 56826.8543518518 | 2014-06-18 20:30:16 | 809034010 | 52.0132 | 60 | 52.0132 | 52.0132 | 0 | 52.0132 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.4874 | 50.4874 | 153.2479 | 0 | PROCESSED | 57615.2996180556 | 2016-08-15 07:11:27 | 57233 | 2015-07-30 00:00:00 | 56867.5608912037 | 2014-07-29 13:27:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090086 | We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAZUHIRO SAKAI | JAP | 9 | AO9 | IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809034010/ | Quick Look | ![]() |
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476 | HETEJ1900.1-2455 | 285.0506 | -24.9802 | 284.284146 | -25.050704 | 283.615122 | -2.248458 | 11.25454685 | -12.90928139 | 259.4192 | 54389.5913425926 | 2007-10-16 14:11:32 | 54390.5071064815 | 2007-10-17 12:10:14 | 402016010 | 41.7591 | 40 | 41.7788 | 41.7591 | 0 | 41.7751 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.9063 | 39.9063 | 79.1058 | 1 | PROCESSED | 57540.3158564815 | 2016-06-01 07:34:50 | 54771 | 2008-11-01 00:00:00 | 54403.1292708333 | 2007-10-30 03:06:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOKO SUZUKI | JAP | 2 | AO2 | HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402016010/ | Quick Look | ![]() |
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477 | TEVJ2032+4130 | 308.0461 | 41.5016 | 307.599311 | 41.330897 | 328.972015 | 57.41697 | 80.25613164 | 1.05964615 | 221.0839 | 54451.984212963 | 2007-12-17 23:37:16 | 54452.9176157407 | 2007-12-18 22:01:22 | 402031010 | 40.0439 | 40 | 40.0439 | 40.0439 | 0 | 40.0439 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3091 | 37.3091 | 80.6419 | 1 | PROCESSED | 57540.8865625 | 2016-06-01 21:16:39 | 54828 | 2008-12-28 00:00:00 | 54460.6569675926 | 2007-12-26 15:46:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHUNJI KITAMOTO | JAP | 2 | AO2 | STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402031010/ | Quick Look | ![]() |
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478 | RXJ1713.7-3946 | 258.074 | -39.935 | 257.205787 | -39.875387 | 260.458717 | -16.88737 | 347.05133682 | -0.37925502 | 269.9977 | 53639.6563194444 | 2005-09-26 15:45:06 | 53641.2960648148 | 2005-09-28 07:06:20 | 100026010 | 68.4959 | 80 | 68.4959 | 68.5653 | 68.5119 | 68.5253 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56.2382 | 56.2382 | 141.6619 | 0 | PROCESSED | 57527.4561921296 | 2016-05-19 10:56:55 | 54247 | 2007-05-27 00:00:00 | 54037.0750694445 | 2006-10-29 01:48:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Observation of RXJ1713.7-3946 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100026010/ | Quick Look | ![]() |
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479 | ABELL 2255 CENTER | 258.2484 | 64.1467 | 258.17067 | 64.203551 | 200.767912 | 84.543322 | 94.02951141 | 34.88778486 | 111.176 | 55234.3014814815 | 2010-02-07 07:14:08 | 55235.405775463 | 2010-02-08 09:44:19 | 804041010 | 44.5337 | 50 | 44.5337 | 44.5417 | 0 | 44.5417 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43.339 | 43.339 | 95.3759 | 1 | PROCESSED | 57550.5171180556 | 2016-06-11 12:24:39 | 55617 | 2011-02-25 00:00:00 | 55250.1645601852 | 2010-02-23 03:56:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040091 | Suzaku discovered an supra thermal component in the plasma of Abell 3667 which exceeds 13 keV. In order to establish this component in merging clusters, we propose two pointing observations of Abell 2255, which hosts a huge radio halo and a radio relic. With these two pointings, we aim at roughly spotting the location of the supra thermal plasma. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 4 | AO4 | PROBING SUPRA THERMAL PLASMA IN ABELL 2255 WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804041010/ | Quick Look | ![]() |
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480 | GC17 | 267.2896 | -29.5968 | 266.49097 | -29.581693 | 267.620125 | -6.178087 | 359.83441438 | -1.00224826 | 260.2809 | 54384.0425578704 | 2007-10-11 01:01:17 | 54384.480787037 | 2007-10-11 11:32:20 | 502005010 | 20.6035 | 20 | 20.6035 | 20.6035 | 0 | 20.6035 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.1743 | 18.1743 | 37.854 | 1 | PROCESSED | 57540.245787037 | 2016-06-01 05:53:56 | 54777 | 2008-11-07 00:00:00 | 54402.5689583333 | 2007-10-29 13:39:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502005010/ | Quick Look | ![]() |
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481 | OPHIUCHUS CLUSTER 1 | 258.2981 | -23.3868 | 257.539766 | -23.328523 | 259.261866 | -0.380707 | 0.65649186 | 9.12279372 | 88.7031 | 54180.6159953704 | 2007-03-21 14:47:02 | 54181.1398611111 | 2007-03-22 03:21:24 | 801022010 | 24.067 | 15 | 24.075 | 24.067 | 0 | 24.075 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.8213 | 21.8213 | 45.254 | 1 | PROCESSED | 57537.7417476852 | 2016-05-29 17:48:07 | 54736 | 2008-09-27 00:00:00 | 54186.192650463 | 2007-03-27 04:37:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801022010/ | Quick Look | ![]() |
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482 | COMA OUTSKIRTS6 | 193.974 | 28.5108 | 193.369273 | 28.781265 | 180.320045 | 31.486616 | 87.70306179 | 88.30207114 | 115.9975 | 55904.7228703704 | 2011-12-09 17:20:56 | 55905.1452662037 | 2011-12-10 03:29:11 | 806025010 | 21.503 | 20 | 21.503 | 21.503 | 0 | 21.503 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.265 | 20.265 | 36.4719 | 0 | PROCESSED | 57604.0827083333 | 2016-08-04 01:59:06 | 56284 | 2012-12-23 00:00:00 | 55915.2118402778 | 2011-12-20 05:05:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806025010/ | Quick Look | ![]() |
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483 | AWM7 | 43.631 | 41.5933 | 42.82175 | 41.390486 | 53.723626 | 23.815753 | 146.34082925 | -15.61629549 | 90.4997 | 53954.2348842593 | 2006-08-07 05:38:14 | 53954.71625 | 2006-08-07 17:11:24 | 801035010 | 18.9858 | 20 | 18.9858 | 18.9858 | 18.9858 | 18.9858 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.5542 | 17.5542 | 41.588 | 0 | PROCESSED | 57535.2434953704 | 2016-05-27 05:50:38 | 54422 | 2007-11-18 00:00:00 | 54020.7471759259 | 2006-10-12 17:55:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801035010/ | Quick Look | ![]() |
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484 | NGC 4631 | 190.5387 | 32.5478 | 189.929771 | 32.821718 | 174.99352 | 33.703009 | 142.74124336 | 84.2191655 | 139.0678 | 54067.1412615741 | 2006-11-28 03:23:25 | 54068.9133217593 | 2006-11-29 21:55:11 | 801019010 | 81.0761 | 80 | 81.0841 | 81.0761 | 0 | 81.0841 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.4358 | 74.4358 | 153.07 | 0 | PROCESSED | 57536.2568865741 | 2016-05-28 06:09:55 | 54735 | 2008-09-26 00:00:00 | 54088.6914699074 | 2006-12-19 16:35:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NORIKO YAMASAKI | JAP | 1 | AO1 | OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801019010/ | Quick Look | ![]() |
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485 | SAGITTARIUS A* | 266.4146 | -29.0061 | 265.619899 | -28.986758 | 266.840195 | -5.604294 | 359.94468967 | -0.04360372 | 105.8159 | 57113.0215162037 | 2015-04-01 00:30:59 | 57113.6827662037 | 2015-04-01 16:23:11 | 409011050 | 28.6706 | 20 | 28.6706 | 28.6706 | 0 | 28.6866 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.891712963 | 2016-08-17 21:24:04 | 56748 | 2014-04-01 00:00:00 | 57125.4008796296 | 2015-04-13 09:37:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011050/ | Quick Look | ![]() |
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486 | THE MOON | 138.793 | 11.1278 | 138.115741 | 11.336148 | 137.780525 | -4.592174 | 219.45159127 | 36.90361182 | 285.3988 | 56784.1992939815 | 2014-05-07 04:46:59 | 56784.3233101852 | 2014-05-07 07:45:34 | 809001060 | 6.4 | 45 | 6.4 | 6.4 | 0 | 6.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.2762 | 6.2762 | 10.7119 | 0 | PROCESSED | 57615.0611805556 | 2016-08-15 01:28:06 | 57218 | 2015-07-15 00:00:00 | 56852.5717708333 | 2014-07-14 13:43:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001060/ | Quick Look | ![]() |
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487 | MARS-P8 | 103.1682 | 25.1356 | 102.40007 | 25.197197 | 101.91311 | 2.237602 | 190.38738197 | 11.42154102 | 298.1062 | 54559.9031365741 | 2008-04-03 21:40:31 | 54560.0072222222 | 2008-04-04 00:10:24 | 403006080 | 2.7489 | 100 | 2.7538 | 2.7578 | 0 | 2.7489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2.2864 | 2.2864 | 8.984 | 0 | PROCESSED | 57542.0500578704 | 2016-06-03 01:12:05 | 54953 | 2009-05-02 00:00:00 | 54577.1637615741 | 2008-04-21 03:55:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006080/ | Quick Look | ![]() |
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488 | CIZA J2242.8+5301 | 340.7602 | 53.1616 | 340.242904 | 52.89922 | 13.612188 | 54.382245 | 104.28022824 | -4.9963098 | 17.994 | 55770.5553703704 | 2011-07-28 13:19:44 | 55772.8210185185 | 2011-07-30 19:42:16 | 806001010 | 122.9419 | 120 | 122.9499 | 122.9499 | 0 | 122.9419 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134.8043 | 134.8043 | 195.7079 | 1 | PROCESSED | 57602.7365393518 | 2016-08-02 17:40:37 | 56162 | 2012-08-23 00:00:00 | 55792.3410069445 | 2011-08-19 08:11:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060014 | Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | SHO NISHINO | JAP | 6 | AO6 | SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806001010/ | Quick Look | ![]() |
489 | A2319NORTH | 290.2404 | 44.0121 | 289.851853 | 43.916672 | 305.965056 | 64.946826 | 75.73364984 | 13.56775034 | 191.4804 | 55925.1947222222 | 2011-12-30 04:40:24 | 55927.5001273148 | 2012-01-01 12:00:11 | 806014010 | 104.7893 | 100 | 104.8293 | 104.7893 | 0 | 104.8293 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 1.8661 | 0 | PROCESSED | 57604.2771064815 | 2016-08-04 06:39:02 | 56340 | 2013-02-17 00:00:00 | 55973.7475115741 | 2012-02-16 17:56:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060044 | We propose the observations of the north subgroup region in the A2319 cluster with Suzaku to investigate dynamical status and particle acceleration process 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 determine the radial velocity of the ICM in the north subgroup region, and compare it with that in the central region which has been already determined from the AO1 data (Sugawara et al. 2009). Using these results and optical observational data of member galaxies, we will determine dynamical status of the ICM and get implications on the particle acceleration process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MOTOKAZU TAKIZAWA | JAP | 6 | AO6 | DYNAMICAL STATUS OF THE HOT GAS AROUND THE NORTH SUBGROUP IN THE A2319 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806014010/ | Quick Look | ![]() |
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490 | COMA OUTSKIRTS2 | 195.8535 | 28.5112 | 195.253601 | 28.779358 | 182.053697 | 32.234375 | 61.20140467 | 87.01280614 | 116.0004 | 55901.4349189815 | 2011-12-06 10:26:17 | 55901.9223842593 | 2011-12-06 22:08:14 | 806021010 | 20.3577 | 20 | 20.3617 | 20.3577 | 0 | 20.3648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.1946 | 19.1946 | 42.114 | 0 | PROCESSED | 57604.0414351852 | 2016-08-04 00:59:40 | 56282 | 2012-12-21 00:00:00 | 55914.2609375 | 2011-12-19 06:15:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806021010/ | Quick Look | ![]() |
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491 | MARS-P20 | 103.6685 | 25.0732 | 102.900981 | 25.137167 | 102.37032 | 2.21732 | 190.63848879 | 11.80707935 | 298.2779 | 54560.9100347222 | 2008-04-04 21:50:27 | 54560.9932175926 | 2008-04-04 23:50:14 | 403006200 | 1.849 | 100 | 1.849 | 1.849 | 0 | 1.849 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.222 | 1.222 | 7.1839 | 0 | PROCESSED | 57542.0733101852 | 2016-06-03 01:45:34 | 54953 | 2009-05-02 00:00:00 | 54578.0575231482 | 2008-04-22 01:22:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006200/ | Quick Look | ![]() |
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492 | SN1006 NE-Rim | 225.9645 | -41.7797 | 225.146779 | -41.584709 | 235.587114 | -23.452842 | 327.82254414 | 14.6038019 | 294.6606 | 53622.1683217593 | 2005-09-09 04:02:23 | 53623.5835532407 | 2005-09-10 14:00:19 | 100019020 | 42.8442 | 50 | 42.8442 | 42.8526 | 42.8522 | 42.8482 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.6156 | 37.6156 | 122.196 | 7 | PROCESSED | 57527.2923611111 | 2016-05-19 07:01:00 | 54247 | 2007-05-27 00:00:00 | 54034.9646875 | 2006-10-26 23:09:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | SN1006 observation with XIS and HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019020/ | Quick Look | ![]() |
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493 | KS1741-293(GCBGD2) | 266.2067 | -29.3539 | 265.409831 | -29.333545 | 266.666806 | -5.956639 | 359.55327497 | -0.0701996 | 265.0162 | 53643.254537037 | 2005-09-30 06:06:32 | 53643.3203703704 | 2005-09-30 07:41:20 | 100037030 | 2.97 | 5 | 2.994 | 2.986 | 2.978 | 2.97 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.8244 | 2.8244 | 5.6799 | 0 | PROCESSED | 57527.4480439815 | 2016-05-19 10:45:11 | 54247 | 2007-05-27 00:00:00 | 54035.7774189815 | 2006-10-27 18:39:29 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037030/ | Quick Look | ![]() |
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494 | Sgr_A_East | 266.5133 | -28.9266 | 265.719082 | -28.907738 | 266.92496 | -5.522692 | 0.05752244 | -0.07594372 | 264.7159 | 53643.3215393518 | 2005-09-30 07:43:01 | 53644.2648611111 | 2005-10-01 06:21:24 | 100037040 | 42.9176 | 50 | 42.9576 | 42.9616 | 42.9176 | 42.9392 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.4533 | 39.4533 | 81.494 | 1 | PROCESSED | 57527.4753356482 | 2016-05-19 11:24:29 | 54247 | 2007-05-27 00:00:00 | 54035.7619675926 | 2006-10-27 18:17:14 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037040/ | Quick Look | ![]() |
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495 | MARS-P27 | 103.964 | 25.0399 | 103.196825 | 25.105264 | 102.640165 | 2.209619 | 190.78318678 | 12.0366945 | 298.3836 | 54561.4933217593 | 2008-04-05 11:50:23 | 54561.5418171296 | 2008-04-05 13:00:13 | 403006270 | 1.0998 | 100 | 1.1078 | 1.0998 | 0 | 1.1158 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.0935 | 1.0935 | 4.1839 | 0 | PROCESSED | 57542.2332175926 | 2016-06-03 05:35:50 | 54953 | 2009-05-02 00:00:00 | 54578.1251273148 | 2008-04-22 03:00:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006270/ | Quick Look | ![]() |
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496 | RX J1712.6-2414 | 258.1492 | -24.2444 | 257.386071 | -24.185404 | 259.195725 | -1.246505 | 359.8664305 | 8.74215246 | 94.4586 | 54889.4875925926 | 2009-02-27 11:42:08 | 54892.2710532407 | 2009-03-02 06:30:19 | 403021010 | 110.4813 | 100 | 110.4893 | 110.4813 | 0 | 110.4893 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.4584 | 89.4584 | 240.4418 | 4 | PROCESSED | 57545.7503587963 | 2016-06-06 18:00:31 | 55330 | 2010-05-14 00:00:00 | 54908.5588310185 | 2009-03-18 13:24:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEYUKI MORI | JAP | 3 | AO3 | ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403021010/ | Quick Look | ![]() |
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497 | HESS J1356-645 2 | 208.8016 | -64.5041 | 207.885224 | -64.258991 | 235.51443 | -48.210014 | 309.72820731 | -2.47708999 | 123.7329 | 56340.1852430556 | 2013-02-17 04:26:45 | 56341.4863425926 | 2013-02-18 11:40:20 | 507020010 | 51.2594 | 50 | 51.2636 | 51.2594 | 0 | 51.2594 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.1505 | 45.1505 | 112.4059 | 2 | PROCESSED | 57610.6176157407 | 2016-08-10 14:49:22 | 56718 | 2014-03-02 00:00:00 | 56352.5089930556 | 2013-03-01 12:12:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAHISA FUJINAGA | JAP | 7 | AO7 | OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507020010/ | Quick Look | ![]() |
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498 | RXJ1713-3946 | 257.7765 | -39.428 | 256.912609 | -39.366986 | 260.174712 | -16.402181 | 347.32530765 | 0.10490445 | 268.0003 | 53990.7111689815 | 2006-09-12 17:04:05 | 53991.0488888889 | 2006-09-13 01:10:24 | 501067010 | 21.1796 | 20 | 21.1876 | 21.1796 | 21.1931 | 21.1956 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21.9861 | 21.9861 | 29.1679 | 0 | PROCESSED | 57535.5530902778 | 2016-05-27 13:16:27 | 54526 | 2008-03-01 00:00:00 | 54020.8250925926 | 2006-10-12 19:48:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501067010/ | Quick Look | ![]() |
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499 | G1.9+0.3 | 267.1951 | -27.1633 | 266.411742 | -27.147772 | 267.489777 | -3.746686 | 1.87759006 | 0.32236452 | 104.4114 | 55643.1608217593 | 2011-03-23 03:51:35 | 55645.2856481482 | 2011-03-25 06:51:20 | 505053010 | 100.9235 | 100 | 100.9235 | 100.9315 | 0 | 100.9315 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.4251 | 83.4251 | 183.5657 | 1 | PROCESSED | 57601.3345833333 | 2016-08-01 08:01:48 | 56025 | 2012-04-08 00:00:00 | 55658.2502546296 | 2011-04-07 06:00:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 5 | AO5 | INVESTIGATION OF THE YOUNGEST SNR G1.9+0.3 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505053010/ | Quick Look | ![]() |
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500 | PSR J1429-5911 | 217.5051 | -59.1899 | 216.584342 | -58.967616 | 237.077372 | -41.598198 | 315.26780851 | 1.30018252 | 101.124 | 55588.2265625 | 2011-01-27 05:26:15 | 55588.7001157407 | 2011-01-27 16:48:10 | 405012010 | 30.3824 | 30 | 30.3904 | 30.3984 | 0 | 30.3824 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28.7923 | 28.7923 | 40.9039 | 0 | PROCESSED | 57600.7562384259 | 2016-07-31 18:08:59 | 55968 | 2012-02-11 00:00:00 | 55602.1404513889 | 2011-02-10 03:22:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405012010/ | Quick Look | ![]() |
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501 | BG CMI | 112.8488 | 9.8847 | 112.163161 | 9.991257 | 113.00147 | -11.750081 | 208.51997296 | 13.31865509 | 292.793 | 54932.5078703704 | 2009-04-11 12:11:20 | 54933.5710532407 | 2009-04-12 13:42:19 | 404029010 | 47.0791 | 40 | 47.0871 | 47.0791 | 0 | 47.0871 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45.0346 | 45.0346 | 91.808 | 2 | PROCESSED | 57546.1223958333 | 2016-06-07 02:56:15 | 55324 | 2010-05-08 00:00:00 | 54949.5279050926 | 2009-04-28 12:40:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404029010/ | Quick Look | ![]() |
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502 | XSS J17223-7301 | 259.6949 | -73.4263 | 258.137466 | -73.372744 | 265.419963 | -50.147658 | 319.10640118 | -19.70481928 | 106.6643 | 55302.152650463 | 2010-04-16 03:39:49 | 55302.5939467593 | 2010-04-16 14:15:17 | 405033010 | 33.3861 | 30 | 33.3861 | 33.3861 | 0 | 33.3861 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.5889 | 25.5889 | 38.1279 | 0 | PROCESSED | 57551.2373726852 | 2016-06-12 05:41:49 | 55692 | 2011-05-11 00:00:00 | 55326.1437731482 | 2010-05-10 03:27:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405033010/ | Quick Look | ![]() |
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503 | AQL X-1 | 287.8278 | 0.5718 | 287.189492 | 0.488033 | 289.388601 | 22.82037 | 35.71173466 | -4.15890942 | 243.2618 | 55858.7269328704 | 2011-10-24 17:26:47 | 55859.5786921296 | 2011-10-25 13:53:19 | 406010030 | 8.495 | 40 | 8.495 | 9.5383 | 0 | 9.5566 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36.4768 | 36.4768 | 73.5819 | 2 | PROCESSED | 57603.6460416667 | 2016-08-03 15:30:18 | 56241 | 2012-11-10 00:00:00 | 55874.1380555556 | 2011-11-09 03:18:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUTAKA YAMAOKA | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010030/ | Quick Look | ![]() |
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504 | OAO1657-415 | 255.2026 | -41.6667 | 254.323073 | -41.593508 | 258.36169 | -18.820662 | 344.36019061 | 0.31327103 | 285.9012 | 55830.3988425926 | 2011-09-26 09:34:20 | 55832.6667939815 | 2011-09-28 16:00:11 | 406011010 | 84.7299 | 80 | 84.7337 | 84.7299 | 0 | 84.7417 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.5885 | 74.5885 | 195.9297 | 2 | PROCESSED | 57603.3220023148 | 2016-08-03 07:43:41 | 56226 | 2012-10-26 00:00:00 | 55858.2768518518 | 2011-10-24 06:38:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROKAZU ODAKA | JAP | 6 | AO6 | WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406011010/ | Quick Look | ![]() |
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505 | GC SOUTH | 266.5016 | -29.1694 | 265.705845 | -29.150477 | 266.920624 | -5.765664 | 359.84485124 | -0.1935349 | 265.0006 | 54004.5960185185 | 2006-09-26 14:18:16 | 54007.8925231482 | 2006-09-29 21:25:14 | 501008010 | 129.5773 | 130 | 129.5773 | 129.5773 | 129.5773 | 129.5773 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111.2591 | 111.2591 | 284.8038 | 5 | PROCESSED | 57535.7712731482 | 2016-05-27 18:30:38 | 54744 | 2008-10-05 00:00:00 | 54021.0929050926 | 2006-10-13 02:13:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | 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 | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501008010/ | Quick Look | ![]() |
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506 | HESS J1745-303 | 266.2629 | -30.3722 | 265.459457 | -30.352101 | 266.742769 | -6.973282 | 358.71029443 | -0.64354718 | 263.6011 | 54015.0950462963 | 2006-10-07 02:16:52 | 54016.4300810185 | 2006-10-08 10:19:19 | 501010010 | 50.6707 | 50 | 50.6707 | 50.6707 | 50.6707 | 50.6707 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 45.6897 | 45.6897 | 115.3119 | 1 | PROCESSED | 57535.8009837963 | 2016-05-27 19:13:25 | 54526 | 2008-03-01 00:00:00 | 54021.698587963 | 2006-10-13 16:45:58 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYO YAMAZAKI | JAP | 1 | AO1 | X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501010010/ | Quick Look | ![]() |
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507 | 1RXSJ175911.0-344921 | 269.7922 | -34.8194 | 268.957803 | -34.816359 | 269.8163 | -11.378443 | 356.38251758 | -5.46102238 | 72.1205 | 55993.9029513889 | 2012-03-07 21:40:15 | 55994.912650463 | 2012-03-08 21:54:13 | 406019010 | 40.1813 | 40 | 40.1813 | 40.1813 | 0 | 40.1813 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.751 | 34.751 | 87.2339 | 1 | PROCESSED | 57604.8358564815 | 2016-08-04 20:03:38 | 56385 | 2013-04-03 00:00:00 | 56016.6680787037 | 2012-03-30 16:02:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEYUKI MORI | JAP | 6 | AO6 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406019010/ | Quick Look | ![]() |
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508 | PSR B1259-63 | 195.6777 | -63.8873 | 194.888189 | -63.618658 | 227.727854 | -50.938694 | 304.1721261 | -1.04270018 | 282.6527 | 54292.6291319444 | 2007-07-11 15:05:57 | 54293.1910763889 | 2007-07-12 04:35:09 | 402014030 | 22.7217 | 20 | 22.7217 | 22.7217 | 0 | 22.7217 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.2808 | 24.2808 | 48.5459 | 0 | PROCESSED | 57539.1606712963 | 2016-05-31 03:51:22 | 54707 | 2008-08-29 00:00:00 | 54339.0273842593 | 2007-08-27 00:39:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014030/ | Quick Look | ![]() |
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509 | CYGNUS_LOOP_P7 | 312.0838 | 30.7678 | 311.566097 | 30.58216 | 326.462182 | 46.307536 | 73.70103145 | -8.0534172 | 239.9966 | 54416.1673032407 | 2007-11-12 04:00:55 | 54416.7223263889 | 2007-11-12 17:20:09 | 501018010 | 24.1545 | 22 | 24.1545 | 24.1545 | 0 | 24.1545 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.861 | 18.861 | 47.92 | 0 | PROCESSED | 57540.4878587963 | 2016-06-01 11:42:31 | 54798 | 2008-11-28 00:00:00 | 54430.1343287037 | 2007-11-26 03:13:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501018010/ | Quick Look | ![]() |
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510 | 1RXSJ165256.3-264503 | 253.236 | -26.7533 | 252.46137 | -26.671186 | 255.025143 | -4.179065 | 355.1420085 | 10.81079439 | 277.5876 | 54337.0024421296 | 2007-08-25 00:03:31 | 54338.0419444444 | 2007-08-26 01:00:24 | 402004010 | 49.5822 | 40 | 49.5822 | 49.5822 | 0 | 49.5822 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6581 | 46.6581 | 89.7779 | 2 | PROCESSED | 57539.6777083333 | 2016-05-31 16:15:54 | 54723 | 2008-09-14 00:00:00 | 54350.4155092593 | 2007-09-07 09:58:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEYUKI MORI | JAP | 2 | AO2 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402004010/ | Quick Look | ![]() |
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511 | PSR B1259-63 | 195.6402 | -63.8787 | 194.8511 | -63.61001 | 227.698758 | -50.941899 | 304.15600524 | -1.03339065 | 289.9992 | 54315.2640856482 | 2007-08-03 06:20:17 | 54316.0419444444 | 2007-08-04 01:00:24 | 402014060 | 24.0388 | 20 | 24.0388 | 24.0388 | 0 | 24.0388 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.5808 | 21.5808 | 67.1959 | 1 | PROCESSED | 57539.3969675926 | 2016-05-31 09:31:38 | 54722 | 2008-09-13 00:00:00 | 54347.6946527778 | 2007-09-04 16:40:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014060/ | Quick Look | ![]() |
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512 | HESS J1825-137 | 276.5031 | -13.6997 | 275.794781 | -13.729527 | 276.397624 | 9.596588 | 17.87105596 | -0.70261201 | 269.3213 | 54025.8175462963 | 2006-10-17 19:37:16 | 54027.1682291667 | 2006-10-19 04:02:15 | 501044010 | 50.293 | 50 | 50.293 | 50.293 | 50.293 | 50.293 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.9557 | 42.9557 | 116.694 | 1 | PROCESSED | 57535.8789351852 | 2016-05-27 21:05:40 | 54526 | 2008-03-01 00:00:00 | 54055.4418634259 | 2006-11-16 10:36:17 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501044010/ | Quick Look | ![]() |
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513 | RXJ1713-3946 | 257.7744 | -39.7271 | 256.908127 | -39.666071 | 260.20044 | -16.700257 | 347.08325974 | -0.07081205 | 268.0001 | 53990.3113310185 | 2006-09-12 07:28:19 | 53990.7106944444 | 2006-09-12 17:03:24 | 501066010 | 20.9207 | 20 | 20.9407 | 20.9207 | 20.926 | 20.9447 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.699 | 20.699 | 34.504 | 1 | PROCESSED | 57535.5600347222 | 2016-05-27 13:26:27 | 54526 | 2008-03-01 00:00:00 | 54020.8077546296 | 2006-10-12 19:23:10 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501066010/ | Quick Look | ![]() |
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514 | GALACTIC CENTER | 265.5037 | -30.2156 | 264.701457 | -30.191826 | 266.078204 | -6.8356 | 358.49956421 | -0.00336241 | 269.0005 | 54018.2813541667 | 2006-10-10 06:45:09 | 54018.887662037 | 2006-10-10 21:18:14 | 501052010 | 19.2451 | 20 | 19.2611 | 19.2611 | 19.2531 | 19.2451 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.0462 | 16.0462 | 52.3799 | 1 | PROCESSED | 57535.818275463 | 2016-05-27 19:38:19 | 54735 | 2008-09-26 00:00:00 | 54053.5074537037 | 2006-11-14 12:10:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501052010/ | Quick Look | ![]() |
515 | H1743-322 | 266.5662 | -32.2338 | 265.750329 | -32.21514 | 267.05149 | -8.827747 | 357.25541352 | -1.83396197 | 273.6881 | 56210.6462268518 | 2012-10-10 15:30:34 | 56211.5862731482 | 2012-10-11 14:04:14 | 407005020 | 21.1922 | 40 | 21.1922 | 21.1922 | 0 | 21.1922 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 41.517 | 41.517 | 81.2159 | 2 | PROCESSED | 57607.7447337963 | 2016-08-07 17:52:25 | 56595 | 2013-10-30 00:00:00 | 56226.5882291667 | 2012-10-26 14:07:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005020/ | Quick Look | ![]() |
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516 | XTE J1855-206 | 283.8765 | -2.601 | 283.223287 | -2.666237 | 284.773693 | 20.130658 | 31.07954127 | -2.09022498 | 75.074 | 57134.7127199074 | 2015-04-22 17:06:19 | 57137.3453125 | 2015-04-25 08:17:15 | 409022010 | 87.725 | 90 | 87.725 | 89.3274 | 0 | 89.3194 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1026157407 | 2016-08-18 02:27:46 | 57593 | 2016-07-24 00:00:00 | 57224.4343171296 | 2015-07-21 10:25:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090101 | Most of High mass X-ray binaries (HMXBs) have strong magnetic fields (~10^12 G) and detected cyclotron resonance scattering features (CRSFs). Many HMXBs with CRSFs have been observed by Suzaku and we derived a new method for estimating magnetic field strength using the observational data. In this observation, we try to observe candidates of strongly magnetized neutron star in HMXBs, EXO 1722-363 and XTE J1855-206 and examine the method. | GALACTIC POINT SOURCES | 4 | C | MAKOTO SASANO | JAP | 9 | AO9 | EXAMINATION OF A NEW METHOD FOR ESTIMATING MAGNETIC FIELD STRENGTH WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409022010/ | Quick Look | ![]() |
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517 | SWIFT J0601.9-8636 | 91.1523 | -86.6779 | 95.292028 | -86.662252 | 269.78546 | -69.879444 | 299.2555588 | -27.75439578 | 292.1727 | 53838.6834259259 | 2006-04-13 16:24:08 | 53839.0779976852 | 2006-04-14 01:52:19 | 701018010 | 19.7657 | 20 | 19.7817 | 19.7817 | 19.7657 | 19.7737 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.6614 | 16.6614 | 34.0599 | 0 | PROCESSED | 57533.4511226852 | 2016-05-25 10:49:37 | 54397 | 2007-10-24 00:00:00 | 53905.4682060185 | 2006-06-19 11:14:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701018010/ | Quick Look | ![]() |
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518 | HEN 3-461 | 159.7779 | -51.4088 | 159.258813 | -51.147936 | 190.933881 | -53.401362 | 282.90269516 | 6.2428626 | 116.1715 | 56278.1336342593 | 2012-12-17 03:12:26 | 56278.906400463 | 2012-12-17 21:45:13 | 407007010 | 45.7348 | 40 | 45.7348 | 45.7348 | 0 | 45.7348 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6774 | 46.6774 | 66.7619 | 0 | PROCESSED | 57608.3071990741 | 2016-08-08 07:22:22 | 56018 | 2012-04-01 00:00:00 | 56303.5505902778 | 2013-01-11 13:12:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | ROMANUS EZE | JAP | 7 | AO7 | SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407007010/ | Quick Look | ![]() |
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519 | AX J1622.1-5005 | 245.5334 | -50.0932 | 244.591386 | -49.975777 | 252.45498 | -28.129926 | 333.60606211 | -0.20489946 | 274.3812 | 56160.9968402778 | 2012-08-21 23:55:27 | 56161.9398148148 | 2012-08-22 22:33:20 | 407018010 | 39.1263 | 40 | 40.5366 | 40.5366 | 0 | 39.1263 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.476 | 37.476 | 81.4619 | 0 | PROCESSED | 57606.9317824074 | 2016-08-06 22:21:46 | 56667 | 2014-01-10 00:00:00 | 56300.5637731482 | 2013-01-08 13:31:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUO MAKISHIMA | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407018010/ | Quick Look | ![]() |
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520 | GX 339-4 | 255.7293 | -48.7348 | 254.78204 | -48.663918 | 259.585808 | -25.807191 | 338.99236079 | -4.30539701 | 107.9544 | 54915.3430555556 | 2009-03-25 08:14:00 | 54916.2711111111 | 2009-03-26 06:30:24 | 403011020 | 39.0792 | 40 | 39.1165 | 39.0792 | 0 | 39.1165 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34.7852 | 34.7852 | 80.1658 | 0 | PROCESSED | 57545.909849537 | 2016-06-06 21:50:11 | 55330 | 2010-05-14 00:00:00 | 54930.1609490741 | 2009-04-09 03:51:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011020/ | Quick Look | ![]() |
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521 | H1743-322 | 266.5676 | -32.2352 | 265.751719 | -32.216547 | 267.052722 | -8.829118 | 357.25483145 | -1.83570092 | 273.6877 | 56204.7822800926 | 2012-10-04 18:46:29 | 56205.6078240741 | 2012-10-05 14:35:16 | 407005010 | 20.811 | 40 | 20.811 | 20.811 | 0 | 20.811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4337 | 42.4337 | 71.3219 | 0 | PROCESSED | 57607.2960300926 | 2016-08-07 07:06:17 | 56595 | 2013-10-30 00:00:00 | 56226.5596296296 | 2012-10-26 13:25:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407005010/ | Quick Look | ![]() |
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522 | THE MOON | 19.4299 | 8.4288 | 18.775956 | 8.165731 | 21.110635 | 0.205257 | 134.00151394 | -53.87712274 | 73.8016 | 56856.6577777778 | 2014-07-18 15:47:12 | 56856.7905439815 | 2014-07-18 18:58:23 | 809001110 | 6.3696 | 45 | 6.3856 | 6.3696 | 0 | 6.3936 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3999305556 | 2016-08-15 09:35:54 | 57233 | 2015-07-30 00:00:00 | 56867.740474537 | 2014-07-29 17:46:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001110/ | Quick Look | ![]() |
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523 | THE MOON | 20.9888 | 9.1871 | 20.332488 | 8.926606 | 22.823039 | 0.333671 | 136.29340358 | -52.83899755 | 73.8 | 56856.7918055556 | 2014-07-18 19:00:12 | 56856.8877662037 | 2014-07-18 21:18:23 | 809001120 | 4.2623 | 45 | 4.2703 | 4.2623 | 0 | 4.2783 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.400775463 | 2016-08-15 09:37:07 | 57233 | 2015-07-30 00:00:00 | 56867.7339930556 | 2014-07-29 17:36:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001120/ | Quick Look | ![]() |
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524 | MARS-P5 | 103.045 | 25.1496 | 102.276729 | 25.210613 | 101.800688 | 2.241477 | 190.32670814 | 11.32616716 | 298.0638 | 54559.6600462963 | 2008-04-03 15:50:28 | 54559.7432407407 | 2008-04-03 17:50:16 | 403006050 | 1.9562 | 100 | 1.9562 | 1.9562 | 0 | 1.9562 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1.9926 | 1.9926 | 7.1679 | 0 | PROCESSED | 57542.0421527778 | 2016-06-03 01:00:42 | 54953 | 2009-05-02 00:00:00 | 54577.1345486111 | 2008-04-21 03:13:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006050/ | Quick Look | ![]() |
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525 | MARS-P9 | 103.2195 | 25.1275 | 102.451442 | 25.18934 | 101.960133 | 2.233755 | 190.41473742 | 11.46031922 | 298.1247 | 54560.0073726852 | 2008-04-04 00:10:37 | 54560.0766666667 | 2008-04-04 01:50:24 | 403006090 | 2.1506 | 100 | 2.1506 | 2.1746 | 0 | 2.1506 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.8919 | 1.8919 | 5.9759 | 0 | PROCESSED | 57542.0488888889 | 2016-06-03 01:10:24 | 54953 | 2009-05-02 00:00:00 | 54577.1428009259 | 2008-04-21 03:25:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006090/ | Quick Look | ![]() |
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526 | V4641 SGR | 274.8371 | -25.4052 | 274.064433 | -25.426808 | 274.361493 | -2.037678 | 6.77442002 | -4.78571714 | 84.0004 | 56741.9737152778 | 2014-03-25 23:22:09 | 56744.8959722222 | 2014-03-28 21:30:12 | 408002010 | 49.2237 | 100 | 49.2237 | 49.2706 | 0 | 49.2242 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 89.7439 | 89.7439 | 252.4556 | 1 | PROCESSED | 57614.1632291667 | 2016-08-14 03:55:03 | 57190 | 2015-06-17 00:00:00 | 56821.8685532407 | 2014-06-13 20:50:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080009 | 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 | KAZUTAKA YAMAOKA | JAP | 8 | AO8-TOO | THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408002010/ | Quick Look | ![]() |
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527 | MARS-P14 | 103.4188 | 25.1057 | 102.650967 | 25.168485 | 102.141964 | 2.228596 | 190.5119865 | 11.61511049 | 298.1941 | 54560.410150463 | 2008-04-04 09:50:37 | 54560.4933333333 | 2008-04-04 11:50:24 | 403006140 | 4.8252 | 100 | 4.8492 | 4.8252 | 0 | 4.8572 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.7214 | 3.7214 | 7.1759 | 0 | PROCESSED | 57542.063125 | 2016-06-03 01:30:54 | 54953 | 2009-05-02 00:00:00 | 54577.9434722222 | 2008-04-21 22:38:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006140/ | Quick Look | ![]() |
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528 | VELA JR P9 | 133.4161 | -45.7633 | 132.983285 | -45.572688 | 159.43463 | -59.191033 | 266.00615013 | -0.63304204 | 347.0009 | 54287.7015856482 | 2007-07-06 16:50:17 | 54287.9516666667 | 2007-07-06 22:50:24 | 502031010 | 13.2524 | 10 | 13.2684 | 13.2524 | 0 | 13.2684 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.8877 | 9.8877 | 21.5999 | 0 | PROCESSED | 57539.1152546296 | 2016-05-31 02:45:58 | 54703 | 2008-08-25 00:00:00 | 54333.4413657407 | 2007-08-21 10:35:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502031010/ | Quick Look | ![]() |
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529 | VELA JR P5 | 132.9105 | -45.488 | 132.477402 | -45.299188 | 158.564821 | -59.145564 | 265.56829981 | -0.72857938 | 347.002 | 54286.4486458333 | 2007-07-05 10:46:03 | 54286.7502777778 | 2007-07-05 18:00:24 | 502027010 | 10.977 | 10 | 10.977 | 10.977 | 0 | 10.977 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.7858 | 10.7858 | 26.0539 | 0 | PROCESSED | 57539.1013541667 | 2016-05-31 02:25:57 | 54696 | 2008-08-18 00:00:00 | 54328.4697800926 | 2007-08-16 11:16:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502027010/ | Quick Look | ![]() |
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530 | VELA JR P12 | 132.2515 | -46.051 | 131.824752 | -45.864543 | 158.385677 | -59.866647 | 265.71195175 | -1.4410688 | 347.0011 | 54289.0722106482 | 2007-07-08 01:43:59 | 54289.4078009259 | 2007-07-08 09:47:14 | 502034010 | 9.9479 | 10 | 9.9479 | 9.9479 | 0 | 9.9479 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.494 | 10.494 | 28.9839 | 0 | PROCESSED | 57539.1227546296 | 2016-05-31 02:56:46 | 54696 | 2008-08-18 00:00:00 | 54328.4792939815 | 2007-08-16 11:30:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502034010/ | Quick Look | ![]() |
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531 | HE FOCUSING CONE | 49.5833 | 10.9603 | 48.902196 | 10.778547 | 50.105188 | -7.060313 | 170.9618047 | -37.8533007 | 73.6953 | 55410.7011921296 | 2010-08-02 16:49:43 | 55413.1439699074 | 2010-08-05 03:27:19 | 505061010 | 101.9651 | 100 | 101.9731 | 101.9731 | 0 | 101.9651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.1452 | 89.1452 | 211.0459 | 2 | PROCESSED | 57552.9158796296 | 2016-06-13 21:58:52 | 55808 | 2011-09-04 00:00:00 | 55441.4075694444 | 2010-09-02 09:46:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI YOSHITAKE | JAP | 5 | AO5 | OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505061010/ | Quick Look | ![]() |
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532 | MARS-P22 | 103.7541 | 25.0677 | 102.986656 | 25.132072 | 102.448087 | 2.219161 | 190.67657625 | 11.87528798 | 298.3117 | 54561.0767013889 | 2008-04-05 01:50:27 | 54561.1598842593 | 2008-04-05 03:50:14 | 403006220 | 4.0246 | 100 | 4.0406 | 4.0246 | 0 | 4.0476 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.102 | 4.102 | 7.1839 | 0 | PROCESSED | 57542.0781712963 | 2016-06-03 01:52:34 | 54953 | 2009-05-02 00:00:00 | 54578.0665625 | 2008-04-22 01:35:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006220/ | Quick Look | ![]() |
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533 | 4U 0614+091 | 94.2826 | 9.1348 | 93.597318 | 9.153924 | 94.364565 | -14.241394 | 200.88027144 | -3.36263018 | 270.7227 | 56737.0982291667 | 2014-03-21 02:21:27 | 56738.4584259259 | 2014-03-22 11:00:08 | 408009020 | 15.6689 | 60 | 15.8314 | 15.6689 | 0 | 15.8205 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 60.5574 | 60.5574 | 117.5018 | 2 | PROCESSED | 57614.0787152778 | 2016-08-14 01:53:21 | 57144 | 2015-05-02 00:00:00 | 56778.6809606482 | 2014-05-01 16:20:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080028 | We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB. | GALACTIC POINT SOURCES | 4 | B | SATOSHI SUGITA | JAP | 8 | AO8 | THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408009020/ | Quick Look | ![]() |
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534 | VELA JR P17 | 133.087 | -46.0455 | 132.657371 | -45.856052 | 159.351353 | -59.55196 | 266.0760896 | -0.98967894 | 347.0002 | 54291.7369444444 | 2007-07-10 17:41:12 | 54291.9238773148 | 2007-07-10 22:10:23 | 502039010 | 13.0326 | 10 | 13.0645 | 13.0646 | 0 | 13.0326 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.8272 | 8.8272 | 16.1439 | 0 | PROCESSED | 57539.1455555556 | 2016-05-31 03:29:36 | 54707 | 2008-08-29 00:00:00 | 54333.4040277778 | 2007-08-21 09:41:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502039010/ | Quick Look | ![]() |
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535 | HESS J0632+057 | 98.2456 | 5.8062 | 97.576893 | 5.844512 | 98.600946 | -17.388931 | 205.66072349 | -1.43796588 | 289.8173 | 54579.6856828704 | 2008-04-23 16:27:23 | 54580.6877199074 | 2008-04-24 16:30:19 | 403018010 | 44.076 | 40 | 44.076 | 44.076 | 0 | 44.076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.4758 | 41.4758 | 86.5658 | 0 | PROCESSED | 57542.3746643518 | 2016-06-03 08:59:31 | 54961 | 2009-05-10 00:00:00 | 54594.1596990741 | 2008-05-08 03:49:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 3 | AO3 | INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403018010/ | Quick Look | ![]() |
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536 | GC_G0.9+0.1 | 266.9332 | -28.1474 | 266.1438 | -28.130586 | 267.277369 | -4.735296 | 0.91503767 | 0.01290063 | 105.8953 | 54536.2637152778 | 2008-03-11 06:19:45 | 54540.229375 | 2008-03-15 05:30:18 | 502051010 | 138.7614 | 133 | 138.7614 | 138.7614 | 0 | 138.7614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122.2214 | 122.2214 | 342.5768 | 1 | PROCESSED | 57541.9299305556 | 2016-06-02 22:19:06 | 54919 | 2009-03-29 00:00:00 | 54550.6988078704 | 2008-03-25 16:46:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 2 | AO2 | SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502051010/ | Quick Look | ![]() |
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537 | SAGITTARIUS A* | 266.4166 | -29.0014 | 265.621928 | -28.982068 | 266.841834 | -5.599552 | 359.94961276 | -0.04264831 | 285.0058 | 56547.2597337963 | 2013-09-12 06:14:01 | 56547.6558101852 | 2013-09-12 15:44:22 | 408017020 | 19.276 | 20 | 19.2823 | 19.2901 | 0 | 19.276 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 21.0834 | 21.0834 | 34.218 | 0 | PROCESSED | 57612.6033796296 | 2016-08-12 14:28:52 | 56956 | 2014-10-26 00:00:00 | 56588.7462152778 | 2013-10-23 17:54:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017020/ | Quick Look | ![]() |
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538 | M17 EAST | 275.3895 | -16.2062 | 274.668063 | -16.230609 | 275.205572 | 7.137102 | 15.15230897 | -0.92571433 | 271.9996 | 54377.3569907407 | 2007-10-04 08:34:04 | 54380.0940277778 | 2007-10-07 02:15:24 | 502052010 | 114.5695 | 107 | 114.5775 | 114.5695 | 0 | 114.5775 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100.8873 | 100.8873 | 236.4498 | 3 | PROCESSED | 57540.2317939815 | 2016-06-01 05:33:47 | 54771 | 2008-11-01 00:00:00 | 54403.5436111111 | 2007-10-30 13:02:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAHIRO TSUJIMOTO | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502052010/ | Quick Look | ![]() |
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539 | VELA JR P32 | 133.3695 | -46.8865 | 132.945153 | -46.696038 | 160.585523 | -60.152729 | 266.8467839 | -1.37881435 | 347.0018 | 54655.3279166667 | 2008-07-08 07:52:12 | 54655.5648032407 | 2008-07-08 13:33:19 | 503044010 | 11.2649 | 10 | 11.2729 | 11.2649 | 0 | 11.2809 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.3375 | 8.3375 | 20.4559 | 0 | PROCESSED | 57543.0006828704 | 2016-06-04 00:00:59 | 55048 | 2009-08-05 00:00:00 | 54679.381087963 | 2008-08-01 09:08:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503044010/ | Quick Look | ![]() |
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540 | RXCJ0018.9-4051 | 4.7354 | -40.8551 | 4.113382 | -41.132744 | 344.925025 | -38.685562 | 326.87167276 | -74.72717506 | 232.4175 | 55161.0142708333 | 2009-11-26 00:20:33 | 55161.4169444444 | 2009-11-26 10:00:24 | 804004010 | 19.3278 | 10 | 19.3278 | 19.3278 | 0 | 19.3278 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.3198 | 13.3198 | 34.7839 | 1 | PROCESSED | 57549.5606481482 | 2016-06-10 13:27:20 | 55553 | 2010-12-23 00:00:00 | 55182.6506712963 | 2009-12-17 15:36:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804004010/ | Quick Look | ![]() |
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541 | ETA CARINAE | 161.1825 | -59.711 | 160.696763 | -59.447791 | 202.133764 | -58.970475 | 287.57247158 | -0.67238651 | 329.3001 | 56476.1821296296 | 2013-07-03 04:22:16 | 56479.0417361111 | 2013-07-06 01:00:06 | 408018010 | 97.524 | 180 | 97.524 | 97.524 | 0 | 97.524 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.8367 | 87.8367 | 247.0497 | 2 | PROCESSED | 57611.768912037 | 2016-08-11 18:27:14 | 56861 | 2014-07-23 00:00:00 | 56492.7286921296 | 2013-07-19 17:29:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080081 | Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms. | GALACTIC POINT SOURCES | 4 | B | TAKAYUKI YUASA | JAP | 8 | AO8 | DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018010/ | Quick Look | ![]() |
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542 | V2301 OPH | 270.155 | 8.1565 | 269.554142 | 8.157196 | 270.169577 | 31.596745 | 34.53366867 | 14.97765204 | 262.0679 | 56576.0003009259 | 2013-10-11 00:00:26 | 56577.3452314815 | 2013-10-12 08:17:08 | 408024020 | 53.1884 | 110 | 53.1884 | 53.1884 | 0 | 53.1884 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.2892 | 47.2892 | 116.1898 | 0 | PROCESSED | 57612.9583333333 | 2016-08-12 23:00:00 | 57184 | 2015-06-11 00:00:00 | 56631.6754282407 | 2013-12-05 16:12:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI HAYASHI | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024020/ | Quick Look | ![]() |
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543 | V2301 OPH | 270.1437 | 8.1764 | 269.542941 | 8.17715 | 270.156471 | 31.616658 | 34.54710657 | 14.99643028 | 71.9008 | 56752.9922800926 | 2014-04-05 23:48:53 | 56754.6945949074 | 2014-04-07 16:40:13 | 408024030 | 62.9253 | 57 | 62.9413 | 62.9253 | 0 | 62.9413 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.5037 | 56.5037 | 147.0677 | 1 | PROCESSED | 57614.2091666667 | 2016-08-14 05:01:12 | 57184 | 2015-06-11 00:00:00 | 56817.8149884259 | 2014-06-09 19:33:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | TAKAYUKI HAYASHI | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408024030/ | Quick Look | ![]() |
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544 | WR140 | 305.1942 | 43.809 | 304.771615 | 43.649401 | 327.418451 | 60.430238 | 80.92425741 | 4.10518752 | 220.5408 | 54812.4360069444 | 2008-12-12 10:27:51 | 54813.5523148148 | 2008-12-13 13:15:20 | 403032010 | 52.9106 | 40 | 52.9106 | 52.9106 | 0 | 52.9106 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 48.2609 | 48.2609 | 96.4318 | 0 | PROCESSED | 57544.9612847222 | 2016-06-05 23:04:15 | 55192 | 2009-12-27 00:00:00 | 54826.2481365741 | 2008-12-26 05:57:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITOMO MAEDA | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403032010/ | Quick Look | ![]() |
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545 | X 1630-472 | 248.5011 | -47.3955 | 247.580071 | -47.291357 | 254.086008 | -25.133666 | 336.90685721 | 0.25132488 | 88.6334 | 57080.103125 | 2015-02-27 02:28:30 | 57081.1542824074 | 2015-02-28 03:42:10 | 409007030 | 5.1108 | 40 | 5.128 | 5.1452 | 0 | 5.1108 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7393634259 | 2016-08-17 17:44:41 | 57458 | 2016-03-11 00:00:00 | 57091.4579513889 | 2015-03-10 10:59:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | 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 | YOSHIHIRO UEDA | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007030/ | Quick Look | ![]() |
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546 | SAGITTARIUS A* | 266.415 | -29.0091 | 265.620279 | -28.98976 | 266.840621 | -5.607284 | 359.94231116 | -0.0454652 | 105.8502 | 57103.3174537037 | 2015-03-22 07:37:08 | 57103.7690162037 | 2015-03-22 18:27:23 | 409011040 | 23.2422 | 20 | 23.2422 | 23.2465 | 0 | 23.2465 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8342824074 | 2016-08-17 20:01:22 | 56748 | 2014-04-01 00:00:00 | 57114.6078472222 | 2015-04-02 14:35:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011040/ | Quick Look | ![]() |
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547 | 1RXSJ013106.4+612035 | 22.7619 | 61.3591 | 21.928492 | 61.101677 | 49.598028 | 47.010357 | 127.66105316 | -1.14841945 | 76.8129 | 55765.7032175926 | 2011-07-23 16:52:38 | 55766.0182060185 | 2011-07-24 00:26:13 | 406034010 | 13.2963 | 20 | 13.2963 | 13.2963 | 0 | 13.2963 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.8829 | 15.8829 | 27.1999 | 0 | PROCESSED | 57602.6424884259 | 2016-08-02 15:25:11 | 56374 | 2013-03-23 00:00:00 | 55784.9886458333 | 2011-08-11 23:43:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMITSU TAKAHASHI | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406034010/ | Quick Look | ![]() |
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548 | 1RXSJ173916.2-214746 | 264.8155 | -21.7912 | 264.064028 | -21.764222 | 265.175612 | 1.563021 | 5.33311568 | 4.97377326 | 96.7097 | 57115.0060069444 | 2015-04-03 00:08:39 | 57115.2681712963 | 2015-04-03 06:26:10 | 409015010 | 12.328 | 12 | 12.349 | 12.3523 | 0 | 12.328 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8972800926 | 2016-08-17 21:32:05 | 57493 | 2016-04-15 00:00:00 | 57126.415625 | 2015-04-14 09:58:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 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 | B | HIDEYUKI MORI | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409015010/ | Quick Look | ![]() |
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549 | UX ARIETIS | 51.6466 | 28.6421 | 50.887812 | 28.467932 | 56.479497 | 9.555722 | 159.59610539 | -22.97107378 | 272.6966 | 55229.7116666667 | 2010-02-02 17:04:48 | 55231.7321064815 | 2010-02-04 17:34:14 | 404008010 | 87.7993 | 90 | 87.7993 | 87.7993 | 0 | 87.7993 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.7429 | 79.7429 | 174.5399 | 0 | PROCESSED | 57550.5166203704 | 2016-06-11 12:23:56 | 55616 | 2011-02-24 00:00:00 | 55249.830150463 | 2010-02-22 19:55:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIN-NOSUKE ISHIKAWA | JAP | 4 | AO4 | STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETIS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404008010/ | Quick Look | ![]() |
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550 | HESS J0632+057 | 98.2448 | 5.8057 | 97.576095 | 5.844008 | 98.600145 | -17.389477 | 205.66080027 | -1.43890266 | 289.9631 | 54941.5631944444 | 2009-04-20 13:31:00 | 54944.1542708333 | 2009-04-23 03:42:09 | 404027010 | 100.0343 | 100 | 100.0343 | 100.0343 | 0 | 100.0343 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.3918 | 82.3918 | 223.8419 | 6 | PROCESSED | 57546.2406481482 | 2016-06-07 05:46:32 | 55336 | 2010-05-20 00:00:00 | 54966.5323958333 | 2009-05-15 12:46:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 4 | AO4 | SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404027010/ | Quick Look | ![]() |
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551 | PERSEUS OFFSET-H | 50.3251 | 41.6598 | 49.495605 | 41.480554 | 58.942633 | 22.403293 | 150.73113668 | -12.9828544 | 270.0006 | 55595.9611458333 | 2011-02-03 23:04:03 | 55596.3536805556 | 2011-02-04 08:29:18 | 805048010 | 18.241 | 25 | 18.249 | 18.249 | 0 | 18.241 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.88 | 14.88 | 33.9039 | 0 | PROCESSED | 57600.8294560185 | 2016-07-31 19:54:25 | 55979 | 2012-02-22 00:00:00 | 55610.233287037 | 2011-02-18 05:35:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805048010/ | Quick Look | ![]() |
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552 | GC_LARGEPROJECT6 | 266.2992 | -29.9408 | 265.498546 | -29.920884 | 266.763082 | -6.541223 | 359.09468885 | -0.44519015 | 265.9621 | 54723.8160532407 | 2008-09-14 19:35:07 | 54725.0348842593 | 2008-09-16 00:50:14 | 503012010 | 57.6855 | 50 | 57.6935 | 57.6855 | 0 | 57.6981 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.9032 | 51.9032 | 105.2878 | 1 | PROCESSED | 57543.8433217593 | 2016-06-04 20:14:23 | 54557 | 2008-04-01 00:00:00 | 54780.6521643518 | 2008-11-10 15:39:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503012010/ | Quick Look | ![]() |
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553 | HESS_J1825-137_3 | 276.1966 | -13.9971 | 275.486722 | -14.025442 | 276.082794 | 9.312755 | 17.46909054 | -0.57831059 | 271.0001 | 54758.195775463 | 2008-10-19 04:41:55 | 54759.7917476852 | 2008-10-20 19:00:07 | 503030010 | 55.4996 | 50 | 55.4996 | 55.4996 | 0 | 55.4996 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.3252 | 47.3252 | 137.8379 | 1 | PROCESSED | 57544.2257407407 | 2016-06-05 05:25:04 | 55148 | 2009-11-13 00:00:00 | 54780.7804050926 | 2008-11-10 18:43:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAAKI TANAKA | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503030010/ | Quick Look | ![]() |
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554 | V1280 SCO | 254.4172 | -32.3368 | 253.607248 | -32.260102 | 256.681689 | -9.612724 | 351.33470039 | 6.5596985 | 97.7451 | 55605.3662615741 | 2011-02-13 08:47:25 | 55608.0501851852 | 2011-02-16 01:12:16 | 405029010 | 99.683 | 100 | 99.699 | 99.683 | 0 | 99.699 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.9306 | 86.9306 | 231.8739 | 2 | PROCESSED | 57600.9978472222 | 2016-07-31 23:56:54 | 55983 | 2012-02-26 00:00:00 | 55617.4142361111 | 2011-02-25 09:56:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | DAI TAKEI | JAP | 5 | AO5 | X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405029010/ | Quick Look | ![]() |
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555 | HESS J1800-240A | 270.4845 | -23.9659 | 269.719972 | -23.966397 | 270.433159 | -0.525758 | 6.13495239 | -0.62617494 | 86.9255 | 54558.6209606482 | 2008-04-02 14:54:11 | 54559.3266087963 | 2008-04-03 07:50:19 | 503025010 | 34.7822 | 30 | 34.7822 | 34.7902 | 0 | 34.7902 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7033 | 25.7033 | 60.9679 | 0 | PROCESSED | 57542.0259837963 | 2016-06-03 00:37:25 | 54953 | 2009-05-02 00:00:00 | 54574.0504861111 | 2008-04-18 01:12:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAAKI TANAKA | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503025010/ | Quick Look | ![]() |
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556 | HESS J1800-240C | 269.7173 | -24.0469 | 268.95232 | -24.043667 | 269.732245 | -0.606264 | 5.71665641 | -0.05804766 | 87.3071 | 54563.0147337963 | 2008-04-07 00:21:13 | 54563.6877662037 | 2008-04-07 16:30:23 | 503027010 | 30.9755 | 30 | 30.9755 | 30.9755 | 0 | 30.9755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.8155 | 27.8155 | 58.1239 | 1 | PROCESSED | 57542.2510185185 | 2016-06-03 06:01:28 | 54953 | 2009-05-02 00:00:00 | 54580.1897453704 | 2008-04-24 04:33:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAAKI TANAKA | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503027010/ | Quick Look | ![]() |
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557 | 24M2791 | 334.9577 | 63.2629 | 334.551329 | 63.011149 | 23.890285 | 63.530312 | 106.81877019 | 5.23758822 | 230.0008 | 55947.3704513889 | 2012-01-21 08:53:27 | 55948.0926388889 | 2012-01-22 02:13:24 | 406023010 | 34.6017 | 30 | 34.6177 | 34.6017 | 0 | 34.6097 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0595 | 35.0595 | 62.3919 | 0 | PROCESSED | 57604.5087847222 | 2016-08-04 12:12:39 | 56340 | 2013-02-17 00:00:00 | 55973.1102893518 | 2012-02-16 02:38:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASANORI OHNO | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406023010/ | Quick Look | ![]() |
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558 | VELA JR P23 | 132.7881 | -46.3947 | 132.362089 | -46.206312 | 159.378374 | -59.957558 | 266.21323714 | -1.3716571 | 347.0013 | 54652.3896759259 | 2008-07-05 09:21:08 | 54652.7710416667 | 2008-07-05 18:30:18 | 503035010 | 15.6901 | 10 | 15.6981 | 15.6901 | 0 | 15.7061 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.039 | 11.039 | 32.9439 | 1 | PROCESSED | 57542.9759490741 | 2016-06-03 23:25:22 | 55031 | 2009-07-19 00:00:00 | 54664.7904513889 | 2008-07-17 18:58:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503035010/ | Quick Look | ![]() |
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559 | PSR J0614-33 | 93.5386 | -33.5015 | 93.081964 | -33.485438 | 95.411067 | -56.876431 | 240.50300829 | -21.83180137 | 119.1484 | 55498.9719675926 | 2010-10-29 23:19:38 | 55499.6140740741 | 2010-10-30 14:44:16 | 405014010 | 31.2109 | 30 | 31.2109 | 31.2109 | 0 | 31.2109 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.3314 | 27.3314 | 55.4499 | 0 | PROCESSED | 57553.8985763889 | 2016-06-14 21:33:57 | 55875 | 2011-11-10 00:00:00 | 55509.0359722222 | 2010-11-09 00:51:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405014010/ | Quick Look | ![]() |
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560 | EMS0918 | 211.2948 | -61.3938 | 210.393622 | -61.154695 | 234.671242 | -44.951341 | 311.64055354 | 0.22486043 | 106.822 | 55589.5588310185 | 2011-01-28 13:24:43 | 55590.0834837963 | 2011-01-29 02:00:13 | 405025010 | 24.5425 | 20 | 24.5505 | 24.5425 | 0 | 24.5585 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.2811 | 23.2811 | 45.3099 | 1 | PROCESSED | 57600.7734606482 | 2016-07-31 18:33:47 | 55972 | 2012-02-15 00:00:00 | 55602.2015046296 | 2011-02-10 04:50:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405025010/ | Quick Look | ![]() |
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561 | VELA JR P35 | 132.966 | -46.9473 | 132.543542 | -46.75827 | 160.188354 | -60.35477 | 266.71715615 | -1.62954887 | 347.0008 | 54656.2642592593 | 2008-07-09 06:20:32 | 54656.5141087963 | 2008-07-09 12:20:19 | 503047010 | 11.5621 | 10 | 11.5861 | 11.5621 | 0 | 11.5941 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6198 | 9.6198 | 21.5839 | 0 | PROCESSED | 57543.0120486111 | 2016-06-04 00:17:21 | 55037 | 2009-07-25 00:00:00 | 54670.2319212963 | 2008-07-23 05:33:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503047010/ | Quick Look | ![]() |
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562 | HIGH LAT. DIFFUSE A | 246.1745 | 43.4846 | 245.775383 | 43.597905 | 228.822222 | 63.555652 | 68.4171583 | 44.39202319 | 129.9994 | 53780.2926388889 | 2006-02-14 07:01:24 | 53781.9640509259 | 2006-02-15 23:08:14 | 500027010 | 73.5787 | 70 | 73.5867 | 73.5867 | 73.5787 | 73.5867 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67.3993 | 67.3993 | 144.3979 | 3 | PROCESSED | 57533.0379976852 | 2016-05-25 00:54:43 | 54247 | 2007-05-27 00:00:00 | 54041.3110416667 | 2006-11-02 07:27:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027010/ | Quick Look | ![]() |
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563 | EMS1308 | 293.0393 | 19.2567 | 292.487947 | 19.148974 | 299.013622 | 40.405253 | 54.62289289 | 0.10827332 | 90.0001 | 55313.4365740741 | 2010-04-27 10:28:40 | 55313.9766203704 | 2010-04-27 23:26:20 | 405028010 | 23.8987 | 20 | 23.9067 | 23.9067 | 0 | 23.8987 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23.209 | 23.209 | 46.652 | 1 | PROCESSED | 57551.306400463 | 2016-06-12 07:21:13 | 55693 | 2011-05-12 00:00:00 | 55327.1789930556 | 2010-05-11 04:17:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405028010/ | Quick Look | ![]() |
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564 | GALACTIC CENTER | 266.0341 | -30.1068 | 265.232432 | -30.085596 | 266.53657 | -6.713302 | 358.83318764 | -0.33628911 | 269.0002 | 54019.4218402778 | 2006-10-11 10:07:27 | 54020.1446064815 | 2006-10-12 03:28:14 | 501057010 | 20.4884 | 20 | 20.4884 | 20.4964 | 20.4964 | 20.4964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.086 | 19.086 | 62.4379 | 0 | PROCESSED | 57535.8262037037 | 2016-05-27 19:49:44 | 54735 | 2008-09-26 00:00:00 | 54053.6059837963 | 2006-11-14 14:32:37 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501057010/ | Quick Look | ![]() |
565 | CYG X-1 | 299.5787 | 35.2024 | 299.108699 | 35.065978 | 313.648056 | 54.25343 | 71.3307159 | 3.0753508 | 59.5691 | 56419.0925578704 | 2013-05-07 02:13:17 | 56419.6071643518 | 2013-05-07 14:34:19 | 407015020 | 1.5124 | 20 | 3.2442 | 1.5124 | 0 | 21.48 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20.9258 | 20.9258 | 44.458 | 0 | PROCESSED | 57611.2625347222 | 2016-08-11 06:18:03 | 56808 | 2014-05-31 00:00:00 | 56442.9715509259 | 2013-05-30 23:19:02 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA YAMADA | JAP | 7 | AO7 | INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407015020/ | Quick Look | ![]() |
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566 | CYGNUS LOOP (P26) | 314.1252 | 30.3135 | 313.601346 | 30.1206 | 328.529731 | 45.204244 | 74.46090737 | -9.70687059 | 49.7995 | 54599.1203587963 | 2008-05-13 02:53:19 | 54599.5474421296 | 2008-05-13 13:08:19 | 503062010 | 16.9247 | 15 | 16.9247 | 16.9327 | 0 | 16.9327 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.441 | 15.441 | 36.892 | 1 | PROCESSED | 57542.5181944444 | 2016-06-03 12:26:12 | 54975 | 2009-05-24 00:00:00 | 54609.1293981482 | 2008-05-23 03:06:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503062010/ | Quick Look | ![]() |
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567 | GC SOUTH BGD | 266.1893 | -28.9082 | 265.395265 | -28.887768 | 266.639666 | -5.511508 | 359.92534776 | 0.17564926 | 265.0003 | 54007.8931365741 | 2006-09-29 21:26:07 | 54009.2884143518 | 2006-10-01 06:55:19 | 501009010 | 51.19 | 50 | 51.198 | 51.206 | 51.19 | 51.198 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.7157 | 47.7157 | 120.5479 | 0 | PROCESSED | 57535.7087847222 | 2016-05-27 17:00:39 | 54735 | 2008-09-26 00:00:00 | 54020.9371064815 | 2006-10-12 22:29:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | 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 | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501009010/ | Quick Look | ![]() |
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568 | G344.7-0.1 | 255.9588 | -41.7032 | 255.078113 | -41.633558 | 258.959028 | -18.797881 | 344.67682908 | -0.15577285 | 89.2821 | 54152.1890393518 | 2007-02-21 04:32:13 | 54153.2919097222 | 2007-02-22 07:00:21 | 501011010 | 42.1336 | 40 | 42.1336 | 42.1336 | 0 | 42.1336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.2016 | 34.2016 | 95.28 | 1 | PROCESSED | 57537.4329050926 | 2016-05-29 10:23:23 | 54777 | 2008-11-07 00:00:00 | 54158.2352662037 | 2007-02-27 05:38:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 1 | AO1 | SUZAKU OBSERVATION OF G344.7-0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501011010/ | Quick Look | ![]() |
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569 | CYGNUS_LOOP_P13 | 313.4901 | 31.0708 | 312.971102 | 30.880128 | 328.238327 | 46.115492 | 74.70349314 | -8.80441033 | 68.2467 | 53865.1416666667 | 2006-05-10 03:24:00 | 53865.5321643518 | 2006-05-10 12:46:19 | 501030010 | 17.073 | 17 | 17.073 | 17.081 | 17.089 | 17.089 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14.269 | 14.269 | 33.7279 | 0 | PROCESSED | 57534.2605092593 | 2016-05-26 06:15:08 | 54394 | 2007-10-21 00:00:00 | 53914.0847569444 | 2006-06-28 02:02:03 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501030010/ | Quick Look | ![]() |
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570 | Sgr_A_East | 266.5146 | -28.9267 | 265.720381 | -28.907844 | 266.926105 | -5.522764 | 0.05802898 | -0.07696746 | 264.7152 | 53636.3044560185 | 2005-09-23 07:18:25 | 53637.462025463 | 2005-09-24 11:05:19 | 100027010 | 44.785 | 50 | 44.801 | 44.8523 | 44.785 | 44.8283 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.8543 | 37.8543 | 100.0139 | 1 | PROCESSED | 57527.4188657407 | 2016-05-19 10:03:10 | 54247 | 2007-05-27 00:00:00 | 54035.502662037 | 2006-10-27 12:03:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027010/ | Quick Look | ![]() |
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571 | PERSEUS W1_2 | 49.5978 | 41.5445 | 48.771099 | 41.36257 | 58.342724 | 22.443076 | 150.3304489 | -13.378921 | 258.3807 | 56328.3362615741 | 2013-02-05 08:04:13 | 56329.0106018518 | 2013-02-06 00:15:16 | 807022010 | 28.9492 | 25 | 28.9492 | 28.9732 | 0 | 28.9492 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.2751 | 26.2751 | 58.2559 | 0 | PROCESSED | 57610.5207523148 | 2016-08-10 12:29:53 | 56715 | 2014-02-27 00:00:00 | 56349.5185648148 | 2013-02-26 12:26:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807022010/ | Quick Look | ![]() |
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572 | CAS A | 351.0231 | 59.0265 | 350.456601 | 58.751794 | 27.744986 | 54.948342 | 111.88943817 | -1.95981315 | 208.1115 | 54876.0965740741 | 2009-02-14 02:19:04 | 54876.8363310185 | 2009-02-14 20:04:19 | 503080010 | 30.0355 | 30 | 30.0355 | 30.0355 | 0 | 30.0355 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0731 | 30.0731 | 63.9139 | 0 | PROCESSED | 57545.551087963 | 2016-06-06 13:13:34 | 55330 | 2010-05-14 00:00:00 | 54892.9889699074 | 2009-03-02 23:44:07 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI AONO | JAP | 3 | AO3 | INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503080010/ | Quick Look | ![]() |
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573 | 3C 326 | 238.0402 | 20.0989 | 237.485976 | 20.247377 | 230.081092 | 39.212111 | 33.27596058 | 48.22956027 | 119.5805 | 54484.6775 | 2008-01-19 16:15:36 | 54486.215462963 | 2008-01-21 05:10:16 | 702006010 | 61.7381 | 60 | 61.7381 | 61.7381 | 0 | 61.7381 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.4126 | 53.4126 | 132.8598 | 1 | PROCESSED | 57541.3565162037 | 2016-06-02 08:33:23 | 54888 | 2009-02-26 00:00:00 | 54515.0338078704 | 2008-02-19 00:48:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF LOBES OF GIANT RADIO GALAXIES, 3C 326 AND 3C 35 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702006010/ | Quick Look | ![]() |
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574 | Crab Nebula | 83.6442 | 22.0129 | 82.891939 | 21.980268 | 84.10941 | -1.298101 | 184.56435264 | -5.77651077 | 84.9978 | 53614.830775463 | 2005-09-01 19:56:19 | 53614.9098263889 | 2005-09-01 21:50:09 | 100015040 | 2.9786 | 5 | 2.9786 | 2.9786 | 2.9786 | 2.9786 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.0493 | 3.0493 | 6.8079 | 0 | PROCESSED | 57527.2502430556 | 2016-05-19 06:00:21 | 54247 | 2007-05-27 00:00:00 | 54109.1815625 | 2007-01-09 04:21:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD boresight check with Crab | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015040/ | Quick Look | ![]() |
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575 | HESS J1745-303 1 | 266.2249 | -30.1096 | 265.423171 | -30.089321 | 266.702778 | -6.71164 | 358.91712668 | -0.478438 | 70.5005 | 54527.7555555556 | 2008-03-02 18:08:00 | 54529.7363310185 | 2008-03-04 17:40:19 | 502016010 | 70.5291 | 67 | 70.5371 | 70.5291 | 0 | 70.5451 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.7932 | 61.7932 | 171.0959 | 3 | PROCESSED | 57541.8000810185 | 2016-06-02 19:12:07 | 54908 | 2009-03-18 00:00:00 | 54539.3190509259 | 2008-03-14 07:39:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502016010/ | Quick Look | ![]() |
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576 | ANTICENTER | 113.3357 | -19.5305 | 112.785719 | -19.421448 | 119.46206 | -40.613154 | 234.9976882 | 0.00424804 | 280.7829 | 54212.8606481482 | 2007-04-22 20:39:20 | 54215.4197222222 | 2007-04-25 10:04:24 | 502021010 | 89.5429 | 80 | 89.5509 | 89.5589 | 0 | 89.5429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.9887 | 78.9887 | 221.0508 | 3 | PROCESSED | 57538.5236689815 | 2016-05-30 12:34:05 | 54744 | 2008-10-05 00:00:00 | 54223.2040046296 | 2007-05-03 04:53:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KENSUKE MASUI | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502021010/ | Quick Look | ![]() |
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577 | VELA JR P1 | 131.9787 | -45.8064 | 131.551046 | -45.620931 | 157.807694 | -59.76004 | 265.40235777 | -1.43438498 | 347.0031 | 54285.3151273148 | 2007-07-04 07:33:47 | 54285.6904398148 | 2007-07-04 16:34:14 | 502023010 | 10.6496 | 10 | 10.6496 | 10.6576 | 0 | 10.6576 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.0446 | 9.0446 | 32.4199 | 0 | PROCESSED | 57539.086412037 | 2016-05-31 02:04:26 | 54696 | 2008-08-18 00:00:00 | 54328.4268402778 | 2007-08-16 10:14:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502023010/ | Quick Look | ![]() |
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578 | 1A1742-294(GC_BGD_1) | 266.5264 | -29.516 | 265.728429 | -29.497192 | 266.950822 | -6.111628 | 359.56008755 | -0.392308 | 264.8664 | 53637.463287037 | 2005-09-24 11:07:08 | 53637.527962963 | 2005-09-24 12:40:16 | 100027030 | 2.0663 | 5 | 2.0663 | 2.0663 | 2.0663 | 2.0663 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.8877 | 1.8877 | 5.584 | 0 | PROCESSED | 57527.4000462963 | 2016-05-19 09:36:04 | 54247 | 2007-05-27 00:00:00 | 54035.4639583333 | 2006-10-27 11:08:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027030/ | Quick Look | ![]() |
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579 | SAGITTARIUS A* | 266.415 | -29.0052 | 265.620304 | -28.98586 | 266.840523 | -5.603385 | 359.94564014 | -0.04343346 | 106.9998 | 56738.4724189815 | 2014-03-22 11:20:17 | 56738.9897685185 | 2014-03-22 23:45:16 | 408017070 | 21.5887 | 20 | 21.6185 | 21.5887 | 0 | 21.6442 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.274 | 19.274 | 44.694 | 0 | PROCESSED | 57614.0833680556 | 2016-08-14 02:00:03 | 57120 | 2015-04-08 00:00:00 | 56750.8212268518 | 2014-04-03 19:42:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017070/ | Quick Look | ![]() |
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580 | 1RXSJ170047.8-314442 | 255.196 | -31.7452 | 254.389249 | -31.672155 | 257.283531 | -8.954733 | 352.21229356 | 6.40020757 | 90.7944 | 56341.4932060185 | 2013-02-18 11:50:13 | 56341.7501273148 | 2013-02-18 18:00:11 | 407027010 | 8.9262 | 12 | 8.9262 | 8.9262 | 0 | 8.9262 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.232 | 8.232 | 22.186 | 0 | PROCESSED | 57610.6225810185 | 2016-08-10 14:56:31 | 56718 | 2014-03-02 00:00:00 | 56352.4986458333 | 2013-03-01 11:58:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEYUKI MORI | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407027010/ | Quick Look | ![]() |
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581 | PBC J0839.7-1214 | 129.9392 | -12.3029 | 129.345024 | -12.125278 | 136.15221 | -29.568931 | 237.21342575 | 17.37856511 | 291.8979 | 55324.6892824074 | 2010-05-08 16:32:34 | 55326.4896990741 | 2010-05-10 11:45:10 | 705007010 | 80.5643 | 80 | 80.5643 | 80.5643 | 0 | 80.5643 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.7418 | 70.7418 | 155.5358 | 1 | PROCESSED | 57551.4721759259 | 2016-06-12 11:19:56 | 55707 | 2011-05-26 00:00:00 | 55341.5690856482 | 2010-05-25 13:39:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 5 | AO5 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705007010/ | Quick Look | ![]() |
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582 | VELA JR P8 | 133.862 | -45.8612 | 133.428362 | -45.669016 | 160.04869 | -59.10729 | 266.28131071 | -0.45847751 | 347.0005 | 54287.3028240741 | 2007-07-06 07:16:04 | 54287.7009722222 | 2007-07-06 16:49:24 | 502030010 | 13.2196 | 10 | 13.2196 | 13.2196 | 0 | 13.2196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.441 | 14.441 | 34.3919 | 0 | PROCESSED | 57539.112662037 | 2016-05-31 02:42:14 | 54703 | 2008-08-25 00:00:00 | 54333.4507175926 | 2007-08-21 10:49:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502030010/ | Quick Look | ![]() |
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583 | VELA JR P13 | 131.851 | -46.106 | 131.426011 | -45.92099 | 157.974394 | -60.061119 | 265.57984888 | -1.69160478 | 347.0011 | 54290.1290162037 | 2007-07-09 03:05:47 | 54290.4411342593 | 2007-07-09 10:35:14 | 502035010 | 9.4089 | 10 | 9.4089 | 9.4089 | 0 | 9.4089 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.9531 | 8.9531 | 26.9639 | 0 | PROCESSED | 57539.1321412037 | 2016-05-31 03:10:17 | 54696 | 2008-08-18 00:00:00 | 54328.4906134259 | 2007-08-16 11:46:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502035010/ | Quick Look | ![]() |
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584 | SN1006 | 225.7268 | -41.9424 | 224.908794 | -41.746586 | 235.456683 | -23.661429 | 327.58003425 | 14.55159393 | 117.0193 | 54521.6264351852 | 2008-02-25 15:02:04 | 54526.8613310185 | 2008-03-01 20:40:19 | 502046010 | 211.7373 | 200 | 211.7453 | 211.7373 | 0 | 211.7453 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 184.3622 | 184.3622 | 417.2759 | 6 | PROCESSED | 57541.8622337963 | 2016-06-02 20:41:37 | 54904 | 2009-03-14 00:00:00 | 54535.729375 | 2008-03-10 17:30:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYA YAMAGUCHI | JAP | 2 | AO2 | THE CENTER REGION OF SN1006 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502046010/ | Quick Look | ![]() |
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585 | HESS J1702-420 | 255.6874 | -42.0709 | 254.803902 | -41.999975 | 258.786548 | -19.184424 | 344.26217794 | -0.21974248 | 106.4451 | 54550.458599537 | 2008-03-25 11:00:23 | 54555.625162037 | 2008-03-30 15:00:14 | 502049010 | 215.6932 | 200 | 215.7053 | 215.6932 | 0 | 215.7053 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140.6375 | 140.6375 | 395.7215 | 6 | PROCESSED | 57542.1678356482 | 2016-06-03 04:01:41 | 54933 | 2009-04-12 00:00:00 | 54566.9486458333 | 2008-04-10 22:46:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 2 | AO2 | RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502049010/ | Quick Look | ![]() |
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586 | N132D | 81.4173 | -69.7177 | 81.522733 | -69.759029 | 311.341106 | -85.51708 | 280.38157857 | -32.71705874 | 53.198 | 53597.6939814815 | 2005-08-15 16:39:20 | 53597.8369328704 | 2005-08-15 20:05:11 | 100002030 | 0 | 7 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6825231482 | 2016-05-12 16:22:50 | 54247 | 2007-05-27 00:00:00 | 54230.4133449074 | 2007-05-10 09:55:13 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD HV ON WITH N132D | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002030/ | Quick Look | ![]() |
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587 | HESS J1731-347 SW | 263.0074 | -34.9458 | 262.173825 | -34.909887 | 264.142527 | -11.646447 | 353.3803333 | -0.77058494 | 92.6086 | 55245.72 | 2010-02-18 17:16:48 | 55246.5231365741 | 2010-02-19 12:33:19 | 504031010 | 41.8615 | 40 | 41.8779 | 41.8615 | 0 | 41.8695 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.1028 | 34.1028 | 69.382 | 0 | PROCESSED | 57550.6419675926 | 2016-06-11 15:24:26 | 55623 | 2011-03-03 00:00:00 | 55257.0493981482 | 2010-03-02 01:11:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504031010/ | Quick Look | ![]() |
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588 | TORNADO | 265.1272 | -30.949 | 264.32027 | -30.923391 | 265.775878 | -7.579198 | 357.70572925 | -0.11631727 | 269.1137 | 55072.5037037037 | 2009-08-29 12:05:20 | 55075.0093055556 | 2009-09-01 00:13:24 | 504036010 | 125.0692 | 120 | 125.0692 | 125.0772 | 0 | 125.0772 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.0913 | 97.0913 | 216.4598 | 3 | PROCESSED | 57548.5178356482 | 2016-06-09 12:25:41 | 55454 | 2010-09-15 00:00:00 | 55088.3064814815 | 2009-09-14 07:21:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKESHI TSURU | JAP | 4 | AO4 | REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504036010/ | Quick Look | ![]() |
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589 | GC_LARGEPROJECT1 | 266.4387 | -28.5683 | 265.646756 | -28.549082 | 266.850456 | -5.166114 | 0.32941305 | 0.16640393 | 260.8767 | 54711.4273958333 | 2008-09-02 10:15:27 | 54712.9530555556 | 2008-09-03 22:52:24 | 503007010 | 52.1523 | 50 | 52.1523 | 52.1523 | 0 | 52.1523 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1838 | 44.1838 | 131.7938 | 2 | PROCESSED | 57543.7627546296 | 2016-06-04 18:18:22 | 54557 | 2008-04-01 00:00:00 | 54780.6858796296 | 2008-11-10 16:27:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503007010/ | Quick Look | ![]() |
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590 | GC_LARGEPROJECT11 | 264.7183 | -31.3859 | 263.908606 | -31.358306 | 265.438625 | -8.028238 | 357.14965021 | -0.05250387 | 268.3335 | 54732.3390046296 | 2008-09-23 08:08:10 | 54733.3897337963 | 2008-09-24 09:21:13 | 503017010 | 51.2865 | 50 | 51.2945 | 51.2865 | 0 | 51.3025 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.5834 | 48.5834 | 90.7759 | 2 | PROCESSED | 57543.9868287037 | 2016-06-04 23:41:02 | 54557 | 2008-04-01 00:00:00 | 54780.6941550926 | 2008-11-10 16:39:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503017010/ | Quick Look | ![]() |
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591 | LOOP 1 L=356.00 | 263.2426 | -31.9466 | 262.429689 | -31.911872 | 264.194275 | -8.641352 | 356.00010804 | 0.70279756 | 93.3363 | 54908.96625 | 2009-03-18 23:11:24 | 54909.8933333333 | 2009-03-19 21:26:24 | 503022010 | 41.3193 | 40 | 41.3193 | 41.3193 | 0 | 41.3193 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3187 | 34.3187 | 80.0699 | 0 | PROCESSED | 57545.8730671296 | 2016-06-06 20:57:13 | 55330 | 2010-05-14 00:00:00 | 54923.2640162037 | 2009-04-02 06:20:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503022010/ | Quick Look | ![]() |
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592 | Crab nebula | 83.8083 | 22.0272 | 83.05592 | 21.995359 | 84.262061 | -1.290429 | 184.63396429 | -5.64031243 | 86.9342 | 53604.5844791667 | 2005-08-22 14:01:39 | 53604.6479861111 | 2005-08-22 15:33:06 | 100007050 | 3.262 | 5 | 3.262 | 3.262 | 3.262 | 3.262 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.179 | 3.179 | 5.448 | 0 | PROCESSED | 57520.7490509259 | 2016-05-12 17:58:38 | 54247 | 2007-05-27 00:00:00 | 54105.3334143518 | 2007-01-05 08:00:07 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Crab Nebula | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007050/ | Quick Look | ![]() |
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593 | LOOP 2 L=356.33 | 263.4562 | -31.667 | 262.645073 | -31.633306 | 264.364444 | -8.35361 | 356.33349006 | 0.70266893 | 94.2779 | 54916.2757060185 | 2009-03-26 06:37:01 | 54917.0786921296 | 2009-03-27 01:53:19 | 503023010 | 31.1527 | 40 | 31.1527 | 31.1527 | 0 | 31.1527 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.2346 | 28.2346 | 69.3699 | 0 | PROCESSED | 57545.9012615741 | 2016-06-06 21:37:49 | 55330 | 2010-05-14 00:00:00 | 54930.234849537 | 2009-04-09 05:38:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503023010/ | Quick Look | ![]() |
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594 | CYGNUS LOOP (P11) | 312.4425 | 31.5127 | 311.927752 | 31.32576 | 327.295676 | 46.874223 | 74.4826992 | -7.83027866 | 49.9999 | 54595.9014814815 | 2008-05-09 21:38:08 | 54596.7391087963 | 2008-05-10 17:44:19 | 503055010 | 31.8947 | 25 | 31.9027 | 31.8947 | 0 | 31.9107 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0738 | 25.0738 | 72.3599 | 0 | PROCESSED | 57542.4981712963 | 2016-06-03 11:57:22 | 54972 | 2009-05-21 00:00:00 | 54606.1436342593 | 2008-05-20 03:26:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503055010/ | Quick Look | ![]() |
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595 | ASO0449 | 299.6429 | 28.7759 | 299.134977 | 28.639283 | 310.497072 | 48.135601 | 65.87759933 | -0.32938525 | 56.1427 | 54974.6386921296 | 2009-05-23 15:19:43 | 54975.5786342593 | 2009-05-24 13:53:14 | 504044010 | 38.7337 | 20 | 38.7337 | 38.7417 | 0 | 38.7417 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.22 | 35.22 | 81.1999 | 2 | PROCESSED | 57546.6654050926 | 2016-06-07 15:58:11 | 55356 | 2010-06-09 00:00:00 | 54987.4424652778 | 2009-06-05 10:37:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504044010/ | Quick Look | ![]() |
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596 | ASO0447 | 298.557 | 28.6365 | 298.049709 | 28.504502 | 309.068665 | 48.278589 | 65.2636943 | 0.41202338 | 90.516 | 54928.7514699074 | 2009-04-07 18:02:07 | 54929.253587963 | 2009-04-08 06:05:10 | 504046010 | 20.5457 | 20 | 20.5457 | 20.5457 | 0 | 20.5457 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.9071 | 16.9071 | 43.3779 | 1 | PROCESSED | 57546.0447106482 | 2016-06-07 01:04:23 | 55324 | 2010-05-08 00:00:00 | 54949.4485300926 | 2009-04-28 10:45:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504046010/ | Quick Look | ![]() |
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597 | CYGNUS LOOP (P24) | 312.134 | 32.2905 | 311.623759 | 32.104666 | 327.393235 | 47.692301 | 74.93132331 | -7.14055521 | 61.3941 | 54621.1479513889 | 2008-06-04 03:33:03 | 54621.6271875 | 2008-06-04 15:03:09 | 503060010 | 18.5046 | 15 | 18.5046 | 18.5046 | 0 | 18.5046 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.999 | 14.999 | 41.3979 | 1 | PROCESSED | 57542.7234027778 | 2016-06-03 17:21:42 | 55003 | 2009-06-21 00:00:00 | 54637.4594675926 | 2008-06-20 11:01:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503060010/ | Quick Look | ![]() |
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598 | (L,B)=(0.107,-1.425) | 267.8602 | -29.5833 | 267.06157 | -29.570962 | 268.118883 | -6.156195 | 0.10035042 | -1.42140103 | 68.0986 | 55261.1636226852 | 2010-03-06 03:55:37 | 55263.893275463 | 2010-03-08 21:26:19 | 504050010 | 100.3991 | 100 | 100.4311 | 100.3991 | 0 | 100.4231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.536 | 80.536 | 235.8218 | 1 | PROCESSED | 57550.8323726852 | 2016-06-11 19:58:37 | 55645 | 2011-03-25 00:00:00 | 55278.4832523148 | 2010-03-23 11:35:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 4 | AO4 | RESOLVING ORIGIN OF THE IRON EMISSION LINES FROM THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504050010/ | Quick Look | ![]() |
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599 | GC(0,-1.6) | 268.0544 | -29.7594 | 267.254612 | -29.748002 | 268.29113 | -6.329868 | 0.03481768 | -1.65633011 | 65.7488 | 54899.6540509259 | 2009-03-09 15:41:50 | 54900.8168865741 | 2009-03-10 19:36:19 | 503081010 | 59.2233 | 50 | 59.2233 | 59.2233 | 0 | 59.2233 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.6018 | 57.6018 | 100.4538 | 1 | PROCESSED | 57545.7843402778 | 2016-06-06 18:49:27 | 55330 | 2010-05-14 00:00:00 | 54916.3813194444 | 2009-03-26 09:09:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI MURAKAMI | JAP | 3 | AO3 | NEW EVIDENCE OF THE PAST ACTIVITY IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503081010/ | Quick Look | ![]() |
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600 | HESSJ1616_PSRJ1617 | 244.3756 | -50.9175 | 243.427641 | -50.794985 | 251.811911 | -29.080089 | 332.50297445 | -0.27465368 | 270.0711 | 55059.1110763889 | 2009-08-16 02:39:57 | 55060.8328009259 | 2009-08-17 19:59:14 | 504056010 | 65.8331 | 50 | 65.8891 | 65.8331 | 0 | 65.8971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.7504 | 41.7504 | 148.7258 | 0 | PROCESSED | 57548.1892708333 | 2016-06-09 04:32:33 | 55437 | 2010-08-29 00:00:00 | 55071.2513425926 | 2009-08-28 06:01:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 4 | AO4 | IS THE MOST ENERGETIC UNIDENTIFIED TEV OBJECT HESSJ1616-508 A PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504056010/ | Quick Look | ![]() |
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601 | HESS J1745-303C | 266.3881 | -30.6242 | 265.582985 | -30.604704 | 266.857963 | -7.222423 | 358.55151469 | -0.86700864 | 101.7444 | 55252.1897800926 | 2010-02-25 04:33:17 | 55253.3842476852 | 2010-02-26 09:13:19 | 504003010 | 50.9065 | 50 | 50.9145 | 50.9145 | 0 | 50.9065 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2708 | 41.2708 | 103.1878 | 3 | PROCESSED | 57550.7231365741 | 2016-06-11 17:21:19 | 55632 | 2011-03-12 00:00:00 | 55264.3901157407 | 2010-03-09 09:21:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504003010/ | Quick Look | ![]() |
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602 | NGC 7603 | 349.73 | 0.2557 | 349.089402 | -0.017972 | 350.656446 | 4.302592 | 80.07171077 | -54.72674929 | 67.5296 | 56080.5080208333 | 2012-06-02 12:11:33 | 56082.6598726852 | 2012-06-04 15:50:13 | 707003010 | 101.2567 | 100 | 101.2602 | 101.2657 | 0 | 101.2567 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.0023 | 96.0023 | 185.9037 | 2 | PROCESSED | 57605.6196875 | 2016-08-05 14:52:21 | 56464 | 2013-06-21 00:00:00 | 56096.2688541667 | 2012-06-18 06:27:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 7 | AO7 | PURE ACCRETION DISK SPECTRUM OF THE SEYFERT 1 NGC 7603 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707003010/ | Quick Look | ![]() |
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603 | RXJ1713-3946 | 258.1633 | -39.7281 | 257.296672 | -39.668915 | 260.511599 | -16.675371 | 347.25895477 | -0.31287235 | 268.0002 | 53989.5311574074 | 2006-09-11 12:44:52 | 53989.9216898148 | 2006-09-11 22:07:14 | 501064010 | 21.322 | 20 | 21.322 | 21.322 | 21.322 | 21.322 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23.0306 | 23.0306 | 33.7279 | 0 | PROCESSED | 57535.5353356482 | 2016-05-27 12:50:53 | 54526 | 2008-03-01 00:00:00 | 54020.8109027778 | 2006-10-12 19:27:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501064010/ | Quick Look | ![]() |
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604 | SGR_B2 | 266.8776 | -28.4437 | 266.086356 | -28.426612 | 267.234654 | -5.032575 | 0.63615824 | -0.0985299 | 266.3663 | 55095.6093518518 | 2009-09-21 14:37:28 | 55096.0418287037 | 2009-09-22 01:00:14 | 504004010 | 10.0572 | 200 | 10.0572 | 10.0572 | 0 | 10.0572 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.4328 | 9.4328 | 37.3409 | 0 | PROCESSED | 57548.6152314815 | 2016-06-09 14:45:56 | 55476 | 2010-10-07 00:00:00 | 55110.2035763889 | 2009-10-06 04:53:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAYOSHI NOBUKAWA | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004010/ | Quick Look | ![]() |
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605 | RIM4 | 311.4678 | 31.0131 | 310.952491 | 30.829697 | 325.890411 | 46.737501 | 73.56601773 | -7.48621797 | 246.0303 | 55155.1210763889 | 2009-11-20 02:54:21 | 55155.3579166667 | 2009-11-20 08:35:24 | 504008010 | 12.1025 | 10 | 12.1025 | 12.1185 | 0 | 12.1105 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.666 | 8.666 | 20.4559 | 0 | PROCESSED | 57549.475462963 | 2016-06-10 11:24:40 | 55534 | 2010-12-04 00:00:00 | 55166.425787037 | 2009-12-01 10:13:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504008010/ | Quick Look | ![]() |
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606 | NEP | 272.8227 | 66.0165 | 272.806643 | 66.002812 | 335.593486 | 88.746745 | 95.79277142 | 28.663354 | 126.3033 | 53776.2556944445 | 2006-02-10 06:08:12 | 53778.0836111111 | 2006-02-12 02:00:24 | 500026010 | 88.5082 | 80 | 88.5322 | 88.5082 | 88.5242 | 88.5322 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 83.6728 | 83.6728 | 157.902 | 0 | PROCESSED | 57532.9856481482 | 2016-05-24 23:39:20 | 54247 | 2007-05-27 00:00:00 | 54041.1403703704 | 2006-11-02 03:22:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | NEP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500026010/ | Quick Look | ![]() |
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607 | PERSEUS G_2 | 50.329 | 41.3745 | 49.501378 | 41.195271 | 58.861053 | 22.128129 | 150.89645322 | -13.21839457 | 259.7649 | 56325.9651157407 | 2013-02-02 23:09:46 | 56326.3181828704 | 2013-02-03 07:38:11 | 807023010 | 14.2445 | 15 | 14.2445 | 14.2525 | 0 | 14.2525 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.5822 | 20.5822 | 30.4839 | 0 | PROCESSED | 57610.4949074074 | 2016-08-10 11:52:40 | 56711 | 2014-02-23 00:00:00 | 56345.4909953704 | 2013-02-22 11:47:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807023010/ | Quick Look | ![]() |
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608 | BLOWOUT6 | 311.7638 | 30.9468 | 311.247593 | 30.762319 | 326.194522 | 46.578638 | 73.67127235 | -7.72686898 | 241.7587 | 55165.8330787037 | 2009-11-30 19:59:38 | 55166.2883449074 | 2009-12-01 06:55:13 | 504016010 | 21 | 19 | 21.008 | 21.016 | 0 | 21 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.7129 | 17.7129 | 39.3279 | 0 | PROCESSED | 57549.644849537 | 2016-06-10 15:28:35 | 55547 | 2010-12-17 00:00:00 | 55181.2630324074 | 2009-12-16 06:18:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504016010/ | Quick Look | ![]() |
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609 | HESS J1427-608 | 216.9609 | -60.8505 | 216.024633 | -60.626609 | 237.709544 | -43.214788 | 314.40487303 | -0.14444396 | 90.5578 | 55209.5761458333 | 2010-01-13 13:49:39 | 55212.1891666667 | 2010-01-16 04:32:24 | 504034010 | 104.1379 | 100 | 104.1379 | 104.1379 | 0 | 104.1379 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.2611 | 71.2611 | 225.7378 | 1 | PROCESSED | 57550.2389930556 | 2016-06-11 05:44:09 | 55594 | 2011-02-02 00:00:00 | 55225.4958449074 | 2010-01-29 11:54:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 4 | AO4 | A SUZAKU OBSERVATION OF HESS J1427-608 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504034010/ | Quick Look | ![]() |
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610 | ASO0402 | 273.3436 | -12.7608 | 272.639832 | -12.775336 | 273.308329 | 10.641449 | 17.24676471 | 2.45193699 | 68.9842 | 55277.3929513889 | 2010-03-22 09:25:51 | 55277.9793287037 | 2010-03-22 23:30:14 | 504042010 | 25.7125 | 20 | 25.7125 | 25.7125 | 0 | 25.7125 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.0152 | 16.0152 | 50.6559 | 1 | PROCESSED | 57550.9498958333 | 2016-06-11 22:47:51 | 55784 | 2011-08-11 00:00:00 | 55417.0893865741 | 2010-08-09 02:08:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504042010/ | Quick Look | ![]() |
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611 | VICINITY OF NGC 4051 | 180.4686 | 44.1146 | 179.828661 | 44.392934 | 159.283243 | 39.862026 | 150.13143213 | 70.30340869 | 109.3717 | 55184.3459606482 | 2009-12-19 08:18:11 | 55186.5140509259 | 2009-12-21 12:20:14 | 504062010 | 89.6305 | 80 | 89.6385 | 89.6465 | 0 | 89.6305 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 37.0758 | 37.0758 | 187.2819 | 2 | PROCESSED | 57549.977337963 | 2016-06-10 23:27:22 | 55581 | 2011-01-20 00:00:00 | 55209.4570833333 | 2010-01-13 10:58:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHISHIGE HAGIHARA | JAP | 4 | AO4 | STUDY OF WARM-HOT GAS TOWARD NGC 4051 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504062010/ | Quick Look | ![]() |
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612 | W51NW | 290.6858 | 14.2133 | 290.110894 | 14.116258 | 294.988251 | 35.876885 | 49.11550833 | -0.31636783 | 105.4558 | 55283.4893634259 | 2010-03-28 11:44:41 | 55284.555 | 2010-03-29 13:19:12 | 504066010 | 44.1125 | 40 | 44.1205 | 44.1205 | 0 | 44.1125 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.8961 | 8.8961 | 92.0639 | 0 | PROCESSED | 57551.0258217593 | 2016-06-12 00:37:11 | 55671 | 2011-04-20 00:00:00 | 55302.5003240741 | 2010-04-16 12:00:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEAKI KATAGIRI | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504066010/ | Quick Look | ![]() |
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613 | CYGNUS_LOOP_P2 | 313.2729 | 31.7708 | 312.75774 | 31.580892 | 328.394465 | 46.831624 | 75.13379207 | -8.21853117 | 240.0005 | 54418.0909722222 | 2007-11-14 02:11:00 | 54418.4168865741 | 2007-11-14 10:00:19 | 501013010 | 16.3799 | 10 | 16.3879 | 16.3879 | 0 | 16.3799 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.9786 | 10.9786 | 28.1519 | 0 | PROCESSED | 57540.5114351852 | 2016-06-01 12:16:28 | 54798 | 2008-11-28 00:00:00 | 54430.1915972222 | 2007-11-26 04:35:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501013010/ | Quick Look | ![]() |
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614 | CYGNUS_LOOP_P14 | 313.2365 | 30.8681 | 312.717032 | 30.678328 | 327.835222 | 46.014729 | 74.40554659 | -8.76356285 | 62.362 | 53867.6311111111 | 2006-05-12 15:08:48 | 53868.0050462963 | 2006-05-13 00:07:16 | 501031010 | 18.5809 | 18 | 18.5809 | 18.5809 | 18.5809 | 18.5809 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12.7378 | 12.7378 | 32.2979 | 0 | PROCESSED | 57534.275775463 | 2016-05-26 06:37:07 | 54394 | 2007-10-21 00:00:00 | 53914.3142476852 | 2006-06-28 07:32:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501031010/ | Quick Look | ![]() |
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615 | PKS1127-145 | 172.5274 | -14.8245 | 171.896651 | -14.548647 | 179.186436 | -16.542663 | 275.2785401 | 43.63731171 | 115.9184 | 54799.7571180556 | 2008-11-29 18:10:15 | 54800.9523611111 | 2008-11-30 22:51:24 | 703004010 | 55.5451 | 40 | 55.5511 | 55.5451 | 0 | 55.5511 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.0123 | 31.0123 | 103.2488 | 0 | PROCESSED | 57544.5555208333 | 2016-06-05 13:19:57 | 54557 | 2008-04-01 00:00:00 | 54809.1987152778 | 2008-12-09 04:46:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703004010/ | Quick Look | ![]() |
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616 | IC443 NORTHWEST | 93.9975 | 22.7552 | 93.240341 | 22.772771 | 93.68801 | -0.634546 | 188.75644855 | 2.86235674 | 91.4819 | 55456.3191435185 | 2010-09-17 07:39:34 | 55458.2829050926 | 2010-09-19 06:47:23 | 505001010 | 83.1917 | 80 | 83.1917 | 83.1917 | 0 | 83.1917 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.6786 | 69.6786 | 169.6457 | 2 | PROCESSED | 57553.4791087963 | 2016-06-14 11:29:55 | 55836 | 2011-10-02 00:00:00 | 55469.4041087963 | 2010-09-30 09:41:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MIDORI OZAWA | JAP | 5 | AO5 | EXPLORING THE ORIGIN OF THE RADIATIVE RECOMBINATION CONTINUUM OF IC443 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505001010/ | Quick Look | ![]() |
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617 | CYGNUS_LOOP_P18 | 312.0547 | 29.7111 | 311.531939 | 29.525574 | 325.8489 | 45.340722 | 72.84665082 | -8.68804998 | 237.4994 | 54087.0528819444 | 2006-12-18 01:16:09 | 54087.3405208333 | 2006-12-18 08:10:21 | 501035010 | 12.011 | 13 | 12.915 | 12.011 | 0 | 12.907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.4394 | 11.4394 | 24.8359 | 3 | PROCESSED | 57536.3543981482 | 2016-05-28 08:30:20 | 54750 | 2008-10-11 00:00:00 | 54096.4390972222 | 2006-12-27 10:32:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501035010/ | Quick Look | ![]() |
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618 | CYGNUS LOOP 7 | 313.929 | 31.0152 | 313.408854 | 30.822982 | 328.70395 | 45.915608 | 74.90122685 | -9.13052292 | 81.814 | 55306.459212963 | 2010-04-20 11:01:16 | 55306.7974189815 | 2010-04-20 19:08:17 | 505015010 | 13.5918 | 12 | 13.5918 | 13.5998 | 0 | 13.5998 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.682 | 12.682 | 29.1959 | 0 | PROCESSED | 57551.269212963 | 2016-06-12 06:27:40 | 55287 | 2010-04-01 00:00:00 | 55393.2216203704 | 2010-07-16 05:19:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505015010/ | Quick Look | ![]() |
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619 | CYGNUS LOOP 14 | 313.0411 | 29.9656 | 312.517703 | 29.77653 | 327.111212 | 45.248773 | 73.58742167 | -9.19932348 | 67.2195 | 55334.4727893518 | 2010-05-18 11:20:49 | 55335.1146759259 | 2010-05-19 02:45:08 | 505022010 | 29.2512 | 29 | 29.2512 | 29.2512 | 0 | 29.2512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.7832 | 24.7832 | 55.4519 | 0 | PROCESSED | 57551.5599305556 | 2016-06-12 13:26:18 | 55287 | 2010-04-01 00:00:00 | 55348.0488888889 | 2010-06-01 01:10:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505022010/ | Quick Look | ![]() |
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620 | FVW319.8+0.3 | 225.913 | -58.2332 | 224.953134 | -58.037768 | 241.861071 | -39.018553 | 319.61922846 | 0.28881447 | 278.3756 | 55413.1563888889 | 2010-08-05 03:45:12 | 55413.9307291667 | 2010-08-05 22:20:15 | 505029010 | 51.384 | 50 | 51.4 | 51.384 | 0 | 51.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.416 | 45.416 | 66.8939 | 2 | PROCESSED | 57552.8424421296 | 2016-06-13 20:13:07 | 55793 | 2011-08-20 00:00:00 | 55427.1529976852 | 2010-08-19 03:40:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 5 | AO5 | SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505029010/ | Quick Look | ![]() |
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621 | HESS J1825-137 BG | 276.9022 | -13.2649 | 276.196149 | -13.29666 | 276.811822 | 10.012623 | 18.4366217 | -0.84356166 | 269.33 | 54027.1689351852 | 2006-10-19 04:03:16 | 54028.5072337963 | 2006-10-20 12:10:25 | 501045010 | 52.1444 | 50 | 52.1524 | 52.1444 | 52.1524 | 52.1444 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.1974 | 42.1974 | 115.6079 | 2 | PROCESSED | 57535.8869907407 | 2016-05-27 21:17:16 | 54526 | 2008-03-01 00:00:00 | 54055.6591550926 | 2006-11-16 15:49:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501045010/ | Quick Look | ![]() |
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622 | L139_B-32 | 28.093 | 28.6837 | 27.38183 | 28.437322 | 36.368533 | 16.024453 | 138.75887563 | -32.3084393 | 253.9538 | 55569.4091319444 | 2011-01-08 09:49:09 | 55571.3188541667 | 2011-01-10 07:39:09 | 505044010 | 84.0041 | 80 | 84.0041 | 84.0041 | 0 | 84.0041 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.0377 | 79.0377 | 164.9839 | 0 | PROCESSED | 57600.6057175926 | 2016-07-31 14:32:14 | 55962 | 2012-02-05 00:00:00 | 55595.2037615741 | 2011-02-03 04:53:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NORIKO YAMASAKI | JAP | 5 | AO5 | STRUCTURE OF THE GALACTIC HALO EMISSION TOWARD THE ANTI-CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505044010/ | Quick Look | ![]() |
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623 | HB21 SOUTH | 311.2512 | 50.6016 | 310.86516 | 50.418766 | 342.682858 | 64.005982 | 88.85305014 | 4.80482025 | 105.492 | 55660.3542361111 | 2011-04-09 08:30:06 | 55662.8155208333 | 2011-04-11 19:34:21 | 506005010 | 132.363 | 150 | 132.371 | 132.371 | 0 | 132.363 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 141.7887 | 141.7887 | 212.6359 | 1 | PROCESSED | 57601.4958564815 | 2016-08-01 11:54:02 | 56159 | 2012-08-20 00:00:00 | 55677.2811342593 | 2011-04-26 06:44:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 6 | AO6 | ORIGIN OF OVER-IONIZATION OF SNR PLASMAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506005010/ | Quick Look | ![]() |
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624 | CYGNUS LOOP BLOWOUT2 | 312.4423 | 29.4154 | 311.917417 | 29.228478 | 326.132278 | 44.939266 | 72.82314938 | -9.13589092 | 78.1524 | 55687.8500578704 | 2011-05-06 20:24:05 | 55688.6488310185 | 2011-05-07 15:34:19 | 506012010 | 35.655 | 35 | 35.655 | 35.655 | 0 | 35.655 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.4815 | 31.4815 | 68.9821 | 0 | PROCESSED | 57601.9748263889 | 2016-08-01 23:23:45 | 56066 | 2012-05-19 00:00:00 | 55700.4593865741 | 2011-05-19 11:01:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506012010/ | Quick Look | ![]() |
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625 | CYGNUS LOOP BLOWOUT6 | 312.8964 | 28.9665 | 312.36858 | 28.777954 | 326.408889 | 44.373591 | 72.71699713 | -9.72555156 | 78.1534 | 55691.9894791667 | 2011-05-10 23:44:51 | 55692.7710069445 | 2011-05-11 18:30:15 | 506016010 | 36.3744 | 35 | 36.3744 | 36.3744 | 0 | 36.3744 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.7568 | 32.7568 | 67.5039 | 0 | PROCESSED | 57602.0240277778 | 2016-08-02 00:34:36 | 56068 | 2012-05-21 00:00:00 | 55701.1981828704 | 2011-05-20 04:45:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506016010/ | Quick Look | ![]() |
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626 | GC23 | 266.578 | -28.0524 | 265.789256 | -28.033865 | 266.960919 | -4.647397 | 0.83380185 | 0.3300796 | 262.2345 | 54386.7855208333 | 2007-10-13 18:51:09 | 54387.2294444444 | 2007-10-14 05:30:24 | 502011010 | 23.013 | 20 | 23.013 | 23.021 | 0 | 23.029 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.0712 | 22.0712 | 38.3199 | 2 | PROCESSED | 57540.2674305556 | 2016-06-01 06:25:06 | 54777 | 2008-11-07 00:00:00 | 54402.5316898148 | 2007-10-29 12:45:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502011010/ | Quick Look | ![]() |
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627 | G23.5+0.1 | 278.489 | -8.375 | 277.807565 | -8.414468 | 278.678732 | 14.810155 | 23.49243074 | 0.03918587 | 261.7121 | 55489.5657291667 | 2010-10-20 13:34:39 | 55491.0730439815 | 2010-10-22 01:45:11 | 505026010 | 48.9761 | 50 | 48.9761 | 48.9761 | 0 | 48.9761 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7884 | 43.7884 | 130.1919 | 0 | PROCESSED | 57553.8193981482 | 2016-06-14 19:39:56 | 55868 | 2011-11-03 00:00:00 | 55502.1887962963 | 2010-11-02 04:31:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505026010/ | Quick Look | ![]() |
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628 | 3C 59 VICINITY 2 | 31.4351 | 28.9234 | 30.715452 | 28.684984 | 39.296603 | 15.198203 | 141.95387958 | -31.18906496 | 250.3 | 55952.5116435185 | 2012-01-26 12:16:46 | 55957.4238773148 | 2012-01-31 10:10:23 | 506025010 | 173.347 | 50 | 173.347 | 173.355 | 0 | 173.355 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 0.5479 | 0.5479 | 86.854 | 0 | PROCESSED | 57604.5146759259 | 2016-08-04 12:21:08 | 56526 | 2013-08-22 00:00:00 | 56167.6426388889 | 2012-08-28 15:25:24 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUHIRO SAKAI | JAP | 6 | AO6 | STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506025010/ | Quick Look | ![]() |
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629 | RADIO_ARC_S_W | 266.7778 | -29.3674 | 265.980729 | -29.349813 | 267.167421 | -5.95796 | 359.8007683 | -0.50226251 | 267.1999 | 56200.9358101852 | 2012-09-30 22:27:34 | 56202.0120601852 | 2012-10-02 00:17:22 | 507018010 | 51.0807 | 50 | 51.1047 | 51.0967 | 0 | 51.0807 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49.115 | 49.115 | 92.9799 | 0 | PROCESSED | 57607.2580324074 | 2016-08-07 06:11:34 | 56592 | 2013-10-27 00:00:00 | 56226.6169675926 | 2012-10-26 14:48:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SYUKYO RYU | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507018010/ | Quick Look | ![]() |
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630 | FERMI_BUBBLE_N5 | 233.6225 | 8.0718 | 233.013762 | 8.238094 | 228.991173 | 26.481108 | 14.37791019 | 47.00724717 | 287.4992 | 56146.9871990741 | 2012-08-07 23:41:34 | 56147.4320949074 | 2012-08-08 10:22:13 | 507005010 | 21.7222 | 20 | 21.7222 | 21.7222 | 0 | 21.7222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.5559 | 19.5559 | 38.4299 | 1 | PROCESSED | 57606.7961921296 | 2016-08-06 19:06:31 | 56535 | 2013-08-31 00:00:00 | 56169.0806944444 | 2012-08-30 01:56:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507005010/ | Quick Look | ![]() |
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631 | FERMI_BUBBLE_S3 | 327.8758 | -46.7423 | 327.0753 | -46.977097 | 312.913491 | -31.549758 | 351.52788223 | -49.77060768 | 44.0052 | 56035.6752777778 | 2012-04-18 16:12:24 | 56036.133587963 | 2012-04-19 03:12:22 | 507011010 | 21.2336 | 20 | 21.2336 | 21.2336 | 0 | 21.2336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.914 | 20.914 | 39.596 | 0 | PROCESSED | 57605.205787037 | 2016-08-05 04:56:20 | 56420 | 2013-05-08 00:00:00 | 56049.1986458333 | 2012-05-02 04:46:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507011010/ | Quick Look | ![]() |
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632 | VELA JR P3 | 132.1192 | -45.6039 | 131.689583 | -45.417926 | 157.761308 | -59.536255 | 265.30669647 | -1.23070071 | 347.0044 | 54285.9040162037 | 2007-07-04 21:41:47 | 54286.1057175926 | 2007-07-05 02:32:14 | 502025010 | 10.298 | 10 | 10.298 | 10.298 | 0 | 10.298 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.726 | 6.726 | 17.4239 | 0 | PROCESSED | 57539.0955902778 | 2016-05-31 02:17:39 | 54696 | 2008-08-18 00:00:00 | 54328.4516782407 | 2007-08-16 10:50:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502025010/ | Quick Look | ![]() |
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633 | IC 443 | 94.3024 | 22.7479 | 93.545319 | 22.766949 | 93.9693 | -0.633748 | 188.89613959 | 3.10659531 | 258.9994 | 56388.2234837963 | 2013-04-06 05:21:49 | 56390.0835763889 | 2013-04-08 02:00:21 | 507015040 | 75.6427 | 300 | 75.6428 | 75.6427 | 0 | 75.6427 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 68.7284 | 68.7284 | 160.6759 | 1 | PROCESSED | 57611.01125 | 2016-08-11 00:16:12 | 56018 | 2012-04-01 00:00:00 | 56401.615775463 | 2013-04-19 14:46:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015040/ | Quick Look | ![]() |
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634 | VELA JR P11 | 132.5986 | -45.8258 | 132.169014 | -45.638098 | 158.553222 | -59.54754 | 265.69032827 | -1.11165473 | 347.0024 | 54288.2314236111 | 2007-07-07 05:33:15 | 54288.6112731482 | 2007-07-07 14:40:14 | 502033010 | 11.2833 | 10 | 11.2833 | 11.2833 | 0 | 11.2833 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2079 | 12.2079 | 32.7901 | 1 | PROCESSED | 57539.1206828704 | 2016-05-31 02:53:47 | 54696 | 2008-08-18 00:00:00 | 54328.4031944445 | 2007-08-16 09:40:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502033010/ | Quick Look | ![]() |
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635 | VELA JR P22 | 132.4428 | -46.6127 | 132.019624 | -46.425546 | 159.213685 | -60.269437 | 266.23093455 | -1.69368029 | 346.9992 | 54652.0565625 | 2008-07-05 01:21:27 | 54652.3891087963 | 2008-07-05 09:20:19 | 503034010 | 15.2643 | 10 | 15.2643 | 15.2709 | 0 | 15.2709 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9717 | 14.9717 | 28.728 | 0 | PROCESSED | 57542.966099537 | 2016-06-03 23:11:11 | 55036 | 2009-07-24 00:00:00 | 54670.1353125 | 2008-07-23 03:14:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503034010/ | Quick Look | ![]() |
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636 | HESSJ1507-622_OFFSET | 227.1815 | -62.1646 | 226.158724 | -61.973493 | 244.511164 | -42.456937 | 318.2247639 | -3.44071412 | 303.001 | 56183.9562268518 | 2012-09-13 22:56:58 | 56185.1042939815 | 2012-09-15 02:30:11 | 507026010 | 40.9122 | 40 | 40.9122 | 40.9418 | 0 | 40.9338 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.0336 | 38.0336 | 99.1798 | 1 | PROCESSED | 57607.0490162037 | 2016-08-07 01:10:35 | 56582 | 2013-10-17 00:00:00 | 56212.7288078704 | 2012-10-12 17:29:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | HIRONORI MATSUMOTO | JAP | 7 | AO7 | SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507026010/ | Quick Look | ![]() |
637 | VELA JR P18 | 133.5064 | -46.0415 | 133.075299 | -45.850566 | 159.830487 | -59.392209 | 266.25968404 | -0.76370949 | 347.0006 | 54291.9244444444 | 2007-07-10 22:11:12 | 54292.1668634259 | 2007-07-11 04:00:17 | 502040010 | 15.0123 | 10 | 15.0123 | 15.0362 | 0 | 15.0203 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.8952 | 12.8952 | 20.9439 | 1 | PROCESSED | 57539.1482407407 | 2016-05-31 03:33:28 | 54696 | 2008-08-18 00:00:00 | 54328.4716666667 | 2007-08-16 11:19:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502040010/ | Quick Look | ![]() |
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638 | LOW_LATITUDE_86-21 | 332.3169 | 30.2173 | 331.751825 | 29.971433 | 347.602182 | 38.425077 | 86.0039952 | -20.78963339 | 82.7457 | 54229.0809259259 | 2007-05-09 01:56:32 | 54230.9966898148 | 2007-05-10 23:55:14 | 502047010 | 81.5486 | 80 | 81.5486 | 81.5486 | 0 | 81.5486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.2931 | 72.2931 | 165.5099 | 2 | PROCESSED | 57538.6557986111 | 2016-05-30 15:44:21 | 54744 | 2008-10-05 00:00:00 | 54244.7948032407 | 2007-05-24 19:04:31 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOMOTAKA YOSHINO | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502047010/ | Quick Look | ![]() |
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639 | HESS J1457-593 | 224.4524 | -59.4762 | 223.48511 | -59.275761 | 241.535779 | -40.451289 | 318.36335314 | -0.44487967 | 305.8997 | 56185.1060185185 | 2012-09-15 02:32:40 | 56186.0216782407 | 2012-09-16 00:31:13 | 507027010 | 31.0479 | 30 | 31.0479 | 31.0479 | 0 | 31.0479 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.0994 | 28.0994 | 79.1059 | 1 | PROCESSED | 57607.0753819445 | 2016-08-07 01:48:33 | 56584 | 2013-10-19 00:00:00 | 56218.5178009259 | 2012-10-18 12:25:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROKAZU ODAKA | JAP | 7 | AO7 | INVESTIGATING A PUTATIVE COSMIC-RAY PEVATRON WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507027010/ | Quick Look | ![]() |
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640 | G298.6-0.0 | 183.3899 | -62.6356 | 182.720759 | -62.35751 | 219.490154 | -53.509251 | 298.59488766 | -0.08324812 | 319.8129 | 56150.8519097222 | 2012-08-11 20:26:45 | 56152.08625 | 2012-08-13 02:04:12 | 507037010 | 17.2388 | 50 | 17.2388 | 17.2388 | 0 | 17.2388 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.1746 | 19.1746 | 106.616 | 0 | PROCESSED | 57606.8422222222 | 2016-08-06 20:12:48 | 56721 | 2014-03-05 00:00:00 | 56291.7215162037 | 2012-12-30 17:18:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037010/ | Quick Look | ![]() |
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641 | CYG_COCOON | 306.8026 | 40.9389 | 306.35518 | 40.773009 | 326.953221 | 57.33325 | 79.25133167 | 1.48664873 | 218.8996 | 56279.1800231482 | 2012-12-18 04:19:14 | 56280.1654976852 | 2012-12-19 03:58:19 | 507040010 | 51.0724 | 50 | 51.0724 | 51.0936 | 0 | 51.0804 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7833 | 42.7833 | 85.1439 | 0 | PROCESSED | 57608.3232291667 | 2016-08-08 07:45:27 | 56683 | 2014-01-26 00:00:00 | 56316.5705324074 | 2013-01-24 13:41:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TSUNEFUMI MIZUNO | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507040010/ | Quick Look | ![]() |
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642 | NGC 4945 | 196.3712 | -49.4666 | 195.641165 | -49.198921 | 217.023772 | -38.637449 | 305.27663793 | 13.34118784 | 313.9062 | 53604.7788310185 | 2005-08-22 18:41:31 | 53605.1010763889 | 2005-08-23 02:25:33 | 100008010 | 14.338 | 15 | 14.338 | 14.338 | 14.338 | 14.338 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 13.8067 | 13.8067 | 27.8419 | 1 | PROCESSED | 57526.8553819444 | 2016-05-18 20:31:45 | 54247 | 2007-05-27 00:00:00 | 54035.5212152778 | 2006-10-27 12:30:33 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000008 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | NGC 4945 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100008010/ | Quick Look | ![]() |
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643 | W44_NORTH | 283.9599 | 1.4928 | 283.326032 | 1.427124 | 285.320102 | 24.193967 | 34.76225024 | -0.29835298 | 254.9998 | 56584.8902083333 | 2013-10-19 21:21:54 | 56586.2084837963 | 2013-10-21 05:00:13 | 508005010 | 55.6459 | 60 | 55.7019 | 55.6459 | 0 | 55.7008 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 47.4531 | 47.4531 | 113.8958 | 1 | PROCESSED | 57613.0578356482 | 2016-08-13 01:23:17 | 56967 | 2014-11-06 00:00:00 | 56597.6717824074 | 2013-11-01 16:07:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508005010/ | Quick Look | ![]() |
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644 | HESS J1534-571 4 | 233.6872 | -56.8979 | 232.705572 | -56.731059 | 246.296725 | -36.40404 | 323.85352453 | -0.81317458 | 295.9989 | 56545.1801157407 | 2013-09-10 04:19:22 | 56545.8042708333 | 2013-09-10 19:18:09 | 508016010 | 42.1696 | 40 | 42.1696 | 42.1936 | 0 | 42.1776 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.9419 | 39.9419 | 53.9199 | 0 | PROCESSED | 57612.5878587963 | 2016-08-12 14:06:31 | 56990 | 2014-11-29 00:00:00 | 56625.6134953704 | 2013-11-29 14:43:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | 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 J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target 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 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508016010/ | Quick Look | ![]() |
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645 | JUPITER | 103.7993 | 23.1163 | 103.042955 | 23.180911 | 102.674134 | 0.280458 | 192.50244401 | 11.09547038 | 264.3793 | 56762.0858912037 | 2014-04-15 02:03:41 | 56762.3890277778 | 2014-04-15 09:20:12 | 508023010 | 13.0905 | 160 | 13.0905 | 13.0905 | 0 | 13.0905 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.005 | 13.005 | 26.1839 | 0 | PROCESSED | 57614.2446527778 | 2016-08-14 05:52:18 | 57212 | 2015-07-09 00:00:00 | 56778.6117708333 | 2014-05-01 14:40:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023010/ | Quick Look | ![]() |
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646 | JUPITER | 104.0402 | 23.0972 | 103.284076 | 23.16295 | 102.896521 | 0.28265 | 192.61518388 | 11.28841687 | 264.4641 | 56764.0628125 | 2014-04-17 01:30:27 | 56764.1911805556 | 2014-04-17 04:35:18 | 508023070 | 4.5577 | 160 | 4.5577 | 4.5577 | 0 | 4.5737 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9502777778 | 2016-08-14 22:48:24 | 57212 | 2015-07-09 00:00:00 | 56782.4904976852 | 2014-05-05 11:46:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023070/ | Quick Look | ![]() |
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647 | JUPITER | 104.5088 | 23.0594 | 103.753114 | 23.127361 | 103.329251 | 0.287317 | 192.8346306 | 11.66394816 | 267.1301 | 56767.4497106482 | 2014-04-20 10:47:35 | 56767.7814583333 | 2014-04-20 18:45:18 | 508023120 | 11.1894 | 160 | 11.1894 | 11.1961 | 0 | 11.1974 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.962974537 | 2016-08-14 23:06:41 | 57212 | 2015-07-09 00:00:00 | 56789.8021759259 | 2014-05-12 19:15:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023120/ | Quick Look | ![]() |
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648 | RCW86_SE | 221.3859 | -62.671 | 220.394052 | -62.460463 | 241.394031 | -43.97094 | 315.61056381 | -2.64231092 | 96.79 | 54863.365787037 | 2009-02-01 08:46:44 | 54864.7550115741 | 2009-02-02 18:07:13 | 503004010 | 53.3274 | 50 | 53.3594 | 53.3274 | 0 | 53.3594 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.8136 | 47.8136 | 119.9879 | 0 | PROCESSED | 57545.4381481482 | 2016-06-06 10:30:56 | 55329 | 2010-05-13 00:00:00 | 54880.5420138889 | 2009-02-18 13:00:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503004010/ | Quick Look | ![]() |
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649 | GC_LARGEPROJECT4 | 266.0398 | -29.5556 | 265.241679 | -29.534433 | 266.526203 | -6.162189 | 359.30535174 | -0.05184233 | 261.05 | 54715.6640393518 | 2008-09-06 15:56:13 | 54717.0690277778 | 2008-09-08 01:39:24 | 503010010 | 53.1056 | 50 | 53.1216 | 53.1056 | 0 | 53.1136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.0646 | 37.0646 | 121.366 | 1 | PROCESSED | 57543.7725694444 | 2016-06-04 18:32:30 | 54557 | 2008-04-01 00:00:00 | 54780.6585648148 | 2008-11-10 15:48:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503010010/ | Quick Look | ![]() |
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650 | VELA PWN W2 | 127.3498 | -45.1919 | 126.932022 | -45.023781 | 151.542711 | -60.896813 | 262.94388066 | -3.64107383 | 303.5006 | 56439.0351851852 | 2013-05-27 00:50:40 | 56439.4696643518 | 2013-05-27 11:16:19 | 508043010 | 19.5844 | 15 | 19.5924 | 19.5844 | 0 | 19.6004 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.6266 | 15.6266 | 37.5339 | 1 | PROCESSED | 57611.391875 | 2016-08-11 09:24:18 | 56816 | 2014-06-08 00:00:00 | 56450.7935532407 | 2013-06-07 19:02:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, 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 western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508043010/ | Quick Look | ![]() |
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651 | GC_LARGEPROJECT10 | 264.8736 | -31.1751 | 264.065254 | -31.148261 | 265.564785 | -7.81275 | 357.39875369 | -0.05245192 | 268.5898 | 54731.2832060185 | 2008-09-22 06:47:49 | 54732.3383912037 | 2008-09-23 08:07:17 | 503016010 | 52.1712 | 50 | 52.1712 | 52.1792 | 0 | 52.1792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.2913 | 49.2913 | 91.1639 | 1 | PROCESSED | 57543.9863425926 | 2016-06-04 23:40:20 | 54557 | 2008-04-01 00:00:00 | 54780.6078935185 | 2008-11-10 14:35:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503016010/ | Quick Look | ![]() |
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652 | VELA PWN W3 | 126.9052 | -45.2087 | 126.488861 | -45.042306 | 150.998783 | -61.06652 | 262.77480933 | -3.90558145 | 95.0008 | 56590.9784606482 | 2013-10-25 23:28:59 | 56591.4343055556 | 2013-10-26 10:25:24 | 508044010 | 13.871 | 15 | 13.871 | 13.871 | 0 | 13.871 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.3448 | 11.3448 | 39.3799 | 1 | PROCESSED | 57613.1197106482 | 2016-08-13 02:52:23 | 57009 | 2014-12-18 00:00:00 | 56643.6595949074 | 2013-12-17 15:49:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, 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 western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508044010/ | Quick Look | ![]() |
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653 | GC_LARGEPROJECT15 | 265.2338 | -30.2129 | 264.431646 | -30.187819 | 265.84334 | -6.840443 | 358.37855715 | 0.19604348 | 267.777 | 54743.1555902778 | 2008-10-04 03:44:03 | 54744.4565277778 | 2008-10-05 10:57:24 | 503021010 | 53.826 | 50 | 53.834 | 53.834 | 0 | 53.826 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.6405 | 49.6405 | 112.3781 | 0 | PROCESSED | 57544.0429861111 | 2016-06-05 01:01:54 | 54557 | 2008-04-01 00:00:00 | 54780.430150463 | 2008-11-10 10:19:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503021010/ | Quick Look | ![]() |
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654 | SGR A | 266.5133 | -28.9285 | 265.71907 | -28.909638 | 266.925006 | -5.524591 | 0.05589981 | -0.0769322 | 266.9997 | 56555.4484490741 | 2013-09-20 10:45:46 | 56556.6446875 | 2013-09-21 15:28:21 | 508064010 | 50.4569 | 50 | 50.4569 | 50.4569 | 0 | 50.4569 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.2248 | 45.2248 | 103.308 | 0 | PROCESSED | 57612.6971527778 | 2016-08-12 16:43:54 | 56956 | 2014-10-26 00:00:00 | 56588.757025463 | 2013-10-23 18:10:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080143 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | YOSHITOMO MAEDA | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508064010/ | Quick Look | ![]() |
655 | HESS_J1825-137_2 | 276.1969 | -13.7002 | 275.488545 | -13.728547 | 276.096187 | 9.609358 | 17.73170044 | -0.43977824 | 271.0001 | 54756.4591666667 | 2008-10-17 11:01:12 | 54758.1953009259 | 2008-10-19 04:41:14 | 503029010 | 57.1993 | 50 | 57.1993 | 57.1993 | 0 | 57.1993 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.185 | 51.185 | 149.9858 | 0 | PROCESSED | 57544.2276157407 | 2016-06-05 05:27:46 | 55148 | 2009-11-13 00:00:00 | 54780.5081365741 | 2008-11-10 12:11:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAAKI TANAKA | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503029010/ | Quick Look | ![]() |
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656 | IRASF11223-1244 | 171.2239 | -12.9662 | 170.593283 | -12.69128 | 177.194404 | -15.365769 | 272.54538498 | 44.73919633 | 107.3062 | 54064.7275347222 | 2006-11-25 17:27:39 | 54065.5709953704 | 2006-11-26 13:42:14 | 701008010 | 40.9415 | 40 | 41.1015 | 40.9415 | 0 | 41.1095 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37.6804 | 37.6804 | 72.8639 | 1 | PROCESSED | 57536.1775925926 | 2016-05-28 04:15:44 | 54735 | 2008-09-26 00:00:00 | 54088.8556828704 | 2006-12-19 20:32:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 1 | AO1 | A SEARCH FOR HIDDEN QSO IN ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701008010/ | Quick Look | ![]() |
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657 | DDO 120 | 185.3167 | 45.8198 | 184.701182 | 46.097069 | 161.957395 | 43.126416 | 138.73502996 | 70.37152611 | 129.0479 | 56256.0169444444 | 2012-11-25 00:24:24 | 56258.4271990741 | 2012-11-27 10:15:10 | 807044010 | 101.7414 | 100 | 101.7414 | 101.7414 | 0 | 101.7414 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.0864 | 91.0864 | 208.1839 | 0 | PROCESSED | 57608.1579861111 | 2016-08-08 03:47:30 | 56644 | 2013-12-18 00:00:00 | 56275.7410648148 | 2012-12-14 17:47:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070107 | We propose to observe an irregular dwarf galaxy DDO120 to detect a hot interstellar medium associated with the dwarf galaxy. The study of the temperature and density of the gas will give us important information about the pollution of the intergalactic medium from galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RYO YAMAMOTO | JAP | 7 | AO7 | SEARCH FOR HOT INTERSTELLAR MEDIUM OF AN IRREGULAR DWARF GALAXY DDO 120 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807044010/ | Quick Look | ![]() |
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658 | HESSJ1614-A | 243.5214 | -52.1022 | 242.56254 | -51.975946 | 251.486678 | -30.347435 | 331.29897546 | -0.76107386 | 283.3889 | 54729.7629050926 | 2008-09-20 18:18:35 | 54730.562662037 | 2008-09-21 13:30:14 | 503073010 | 53.6494 | 50 | 53.6574 | 53.6494 | 0 | 53.6654 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.8713 | 40.8713 | 69.0719 | 0 | PROCESSED | 57543.9752662037 | 2016-06-04 23:24:23 | 55148 | 2009-11-13 00:00:00 | 54780.4246990741 | 2008-11-10 10:11:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503073010/ | Quick Look | ![]() |
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659 | HESSJ1832 | 278.156 | -8.4222 | 277.474303 | -8.460064 | 278.335703 | 14.782649 | 23.29856204 | 0.30967904 | 88.1963 | 55659.2543518518 | 2011-04-08 06:06:16 | 55660.3454282407 | 2011-04-09 08:17:25 | 506021010 | 40.3432 | 40 | 40.3432 | 40.3432 | 0 | 40.3432 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8513 | 34.8513 | 94.2578 | 1 | PROCESSED | 57601.464224537 | 2016-08-01 11:08:29 | 56043 | 2012-04-26 00:00:00 | 55673.2950925926 | 2011-04-22 07:04:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506021010/ | Quick Look | ![]() |
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660 | CYGNUS LOOP (P25) | 311.8608 | 32.1678 | 311.350497 | 31.982956 | 327.005863 | 47.670937 | 74.68970828 | -7.03578766 | 60.8878 | 54621.6278472222 | 2008-06-04 15:04:06 | 54622.1488888889 | 2008-06-05 03:34:24 | 503061010 | 25.9959 | 20 | 25.9959 | 25.9959 | 0 | 25.9959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8791 | 23.8791 | 45.01 | 0 | PROCESSED | 57542.7242476852 | 2016-06-03 17:22:55 | 55003 | 2009-06-21 00:00:00 | 54636.2508217593 | 2008-06-19 06:01:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503061010/ | Quick Look | ![]() |
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661 | IC1586 | 11.9805 | 22.3783 | 11.316843 | 22.105657 | 19.903516 | 15.841027 | 121.86323541 | -40.48615304 | 70.9045 | 55006.4686458333 | 2009-06-24 11:14:51 | 55007.0280555556 | 2009-06-25 00:40:24 | 704005010 | 23.5306 | 20 | 23.5306 | 24.3466 | 0 | 24.3546 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.2778 | 22.2778 | 48.3259 | 0 | PROCESSED | 57547.6510648148 | 2016-06-08 15:37:32 | 55385 | 2010-07-08 00:00:00 | 55019.1259259259 | 2009-07-07 03:01:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704005010/ | Quick Look | ![]() |
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662 | VELA PWN GEV3 | 128.0196 | -44.9062 | 127.597638 | -44.735505 | 152.091567 | -60.413918 | 262.99085627 | -3.09029782 | 119.9755 | 56986.5006481482 | 2014-11-25 12:00:56 | 56986.9105439815 | 2014-11-25 21:51:11 | 509013010 | 18.4893 | 15 | 18.4893 | 18.4969 | 0 | 18.4893 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8178009259 | 2016-08-16 19:37:38 | 57366 | 2015-12-10 00:00:00 | 57002.4411226852 | 2014-12-11 10:35:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509013010/ | Quick Look | ![]() |
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663 | VELA PWN GEV4 | 127.5996 | -44.9062 | 127.17888 | -44.73712 | 151.566964 | -60.561222 | 262.81539743 | -3.33071285 | 121.1346 | 56986.9114814815 | 2014-11-25 21:52:32 | 56987.558587963 | 2014-11-26 13:24:22 | 509014010 | 17.9817 | 15 | 17.9817 | 17.9897 | 0 | 17.9977 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8244328704 | 2016-08-16 19:47:11 | 57368 | 2015-12-12 00:00:00 | 57002.4392824074 | 2014-12-11 10:32:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509014010/ | Quick Look | ![]() |
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664 | G166.0+4.3_NE | 81.7715 | 42.9863 | 80.874617 | 42.944315 | 83.616156 | 19.728231 | 166.13139999 | 4.39632756 | 84.8097 | 56922.0215740741 | 2014-09-22 00:31:04 | 56923.3544444444 | 2014-09-23 08:30:24 | 509022020 | 58.5598 | 60 | 58.5598 | 61.5039 | 0 | 61.4879 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2.207 | 2.207 | 5.696 | 0 | PROCESSED | 57616.5872685185 | 2016-08-16 14:05:40 | 57312 | 2015-10-17 00:00:00 | 56945.1963657407 | 2014-10-15 04:42:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509022020/ | Quick Look | ![]() |
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665 | CIZA J1358.9-4750_NW | 209.4473 | -47.6057 | 208.659126 | -47.362265 | 225.512998 | -33.070935 | 314.36323033 | 13.78794346 | 293.0002 | 56880.8612615741 | 2014-08-11 20:40:13 | 56881.8265972222 | 2014-08-12 19:50:18 | 509028010 | 41.501 | 40 | 41.501 | 41.525 | 0 | 41.509 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.9918 | 7.9918 | 20.64 | 0 | PROCESSED | 57616.4817939815 | 2016-08-16 11:33:47 | 57267 | 2015-09-02 00:00:00 | 56898.4888657407 | 2014-08-29 11:43:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509028010/ | Quick Look | ![]() |
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666 | RADIO_ARC_SOUTH | 266.9853 | -29.0688 | 266.190093 | -29.052225 | 267.342882 | -5.6555 | 0.15000746 | -0.5026703 | 267.1998 | 56186.0290509259 | 2012-09-16 00:41:50 | 56188.8203472222 | 2012-09-18 19:41:18 | 507016010 | 103.472 | 100 | 103.472 | 103.472 | 0 | 103.472 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.1906 | 89.1906 | 241.1319 | 4 | PROCESSED | 57607.146875 | 2016-08-07 03:31:30 | 56668 | 2014-01-11 00:00:00 | 56303.6234490741 | 2013-01-11 14:57:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SYUKYO RYU | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507016010/ | Quick Look | ![]() |
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667 | VELA JR SE1 | 133.9641 | -46.7818 | 133.536852 | -46.589245 | 161.150153 | -59.841767 | 267.02895458 | -1.00032542 | 109.9994 | 56621.589525463 | 2013-11-25 14:08:55 | 56622.3175462963 | 2013-11-26 07:37:16 | 508060010 | 40.5996 | 40 | 40.5996 | 40.5996 | 0 | 40.6057 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6535 | 46.6535 | 62.8959 | 0 | PROCESSED | 57613.4271990741 | 2016-08-13 10:15:10 | 56998 | 2014-12-07 00:00:00 | 56632.5928240741 | 2013-12-06 14:13:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 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) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | TARO FUKUYAMA | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508060010/ | Quick Look | ![]() |
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668 | M31 | 10.6944 | 41.2627 | 10.010045 | 40.988882 | 27.852586 | 33.34214 | 121.18191229 | -21.57961988 | 231.6592 | 54115.6775578704 | 2007-01-15 16:15:41 | 54117.4572222222 | 2007-01-17 10:58:24 | 801043010 | 99.8723 | 100 | 99.8723 | 99.8723 | 0 | 99.8723 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.9124 | 103.9124 | 153.7238 | 1 | PROCESSED | 57536.8902777778 | 2016-05-28 21:22:00 | 54744 | 2008-10-05 00:00:00 | 54132.9457291667 | 2007-02-01 22:41:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMITSU TAKAHASHI | JAP | 1 | AO1 | DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801043010/ | Quick Look | ![]() |
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669 | RXJ1713-3946_ID1 | 257.9616 | -39.5166 | 257.09684 | -39.456462 | 260.331165 | -16.477991 | 347.33828294 | -0.06271892 | 87.0007 | 55242.129375 | 2010-02-15 03:06:18 | 55243.2502199074 | 2010-02-16 06:00:19 | 504027010 | 61.5331 | 60 | 61.5578 | 61.5331 | 0 | 61.5738 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46.7259 | 46.7259 | 96.8238 | 0 | PROCESSED | 57550.6101273148 | 2016-06-11 14:38:35 | 55622 | 2011-03-02 00:00:00 | 55253.4734259259 | 2010-02-26 11:21:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504027010/ | Quick Look | ![]() |
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670 | HESS J1745-303A | 265.7791 | -30.3241 | 264.976083 | -30.301658 | 266.320995 | -6.936807 | 358.53258375 | -0.26269922 | 103.33 | 55253.3854166667 | 2010-02-26 09:15:00 | 55254.6758796296 | 2010-02-27 16:13:16 | 504001010 | 51.1538 | 50 | 51.1618 | 51.1538 | 0 | 51.1685 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.2196 | 42.2196 | 111.4581 | 1 | PROCESSED | 57550.7381134259 | 2016-06-11 17:42:53 | 55636 | 2011-03-16 00:00:00 | 55267.2568634259 | 2010-03-12 06:09:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504001010/ | Quick Look | ![]() |
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671 | RADIO_ARC_S_E | 267.1914 | -28.7693 | 266.398054 | -28.753729 | 267.517971 | -5.352408 | 0.49965543 | -0.50260843 | 267.4999 | 56199.7928125 | 2012-09-29 19:01:39 | 56200.9349652778 | 2012-09-30 22:26:21 | 507017010 | 54.1782 | 50 | 54.2022 | 54.1782 | 0 | 54.202 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51.7936 | 51.7936 | 98.6799 | 0 | PROCESSED | 57607.2277777778 | 2016-08-07 05:28:00 | 56592 | 2013-10-27 00:00:00 | 56226.621400463 | 2012-10-26 14:54:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SYUKYO RYU | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507017010/ | Quick Look | ![]() |
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672 | BLOWOUT2 | 311.9515 | 31.5359 | 311.437845 | 31.350733 | 326.744585 | 47.059417 | 74.23825049 | -7.48819964 | 243.427 | 55158.9662615741 | 2009-11-23 23:11:25 | 55159.5106944444 | 2009-11-24 12:15:24 | 504012010 | 26.5494 | 23 | 26.5654 | 26.5494 | 0 | 26.5734 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.9401 | 19.9401 | 47.0319 | 1 | PROCESSED | 57549.5397800926 | 2016-06-10 12:57:17 | 55545 | 2010-12-15 00:00:00 | 55176.2336921296 | 2009-12-11 05:36:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504012010/ | Quick Look | ![]() |
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673 | W49B | 287.7847 | 9.1153 | 287.186342 | 9.031642 | 290.654992 | 31.289584 | 43.2812159 | -0.18378496 | 89.2674 | 54921.5302662037 | 2009-03-31 12:43:35 | 54923.0613425926 | 2009-04-02 01:28:20 | 504035010 | 61.7825 | 100 | 61.7905 | 61.7845 | 0 | 61.7825 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 55.1556 | 55.1556 | 132.2739 | 3 | PROCESSED | 57546.0146412037 | 2016-06-07 00:21:05 | 55324 | 2010-05-08 00:00:00 | 54949.4493287037 | 2009-04-28 10:47:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MIDORI OZAWA | JAP | 4 | AO4 | UNMASK THE NATURE OF W49B ! | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504035010/ | Quick Look | ![]() |
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674 | FESI2 | 313.183 | 30.3797 | 312.661298 | 30.190122 | 327.500793 | 45.583083 | 73.99193661 | -9.03499466 | 225.2405 | 55174.9860300926 | 2009-12-09 23:39:53 | 55175.7904398148 | 2009-12-10 18:58:14 | 504018010 | 34.5904 | 34 | 34.5904 | 34.5904 | 0 | 34.5904 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.318 | 30.318 | 69.4939 | 0 | PROCESSED | 57549.7573032407 | 2016-06-10 18:10:31 | 55555 | 2010-12-25 00:00:00 | 55189.1622916667 | 2009-12-24 03:53:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504018010/ | Quick Look | ![]() |
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675 | PKS 0558-504 | 89.9324 | -50.4401 | 89.628897 | -50.441186 | 89.861567 | -73.881962 | 257.95192858 | -28.57760064 | 211.3321 | 54120.8400925926 | 2007-01-20 20:09:44 | 54121.3279976852 | 2007-01-21 07:52:19 | 701011040 | 19.7381 | 20 | 19.7541 | 19.7381 | 0 | 19.7541 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.175 | 17.175 | 42.1359 | 0 | PROCESSED | 57536.8909953704 | 2016-05-28 21:23:02 | 54735 | 2008-09-26 00:00:00 | 54137.1036921296 | 2007-02-06 02:29:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011040/ | Quick Look | ![]() |
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676 | SWIFT J0255.2-0011 | 43.8161 | -0.2397 | 43.176621 | -0.441669 | 41.282729 | -16.217011 | 175.95402612 | -49.91735431 | 256.3177 | 54123.6209490741 | 2007-01-23 14:54:10 | 54126.2294560185 | 2007-01-26 05:30:25 | 701013010 | 101.6321 | 100 | 101.6321 | 101.6321 | 0 | 101.6321 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.2824 | 86.2824 | 225.3379 | 3 | PROCESSED | 57536.9811342593 | 2016-05-28 23:32:50 | 54735 | 2008-09-26 00:00:00 | 54137.3009027778 | 2007-02-06 07:13:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701013010/ | Quick Look | ![]() |
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677 | ESO 428-G014 | 109.1256 | -29.3248 | 108.632746 | -29.234716 | 116.992827 | -50.987581 | 241.87528565 | -7.96864273 | 123.1273 | 55516.1372569445 | 2010-11-16 03:17:39 | 55518.5508680556 | 2010-11-18 13:13:15 | 705008010 | 82.8873 | 80 | 82.9033 | 82.8873 | 0 | 82.9033 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.4518 | 68.4518 | 208.5016 | 2 | PROCESSED | 57554.1967361111 | 2016-06-15 04:43:18 | 55898 | 2011-12-03 00:00:00 | 55530.4256597222 | 2010-11-30 10:12:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 5 | AO5 | SUZAKU VIEW OF NON-HIDDEN BROAD LINE REGION SEYFERT 2 GALAXY ESO 428-G014 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705008010/ | Quick Look | ![]() |
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678 | SWIFT J0505.7-2348 | 76.4285 | -23.9055 | 75.907939 | -23.972083 | 71.84647 | -46.496539 | 225.00444872 | -33.15769393 | 284.9903 | 53826.9254166667 | 2006-04-01 22:12:36 | 53829.1216898148 | 2006-04-04 02:55:14 | 701014010 | 78.5544 | 80 | 78.5544 | 78.5544 | 78.5544 | 78.5544 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.4937 | 53.4937 | 189.6979 | 1 | PROCESSED | 57533.4023726852 | 2016-05-25 09:39:25 | 54439 | 2007-12-05 00:00:00 | 53945.2822569444 | 2006-07-29 06:46:27 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701014010/ | Quick Look | ![]() |
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679 | IRAS 01250+2832 | 21.9819 | 28.787 | 21.285155 | 28.528242 | 31.216552 | 18.139977 | 132.5132824 | -33.40495941 | 250.843 | 55571.3211805556 | 2011-01-10 07:42:30 | 55572.5926388889 | 2011-01-11 14:13:24 | 705024010 | 57.5829 | 50 | 57.5829 | 57.5829 | 0 | 57.5829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.8082 | 54.8082 | 109.8299 | 1 | PROCESSED | 57600.6088194444 | 2016-07-31 14:36:42 | 55962 | 2012-02-05 00:00:00 | 55595.2272569444 | 2011-02-03 05:27:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINKI OYABU | JAP | 5 | AO5 | SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705024010/ | Quick Look | ![]() |
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680 | IRAS 00521-7054 | 13.5029 | -70.6421 | 13.04558 | -70.91316 | 316.631077 | -63.690795 | 302.62218098 | -46.48460341 | 40.2116 | 56431.8840740741 | 2013-05-19 21:13:04 | 56434.2543287037 | 2013-05-22 06:06:14 | 708005010 | 103.045 | 100 | 103.053 | 103.045 | 0 | 103.053 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.3405 | 87.3405 | 204.7697 | 1 | PROCESSED | 57611.3837152778 | 2016-08-11 09:12:33 | 56809 | 2014-06-01 00:00:00 | 56443.6034259259 | 2013-05-31 14:28:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080036 | The existence of a broad iron line in AGN is still very debated. Amongst the several claims of detection of broad iron lines performed in the last decade, that of IRAS 00521-7054 is one of the most surprising. This type-2 object appears to show in fact an extremely broadened iron line, which would require a maximally rotating supermassive black hole and the presence of light bending. However, due to the lack of high-quality broadband studies, alternative explanations, as a clumpy-absorbers scenario, cannot be ruled out. The aim of this proposal is to perform a 100ks observation of IRAS 00521-7054. Thanks to its large band coverage and its good sensitivity in the iron-line region, Suzaku will allow us to clearly understand the origin of the intriguing spectral features of IRAS 00521-7054. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CLAUDIO RICCI | JAP | 8 | AO8 | UNDERSTANDING THE ORIGIN OF THE PECULIAR X-RAY SPECTRAL FEATURES OF THE SEYFERT 2 IRAS 00521-7054 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708005010/ | Quick Look | ![]() |
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681 | 3C_397 | 286.9038 | 7.1223 | 286.296185 | 7.042755 | 289.336416 | 29.435283 | 41.11064468 | -0.32936267 | 256.5108 | 55493.8258449074 | 2010-10-24 19:49:13 | 55495.8022337963 | 2010-10-26 19:15:13 | 505008010 | 69.3266 | 70 | 69.3266 | 69.3266 | 0 | 69.3266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62.1653 | 62.1653 | 170.7319 | 0 | PROCESSED | 57553.8922800926 | 2016-06-14 21:24:53 | 55287 | 2010-04-01 00:00:00 | 55505.3393981482 | 2010-11-05 08:08:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505008010/ | Quick Look | ![]() |
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682 | SWIFT J0138.6-4001 | 24.6022 | -39.9757 | 24.058156 | -40.229446 | 3.045259 | -45.758208 | 268.75310615 | -73.8819888 | 44.7851 | 53890.7590740741 | 2006-06-04 18:13:04 | 53891.2085532407 | 2006-06-05 05:00:19 | 701015010 | 21.1979 | 20 | 21.2139 | 21.1979 | 21.2139 | 21.2139 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.4771 | 17.4771 | 38.8319 | 1 | PROCESSED | 57534.4839814815 | 2016-05-26 11:36:56 | 54394 | 2007-10-21 00:00:00 | 53926.7722337963 | 2006-07-10 18:32:01 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701015010/ | Quick Look | ![]() |
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683 | SWIFT J0350.1-5019 | 57.5863 | -50.3518 | 57.229549 | -50.501821 | 28.784936 | -67.035424 | 259.75531799 | -48.98660415 | 277.9348 | 54162.2927777778 | 2007-03-03 07:01:36 | 54162.5036921296 | 2007-03-03 12:05:19 | 701017030 | 8.1487 | 10 | 8.1567 | 8.1487 | 0 | 8.1567 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.0597 | 7.0597 | 18.2159 | 0 | PROCESSED | 57537.5866898148 | 2016-05-29 14:04:50 | 54750 | 2008-10-11 00:00:00 | 54167.6235763889 | 2007-03-08 14:57:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017030/ | Quick Look | ![]() |
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684 | TON S180 | 14.333 | -22.3803 | 13.720307 | -22.650448 | 3.73482 | -26.131336 | 138.98529016 | -85.06726133 | 237.1425 | 54078.5680671296 | 2006-12-09 13:38:01 | 54081.3584953704 | 2006-12-12 08:36:14 | 701021010 | 120.6609 | 120 | 120.6849 | 120.6609 | 0 | 120.6769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.3128 | 109.3128 | 241.052 | 3 | PROCESSED | 57536.3458680556 | 2016-05-28 08:18:03 | 54735 | 2008-09-26 00:00:00 | 54094.4773958333 | 2006-12-25 11:27:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | SOFT X-RAY EMISSION FROM SUPER-EDDINGTON ACCRETION DISK IN TON S180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701021010/ | Quick Look | ![]() |
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685 | CYGNUS LOOP 5 | 312.0188 | 31.9594 | 311.507127 | 31.773986 | 327.066622 | 47.426634 | 74.60885135 | -7.27014396 | 81.8368 | 55305.8645833333 | 2010-04-19 20:45:00 | 55306.4578125 | 2010-04-20 10:59:15 | 505013010 | 26.8452 | 26 | 26.8452 | 26.8452 | 0 | 26.8452 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.277 | 21.277 | 51.232 | 2 | PROCESSED | 57551.2602083333 | 2016-06-12 06:14:42 | 55287 | 2010-04-01 00:00:00 | 55364.2036458333 | 2010-06-17 04:53:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505013010/ | Quick Look | ![]() |
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686 | CYGNUS LOOP 11 | 313.8693 | 30.5587 | 313.347105 | 30.366695 | 328.378211 | 45.516461 | 74.51088669 | -9.3807208 | 82.002 | 55328.698587963 | 2010-05-12 16:45:58 | 55329.1251736111 | 2010-05-13 03:00:15 | 505019010 | 18.8976 | 18 | 18.9056 | 18.8976 | 0 | 18.9136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9048 | 14.9048 | 36.8539 | 1 | PROCESSED | 57551.490150463 | 2016-06-12 11:45:49 | 55287 | 2010-04-01 00:00:00 | 55393.3619791667 | 2010-07-16 08:41:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505019010/ | Quick Look | ![]() |
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687 | WESTERLUND1_4 | 253.5509 | -45.3005 | 252.641306 | -45.219522 | 257.53427 | -22.567529 | 340.7711384 | -1.01287357 | 288.2868 | 55463.3974652778 | 2010-09-24 09:32:21 | 55464.5203587963 | 2010-09-25 12:29:19 | 505052010 | 49.627 | 50 | 49.627 | 49.627 | 0 | 49.627 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2137 | 40.2137 | 97.0079 | 1 | PROCESSED | 57553.5510416667 | 2016-06-14 13:13:30 | 55840 | 2011-10-06 00:00:00 | 55474.1080208333 | 2010-10-05 02:35:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505052010/ | Quick Look | ![]() |
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688 | NGC5135 | 201.4174 | -29.8897 | 200.719488 | -29.629866 | 211.188294 | -19.343803 | 311.72101463 | 32.39717213 | 286.1252 | 54284.2497800926 | 2007-07-03 05:59:41 | 54285.3057175926 | 2007-07-04 07:20:14 | 702005010 | 52.4964 | 50 | 52.4964 | 52.4964 | 0 | 52.4964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.7837 | 49.7837 | 91.2209 | 2 | PROCESSED | 57539.1022222222 | 2016-05-31 02:27:12 | 54696 | 2008-08-18 00:00:00 | 54328.4497453704 | 2007-08-16 10:47:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702005010/ | Quick Look | ![]() |
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689 | NGC5643 | 218.1422 | -44.2268 | 217.336243 | -44.006582 | 230.485298 | -27.635672 | 321.40267054 | 14.9878026 | 293.4229 | 54331.8795023148 | 2007-08-19 21:06:29 | 54332.9724421296 | 2007-08-20 23:20:19 | 702010010 | 42.8823 | 50 | 42.8903 | 42.8903 | 0 | 42.8823 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8685 | 40.8685 | 94.386 | 2 | PROCESSED | 57539.6330902778 | 2016-05-31 15:11:39 | 54770 | 2008-10-31 00:00:00 | 54402.2016782407 | 2007-10-29 04:50:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702010010/ | Quick Look | ![]() |
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690 | NGC 7314 | 338.9055 | -25.9984 | 338.214858 | -26.257583 | 330.662233 | -15.873025 | 27.22535085 | -59.7013223 | 59.6979 | 54215.4316319444 | 2007-04-25 10:21:33 | 54217.9516666667 | 2007-04-27 22:50:24 | 702015010 | 109.0198 | 100 | 109.0198 | 109.0198 | 0 | 109.0198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.2408 | 92.2408 | 217.7139 | 2 | PROCESSED | 57538.5280439815 | 2016-05-30 12:40:23 | 54744 | 2008-10-05 00:00:00 | 54230.4096527778 | 2007-05-10 09:49:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 2 | AO2 | RAPID SPECTRAL X-RAY VARIABILITY IN THE SEYFERT GALAXY NGC 7314: UNDERSTANDING ENERGY RELEASE PROCESSES IN AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702015010/ | Quick Look | ![]() |
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691 | IGR J21247+5058 | 321.1969 | 51.0428 | 320.772046 | 50.826527 | 353.918258 | 60.483587 | 93.38215801 | 0.42876214 | 108.8126 | 54206.5871759259 | 2007-04-16 14:05:32 | 54208.4613888889 | 2007-04-18 11:04:24 | 702027010 | 85.0319 | 80 | 85.0319 | 85.0399 | 0 | 85.0479 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.9709 | 70.9709 | 161.8949 | 2 | PROCESSED | 57538.4530671296 | 2016-05-30 10:52:25 | 54744 | 2008-10-05 00:00:00 | 54214.1071412037 | 2007-04-24 02:34:17 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 2 | AO2 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702027010/ | Quick Look | ![]() |
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692 | MRK 1239 | 148.0816 | -1.6118 | 147.44487 | -1.376316 | 150.825441 | -13.652204 | 239.27134701 | 38.21950621 | 286.5242 | 54226.0919907407 | 2007-05-06 02:12:28 | 54227.5973726852 | 2007-05-07 14:20:13 | 702031010 | 63.128 | 80 | 63.128 | 63.128 | 0 | 63.128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.5944 | 53.5944 | 130.0619 | 2 | PROCESSED | 57615.5991435185 | 2016-08-15 14:22:46 | 54744 | 2008-10-05 00:00:00 | 54235.4602662037 | 2007-05-15 11:02:47 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 2 | AO2 | SUZAKU VIEW OF "HIDDEN" NARROW-LINE SEYFERT 1 GALAXY MRK 1239 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702031010/ | Quick Look | ![]() |
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693 | JUPITER | 29.0345 | 10.6283 | 28.369064 | 10.38411 | 30.736601 | -1.177073 | 147.65759499 | -49.11229838 | 249.1849 | 55938.2087962963 | 2012-01-12 05:00:40 | 55939.2481944444 | 2012-01-13 05:57:24 | 506006040 | 38.6289 | 160 | 38.6289 | 38.6367 | 0 | 38.6369 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.7692 | 31.7692 | 89.7859 | 0 | PROCESSED | 57604.3463657407 | 2016-08-04 08:18:46 | 56388 | 2013-04-06 00:00:00 | 56020.1680208333 | 2012-04-03 04:01:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006040/ | Quick Look | ![]() |
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694 | CYGNUS LOOP BLOWOUT1 | 312.1499 | 29.2487 | 311.624762 | 29.062833 | 325.710057 | 44.881262 | 72.53069275 | -9.03908096 | 78.1532 | 55686.7775578704 | 2011-05-05 18:39:41 | 55687.8494907407 | 2011-05-06 20:23:16 | 506011010 | 48.5641 | 50 | 48.5641 | 48.5641 | 0 | 48.5641 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.0429 | 42.0429 | 92.5799 | 1 | PROCESSED | 57601.954224537 | 2016-08-01 22:54:05 | 56066 | 2012-05-19 00:00:00 | 55698.3278472222 | 2011-05-17 07:52:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506011010/ | Quick Look | ![]() |
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695 | GAMMACYGNI_NWSHELL2 | 304.652 | 40.6975 | 304.208167 | 40.540107 | 324.021819 | 57.820534 | 78.12229495 | 2.68416641 | 82.9982 | 55665.3027430556 | 2011-04-14 07:15:57 | 55666.2688657407 | 2011-04-15 06:27:10 | 506018010 | 39.712 | 40 | 39.712 | 39.712 | 0 | 39.712 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.1165 | 36.1165 | 83.4379 | 0 | PROCESSED | 57601.5048032407 | 2016-08-01 12:06:55 | 56058 | 2012-05-11 00:00:00 | 55690.9818402778 | 2011-05-09 23:33:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 6 | AO6 | SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506018010/ | Quick Look | ![]() |
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696 | S147_N | 87.0463 | 27.5187 | 86.260987 | 27.502453 | 87.375766 | 4.104837 | 181.50494456 | -0.25223067 | 273.8998 | 55997.2930324074 | 2012-03-11 07:01:58 | 55998.555787037 | 2012-03-12 13:20:20 | 506031010 | 54.8833 | 55 | 54.8913 | 54.8833 | 0 | 54.8913 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.1919 | 52.1919 | 109.054 | 1 | PROCESSED | 57604.8728472222 | 2016-08-04 20:56:54 | 56385 | 2013-04-03 00:00:00 | 56016.6668287037 | 2012-03-30 16:00:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA HANABATA | JAP | 6 | AO6 | STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506031010/ | Quick Look | ![]() |
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697 | PKS0208-512 | 32.6864 | -51.0102 | 32.231145 | -51.245187 | 0.269734 | -58.029766 | 276.09849974 | -61.78596913 | 230.2146 | 54814.3149074074 | 2008-12-14 07:33:28 | 54815.4793171296 | 2008-12-15 11:30:13 | 703002010 | 51.9594 | 40 | 51.9834 | 51.9594 | 0 | 51.9834 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.559 | 42.559 | 100.5999 | 0 | PROCESSED | 57544.9648032407 | 2016-06-05 23:09:19 | 54557 | 2008-04-01 00:00:00 | 54826.3087268518 | 2008-12-26 07:24:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703002010/ | Quick Look | ![]() |
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698 | 4C73.08 | 147.4414 | 73.2521 | 146.291521 | 73.485172 | 114.906674 | 54.77086 | 138.04435007 | 38.07252036 | 100.3847 | 54786.9238888889 | 2008-11-16 22:10:24 | 54788.4946643518 | 2008-11-18 11:52:19 | 703018010 | 81.3752 | 80 | 81.3752 | 81.3752 | 0 | 81.3752 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.4533 | 72.4533 | 135.692 | 0 | PROCESSED | 57544.4300694444 | 2016-06-05 10:19:18 | 55164 | 2009-11-29 00:00:00 | 54798.0487152778 | 2008-11-28 01:10:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI YAJI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF LOBES OF GIANT RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703018010/ | Quick Look | ![]() |
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699 | ERIDANUS_ARCB_SPOT | 53.3104 | -9.6904 | 52.708102 | -9.857933 | 48.180187 | -27.963294 | 196.20250346 | -48.10218961 | 67.1761 | 56138.1083101852 | 2012-07-30 02:35:58 | 56139.0792476852 | 2012-07-31 01:54:07 | 507032010 | 40.6186 | 40 | 40.6186 | 40.6186 | 0 | 40.6186 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.171 | 35.171 | 83.8699 | 1 | PROCESSED | 57606.7122337963 | 2016-08-06 17:05:37 | 56528 | 2013-08-24 00:00:00 | 56162.0431018518 | 2012-08-23 01:02:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NORIKO YAMASAKI | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE ERIDANUS SUPER BUBBLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507032010/ | Quick Look | ![]() |
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700 | FERMI_BUBBLE_S1 | 329.068 | -46.6182 | 328.273423 | -46.856069 | 313.852963 | -31.76179 | 351.41726681 | -50.59485428 | 44.0071 | 56034.6949884259 | 2012-04-17 16:40:47 | 56035.2070717593 | 2012-04-18 04:58:11 | 507009010 | 25.3149 | 20 | 25.3149 | 25.3229 | 0 | 25.3229 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.7973 | 24.7973 | 44.2399 | 0 | PROCESSED | 57605.1828703704 | 2016-08-05 04:23:20 | 56420 | 2013-05-08 00:00:00 | 56049.2134722222 | 2012-05-02 05:07:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507009010/ | Quick Look | ![]() |
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701 | MRK 573 | 26.0161 | 2.2904 | 25.370891 | 2.039517 | 24.959775 | -7.914401 | 148.3199793 | -57.9636564 | 249.71 | 55217.5861226852 | 2010-01-21 14:04:01 | 55219.0328587963 | 2010-01-23 00:47:19 | 704002010 | 64.3118 | 60 | 64.3118 | 64.3118 | 0 | 64.3118 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.7471 | 53.7471 | 124.992 | 0 | PROCESSED | 57550.3256944445 | 2016-06-11 07:49:00 | 55612 | 2011-02-20 00:00:00 | 55245.753599537 | 2010-02-18 18:05:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 4 | AO4 | SEARCH FOR COMPTON THICK AGNS WITH A HEAVILY ABSORBED REFLECTION COMPONENT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704002010/ | Quick Look | ![]() |
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702 | IC 443 | 94.3026 | 22.7461 | 93.545529 | 22.76515 | 93.969538 | -0.635542 | 188.89781567 | 3.10590753 | 258.9991 | 56382.4892824074 | 2013-03-31 11:44:34 | 56385.8835763889 | 2013-04-03 21:12:21 | 507015030 | 131.1823 | 300 | 131.1823 | 131.1823 | 0 | 131.1823 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113.8514 | 113.8514 | 293.2478 | 1 | PROCESSED | 57611.0338194444 | 2016-08-11 00:48:42 | 56018 | 2012-04-01 00:00:00 | 56394.7872337963 | 2013-04-12 18:53:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015030/ | Quick Look | ![]() |
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703 | CYG_BGD2 | 306.9576 | 42.391 | 306.519882 | 42.224487 | 328.379789 | 58.578032 | 80.50042704 | 2.23726855 | 218.3998 | 56280.6304166667 | 2012-12-19 15:07:48 | 56281.1313888889 | 2012-12-20 03:09:12 | 507042010 | 25.6249 | 25 | 25.6249 | 25.6249 | 0 | 25.6489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.025 | 25.025 | 43.2739 | 1 | PROCESSED | 57608.3181018518 | 2016-08-08 07:38:04 | 56683 | 2014-01-26 00:00:00 | 56316.5346990741 | 2013-01-24 12:49:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TSUNEFUMI MIZUNO | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507042010/ | Quick Look | ![]() |
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704 | VELA PWN N5 | 128.8386 | -43.7507 | 128.405645 | -43.5769 | 151.977516 | -59.119722 | 262.41040878 | -1.9318018 | 327.6005 | 56110.3470717593 | 2012-07-02 08:19:47 | 56110.6620138889 | 2012-07-02 15:53:18 | 507052010 | 18.1486 | 15 | 18.1566 | 18.1486 | 0 | 18.1566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.4582 | 17.4582 | 27.208 | 1 | PROCESSED | 57606.5339930556 | 2016-08-06 12:48:57 | 56493 | 2013-07-20 00:00:00 | 56127.126712963 | 2012-07-19 03:02:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507052010/ | Quick Look | ![]() |
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705 | JUPITER | 104.3277 | 23.0738 | 103.571845 | 23.140907 | 103.162022 | 0.285142 | 192.75008442 | 11.51865374 | 264.5662 | 56766.1211111111 | 2014-04-19 02:54:24 | 56766.4481365741 | 2014-04-19 10:45:19 | 508023080 | 15.9616 | 160 | 15.9776 | 15.9616 | 0 | 15.9806 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9566782407 | 2016-08-14 22:57:37 | 57212 | 2015-07-09 00:00:00 | 56782.5045486111 | 2014-05-05 12:06:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023080/ | Quick Look | ![]() |
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706 | SWIFT J2248.8+1725 | 342.1903 | 17.444 | 341.576565 | 17.179413 | 350.711211 | 23.025613 | 85.72592105 | -36.41328844 | 248.2402 | 56997.6938888889 | 2014-12-06 16:39:12 | 56999.668287037 | 2014-12-08 16:02:20 | 709004010 | 78.0938 | 80 | 78.0938 | 78.0938 | 0 | 78.0938 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.8266 | 68.8266 | 170.56 | 1 | PROCESSED | 57617.5240046296 | 2016-08-17 12:34:34 | 57460 | 2016-03-13 00:00:00 | 57092.3224652778 | 2015-03-11 07:44:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090018 | We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance 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 fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI TERASHIMA | JAP | 9 | AO9 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709004010/ | Quick Look | ![]() |
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707 | A133_E | 15.9075 | -21.8935 | 15.297134 | -22.16169 | 5.436545 | -26.315725 | 151.49316881 | -84.07673835 | 44.9955 | 55356.7284953704 | 2010-06-09 17:29:02 | 55358.0015393518 | 2010-06-11 00:02:13 | 805021010 | 51.5523 | 50 | 51.5641 | 51.5603 | 0 | 51.5523 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.2547 | 46.2547 | 109.984 | 1 | PROCESSED | 57551.9411458333 | 2016-06-12 22:35:15 | 55737 | 2011-06-25 00:00:00 | 55375.7548842593 | 2010-06-28 18:07:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805021010/ | Quick Look | ![]() |
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708 | 1216-015 | 184.787 | -1.8118 | 184.145709 | -1.534245 | 185.108736 | 0.239101 | 286.61259693 | 60.03288042 | 293.8466 | 55010.1063773148 | 2009-06-28 02:33:11 | 55010.6043287037 | 2009-06-28 14:30:14 | 704006010 | 20.7779 | 20 | 20.7779 | 20.7859 | 0 | 20.7859 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57547.6897337963 | 2016-06-08 16:33:13 | 55388 | 2010-07-11 00:00:00 | 55020.3653009259 | 2009-07-08 08:46:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704006010/ | Quick Look | ![]() |
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709 | UGC 12741 | 355.4449 | 30.6414 | 354.81812 | 30.364038 | 9.270542 | 29.65828 | 105.65559107 | -29.88276227 | 64.429 | 54989.5219560185 | 2009-06-07 12:31:37 | 54990.6711111111 | 2009-06-08 16:06:24 | 704014010 | 47.9458 | 40 | 47.9538 | 47.9458 | 0 | 47.9458 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41.5244 | 41.5244 | 99.2799 | 0 | PROCESSED | 57547.5132060185 | 2016-06-08 12:19:01 | 55367 | 2010-06-20 00:00:00 | 55001.0091435185 | 2009-06-19 00:13:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704014010/ | Quick Look | ![]() |
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710 | JUPITER | 103.925 | 23.1078 | 103.168762 | 23.173006 | 102.79003 | 0.283016 | 192.55993514 | 11.19674467 | 264.4254 | 56763.06625 | 2014-04-16 01:35:24 | 56763.3890162037 | 2014-04-16 09:20:11 | 508023040 | 14.5693 | 160 | 14.5773 | 14.5693 | 0 | 14.5847 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9505902778 | 2016-08-14 22:48:51 | 57212 | 2015-07-09 00:00:00 | 56839.6932175926 | 2014-07-01 16:38:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023040/ | Quick Look | ![]() |
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711 | NGC 3431 | 162.8114 | -17.015 | 162.196181 | -16.749458 | 171.110311 | -22.386386 | 266.03803779 | 37.10135134 | 298.5009 | 56089.5660648148 | 2012-06-11 13:35:08 | 56091.5571412037 | 2012-06-13 13:22:17 | 707012010 | 65.6756 | 70 | 65.6756 | 65.6756 | 0 | 65.6756 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.8819 | 59.8819 | 171.9959 | 2 | PROCESSED | 57605.6909259259 | 2016-08-05 16:34:56 | 56473 | 2013-06-30 00:00:00 | 56106.3662384259 | 2012-06-28 08:47:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | POSHAK GANDHI | JAP | 7 | AO7 | WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707012010/ | Quick Look | ![]() |
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712 | HESS J1534-571 3 | 234.1055 | -57.4189 | 233.115127 | -57.253673 | 246.756574 | -36.836074 | 323.73309574 | -1.36851406 | 296.0043 | 56544.6705787037 | 2013-09-09 16:05:38 | 56545.1793171296 | 2013-09-10 04:18:13 | 508015010 | 38.7487 | 40 | 38.7727 | 38.7647 | 0 | 38.7487 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.947 | 29.947 | 43.9439 | 0 | PROCESSED | 57612.5739814815 | 2016-08-12 13:46:32 | 56956 | 2014-10-26 00:00:00 | 56588.8303125 | 2013-10-23 19:55:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | 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 J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target 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 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508015010/ | Quick Look | ![]() |
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713 | HESSJ1858-A | 284.5878 | 2.0823 | 283.956685 | 2.013656 | 286.075284 | 24.712449 | 35.57325236 | -0.58765875 | 251.7991 | 56592.8339467593 | 2013-10-27 20:00:53 | 56593.9759027778 | 2013-10-28 23:25:18 | 508021010 | 51.6531 | 50 | 51.6611 | 51.6691 | 0 | 51.6531 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.7792 | 48.7792 | 98.6558 | 1 | PROCESSED | 57613.1533796296 | 2016-08-13 03:40:52 | 56975 | 2014-11-14 00:00:00 | 56608.6801388889 | 2013-11-12 16:19:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080052 | 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 | B | HIRONORI MATSUMOTO | JAP | 8 | AO8 | DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508021010/ | Quick Look | ![]() |
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714 | ARK 347 | 181.0952 | 20.2476 | 180.45595 | 20.52594 | 172.634722 | 18.942585 | 243.01628342 | 77.22827936 | 294.4295 | 55377.99625 | 2010-06-30 23:54:36 | 55378.8668171296 | 2010-07-01 20:48:13 | 705002010 | 38.9726 | 40 | 38.9886 | 38.9726 | 0 | 38.9886 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.9876 | 35.9876 | 75.2099 | 0 | PROCESSED | 57552.4401851852 | 2016-06-13 10:33:52 | 55772 | 2011-07-30 00:00:00 | 55404.2387268518 | 2010-07-27 05:43:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 5 | AO5 | THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705002010/ | Quick Look | ![]() |
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715 | HESS J1534-571 1 | 234.0464 | -57.1146 | 233.060336 | -56.949151 | 246.608003 | -36.554258 | 323.88573784 | -1.10331415 | 295.9997 | 56543.4345138889 | 2013-09-08 10:25:42 | 56544.0210300926 | 2013-09-09 00:30:17 | 508013010 | 36.891 | 40 | 36.899 | 36.891 | 0 | 36.899 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36.0704 | 36.0704 | 50.6719 | 0 | PROCESSED | 57612.5616319444 | 2016-08-12 13:28:45 | 56990 | 2014-11-29 00:00:00 | 56622.6022569444 | 2013-11-26 14:27:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | 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 J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target 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 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508013010/ | Quick Look | ![]() |
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716 | SGR C | 266.1575 | -29.4721 | 265.359887 | -29.451505 | 266.626891 | -6.075935 | 359.43010365 | -0.09543697 | 265.018 | 56559.2657060185 | 2013-09-24 06:22:37 | 56561.8960763889 | 2013-09-26 21:30:21 | 508019010 | 104.2256 | 100 | 104.2495 | 104.2415 | 0 | 104.2256 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.1975 | 91.1975 | 227.2419 | 1 | PROCESSED | 57612.8165277778 | 2016-08-12 19:35:48 | 56956 | 2014-10-26 00:00:00 | 56588.6596643518 | 2013-10-23 15:49:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080043 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508019010/ | Quick Look | ![]() |
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717 | EMS0873 | 200.796 | 29.7234 | 200.211284 | 29.984115 | 186.018841 | 35.27496 | 55.1881509 | 82.55574598 | 136.0743 | 55527.7704976852 | 2010-11-27 18:29:31 | 55528.2800231482 | 2010-11-28 06:43:14 | 705029010 | 22.7849 | 20 | 22.7849 | 22.7849 | 0 | 22.7849 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.8106 | 20.8106 | 44.0079 | 2 | PROCESSED | 57554.227974537 | 2016-06-15 05:28:17 | 55903 | 2011-12-08 00:00:00 | 55536.9832523148 | 2010-12-06 23:35:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705029010/ | Quick Look | ![]() |
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718 | VELA PWN GEV2 | 128.4409 | -44.9066 | 128.017684 | -44.734295 | 152.61498 | -60.265788 | 263.16834954 | -2.85026128 | 119.7193 | 56985.851099537 | 2014-11-24 20:25:35 | 56986.5001273148 | 2014-11-25 12:00:11 | 509012010 | 19.1078 | 15 | 19.1398 | 19.1238 | 0 | 19.1078 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8168981482 | 2016-08-16 19:36:20 | 57366 | 2015-12-10 00:00:00 | 57009.4112268518 | 2014-12-18 09:52:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509012010/ | Quick Look | ![]() |
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719 | NGC 4785 | 193.3693 | -48.746 | 192.657492 | -48.474679 | 214.374181 | -38.980118 | 303.27856941 | 14.12437615 | 296.8629 | 56495.4767013889 | 2013-07-22 11:26:27 | 56496.6341782407 | 2013-07-23 15:13:13 | 708003010 | 79.3882 | 70 | 79.3882 | 79.3962 | 0 | 79.3882 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.777 | 70.777 | 99.994 | 0 | PROCESSED | 57611.9465972222 | 2016-08-11 22:43:06 | 56876 | 2014-08-07 00:00:00 | 56509.7469907407 | 2013-08-05 17:55:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080027 | At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | POSHAK GANDHI | JAP | 8 | AO8 | THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708003010/ | Quick Look | ![]() |
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720 | Cen A | 201.3695 | -43.0177 | 200.636124 | -42.757733 | 217.139897 | -31.325572 | 309.51950829 | 19.41821819 | 303.9158 | 53601.1523032407 | 2005-08-19 03:39:19 | 53602.4098148148 | 2005-08-20 09:50:08 | 100005010 | 64.6759 | 40 | 64.6942 | 64.7658 | 64.6759 | 64.7399 | 5 | 2 | 5 | 5 | 1 | 0 | 0 | 66.2582 | 66.2582 | 108.6119 | 0 | PROCESSED | 57520.7361921296 | 2016-05-12 17:40:07 | 53705 | 2005-12-01 00:00:00 | 53905.4597106482 | 2006-06-19 11:01:59 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000005 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Cen A | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100005010/ | Quick Look | ![]() |
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721 | 1FGL J1311.7-3429 | 197.9423 | -34.512 | 197.244044 | -34.24657 | 210.304099 | -24.759106 | 307.68226276 | 28.17214982 | 298.263 | 55774.7002314815 | 2011-08-01 16:48:20 | 55776.7362847222 | 2011-08-03 17:40:15 | 706001010 | 82.4771 | 80 | 82.4771 | 82.4771 | 0 | 82.4771 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.3737 | 70.3737 | 175.8638 | 2 | PROCESSED | 57602.7690046296 | 2016-08-02 18:27:22 | 56219 | 2012-10-19 00:00:00 | 55851.4595601852 | 2011-10-17 11:01:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF "NEW-TYPE'' GAMMA-RAY SOURCES DETECTED WITH FERMI-LAT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706001010/ | Quick Look | ![]() |
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722 | 1FGL J1946.7-5404 | 296.6052 | -54.0506 | 295.618874 | -54.173159 | 288.105396 | -32.270844 | 343.89458124 | -29.55670998 | 268.6577 | 55865.7799074074 | 2011-10-31 18:43:04 | 55866.783599537 | 2011-11-01 18:48:23 | 706026010 | 42.3959 | 40 | 42.3959 | 42.3988 | 0 | 42.3988 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.8833 | 54.8833 | 86.7079 | 0 | PROCESSED | 57603.6796990741 | 2016-08-03 16:18:46 | 56246 | 2012-11-15 00:00:00 | 55879.1861574074 | 2011-11-14 04:28:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOTO MAEDA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706026010/ | Quick Look | ![]() |
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723 | PERSEUS H_2 | 50.3295 | 41.6532 | 49.500037 | 41.47397 | 58.944091 | 22.396043 | 150.73770492 | -12.98651547 | 259.0589 | 56327.8720949074 | 2013-02-04 20:55:49 | 56328.3355092593 | 2013-02-05 08:03:08 | 807021010 | 20.3456 | 20 | 20.3636 | 20.3456 | 0 | 20.3536 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.8776 | 21.8776 | 40.034 | 0 | PROCESSED | 57610.5111921296 | 2016-08-10 12:16:07 | 56715 | 2014-02-27 00:00:00 | 56349.4892708333 | 2013-02-26 11:44:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807021010/ | Quick Look | ![]() |
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724 | HESS J1641-463 | 250.2616 | -46.3013 | 249.347836 | -46.205158 | 255.208281 | -23.867274 | 338.52580532 | 0.09066192 | 282.4572 | 56900.1342939815 | 2014-08-31 03:13:23 | 56902.1166435185 | 2014-09-02 02:47:58 | 509010020 | 0 | 40 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5303356482 | 2016-08-16 12:43:41 | 56748 | 2014-04-01 00:00:00 | 57122.3887268518 | 2015-04-10 09:19:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090045 | The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 9 | AO9 | IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509010020/ | Quick Look | ![]() |
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725 | RX J1633+4718 | 248.3342 | 47.2989 | 247.973952 | 47.402455 | 228.776709 | 67.659807 | 73.52584527 | 42.62417772 | 308.6809 | 55760.5047916667 | 2011-07-18 12:06:54 | 55761.4376388889 | 2011-07-19 10:30:12 | 706027020 | 37.51 | 40 | 37.51 | 37.51 | 0 | 37.51 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57602.5962847222 | 2016-08-02 14:18:39 | 56152 | 2012-08-13 00:00:00 | 55830.7262268518 | 2011-09-26 17:25:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027020/ | Quick Look | ![]() |
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726 | CIZA J1358.9-4750_SE | 209.9655 | -47.9267 | 209.17324 | -47.684492 | 226.050091 | -33.219593 | 314.62109256 | 13.3860264 | 293 | 56881.8273032407 | 2014-08-12 19:51:19 | 56882.7188773148 | 2014-08-13 17:15:11 | 509026010 | 41.3601 | 40 | 41.3601 | 41.3601 | 0 | 41.3601 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5.8509 | 5.8509 | 14.04 | 0 | PROCESSED | 57616.4947800926 | 2016-08-16 11:52:29 | 57270 | 2015-09-05 00:00:00 | 56902.1901273148 | 2014-09-02 04:33:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509026010/ | Quick Look | ![]() |
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727 | 3C 227 | 146.9365 | 7.4245 | 146.275614 | 7.656926 | 146.610705 | -5.546093 | 228.57888407 | 42.2858038 | 108.3139 | 56237.0794675926 | 2012-11-06 01:54:26 | 56239.0279513889 | 2012-11-08 00:40:15 | 707004010 | 82.5325 | 80 | 82.5405 | 82.5325 | 0 | 82.5405 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.4299 | 71.4299 | 168.3338 | 0 | PROCESSED | 57608.0036342593 | 2016-08-08 00:05:14 | 56631 | 2013-12-05 00:00:00 | 56264.6488773148 | 2012-12-03 15:34:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | FUMIE TAZAKI | JAP | 7 | AO7 | STUDY OF NUCLEAR STRUCTURE OF BLRGS WITH HIGH ACCRETION RATE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707004010/ | Quick Look | ![]() |
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728 | 2FGL J1502.1+5548 | 225.5826 | 55.8575 | 225.235279 | 56.052883 | 185.603435 | 66.74758 | 92.73148616 | 52.90392629 | 345.2903 | 56069.912974537 | 2012-05-22 21:54:41 | 56070.8342824074 | 2012-05-23 20:01:22 | 707008010 | 62.8733 | 60 | 62.8813 | 62.8813 | 0 | 62.8733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.167 | 56.167 | 79.5899 | 1 | PROCESSED | 57605.4999652778 | 2016-08-05 11:59:57 | 56449 | 2013-06-06 00:00:00 | 56083.096875 | 2012-06-05 02:19:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSUKE TAKAHASHI | JAP | 7 | AO7 | SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707008010/ | Quick Look | ![]() |
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729 | 2FGL J0157.2-5259 | 29.3567 | -53.0295 | 28.896901 | -53.272777 | 354.834799 | -58.248558 | 282.0695167 | -61.34394411 | 33.9769 | 56075.6946064815 | 2012-05-28 16:40:14 | 56076.2565162037 | 2012-05-29 06:09:23 | 707011010 | 32.0753 | 30 | 32.0753 | 32.0753 | 0 | 32.0753 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.7784 | 31.7784 | 48.5239 | 1 | PROCESSED | 57605.5386458333 | 2016-08-05 12:55:39 | 56527 | 2013-08-23 00:00:00 | 56161.0508449074 | 2012-08-22 01:13:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707011010/ | Quick Look | ![]() |
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730 | NGC1365 | 53.4038 | -36.1454 | 52.926467 | -36.312356 | 36.802809 | -53.044895 | 237.96455345 | -54.59601318 | 66.4692 | 56137.3445138889 | 2012-07-29 08:16:06 | 56138.1030208333 | 2012-07-30 02:28:21 | 707017040 | 31.3603 | 30 | 31.3683 | 31.3683 | 0 | 31.3603 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28.2314 | 28.2314 | 65.5279 | 2 | PROCESSED | 57606.7020717593 | 2016-08-06 16:50:59 | 56528 | 2013-08-24 00:00:00 | 56162.0367361111 | 2012-08-23 00:52:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017040/ | Quick Look | ![]() |
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731 | SWIFT J164449.3+1573 | 251.1623 | 57.5874 | 250.936922 | 57.677768 | 216.812116 | 77.507745 | 86.72267547 | 39.46447046 | 15.8437 | 56064.7296064815 | 2012-05-17 17:30:38 | 56066.0522106482 | 2012-05-19 01:15:11 | 707018010 | 80.8141 | 80 | 80.8221 | 80.8141 | 0 | 80.8221 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.3379 | 74.3379 | 114.2699 | 0 | PROCESSED | 57605.4610648148 | 2016-08-05 11:03:56 | 56442 | 2013-05-30 00:00:00 | 56076.0214351852 | 2012-05-29 00:30:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYUICHI USUI | JAP | 7 | AO7 | ONE YEAR AFTER THE TIDAL DISRUPTION OF SWIFT J164449.3+1573451 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707018010/ | Quick Look | ![]() |
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732 | Crab Nebula | 83.727 | 22.1071 | 82.97419 | 22.074866 | 84.190219 | -1.207347 | 184.52563634 | -5.6612791 | 84.9996 | 53615.0424652778 | 2005-09-02 01:01:09 | 53615.2432175926 | 2005-09-02 05:50:14 | 100015060 | 6.5256 | 5 | 6.5256 | 6.5256 | 6.5256 | 6.5256 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6.7599 | 6.7599 | 17.34 | 0 | PROCESSED | 57527.2534490741 | 2016-05-19 06:04:58 | 54247 | 2007-05-27 00:00:00 | 54109.1715393518 | 2007-01-09 04:07:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD boresight check with Crab | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015060/ | Quick Look | ![]() |
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733 | NGC 1667 | 72.1445 | -6.2644 | 71.533156 | -6.35119 | 69.717897 | -28.457954 | 203.99435404 | -30.10712566 | 81.9813 | 53964.3614814815 | 2006-08-17 08:40:32 | 53965.2536805556 | 2006-08-18 06:05:18 | 701006010 | 39.253 | 40 | 39.253 | 39.261 | 39.261 | 39.261 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.7281 | 35.7281 | 77.0759 | 0 | PROCESSED | 57535.2875578704 | 2016-05-27 06:54:05 | 54526 | 2008-03-01 00:00:00 | 54020.7803009259 | 2006-10-12 18:43:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701006010/ | Quick Look | ![]() |
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734 | NGC4418 | 186.7074 | -0.9383 | 186.066307 | -0.661629 | 186.526079 | 1.80107 | 290.03230216 | 61.31559989 | 292.8039 | 53929.4791898148 | 2006-07-13 11:30:02 | 53931.280775463 | 2006-07-15 06:44:19 | 701001010 | 68.3485 | 70 | 68.3485 | 68.3485 | 68.3485 | 68.3485 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57.1103 | 57.1103 | 155.634 | 1 | PROCESSED | 57534.9858564815 | 2016-05-26 23:39:38 | 54408 | 2007-11-04 00:00:00 | 53942.4601388889 | 2006-07-26 11:02:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701001010/ | Quick Look | ![]() |
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735 | PKS 0558-504 | 89.9338 | -50.4417 | 89.630316 | -50.442779 | 89.864771 | -73.883563 | 257.95388656 | -28.57696937 | 207.8266 | 54117.4686226852 | 2007-01-17 11:14:49 | 54118.1127777778 | 2007-01-18 02:42:24 | 701011010 | 20.6207 | 20 | 20.6207 | 20.6207 | 0 | 20.6207 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.914 | 18.914 | 55.6479 | 0 | PROCESSED | 57536.8527777778 | 2016-05-28 20:28:00 | 54735 | 2008-09-26 00:00:00 | 54133.0355787037 | 2007-02-02 00:51:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011010/ | Quick Look | ![]() |
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736 | PKS 0558-504 | 89.9338 | -50.4409 | 89.630307 | -50.441979 | 89.864775 | -73.882763 | 257.95298672 | -28.57684464 | 209.1054 | 54118.6998032407 | 2007-01-18 16:47:43 | 54119.2654976852 | 2007-01-19 06:22:19 | 701011020 | 18.8753 | 20 | 18.8753 | 18.8753 | 0 | 18.8753 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.0497 | 18.0497 | 48.87 | 1 | PROCESSED | 57536.8739814815 | 2016-05-28 20:58:32 | 54735 | 2008-09-26 00:00:00 | 54133.3967361111 | 2007-02-02 09:31:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011020/ | Quick Look | ![]() |
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737 | NGC 5273 | 205.535 | 35.6446 | 204.979886 | 35.89633 | 186.960858 | 42.373618 | 74.3162813 | 76.25118024 | 278.9999 | 56489.1929976852 | 2013-07-16 04:37:55 | 56491.0543171296 | 2013-07-18 01:18:13 | 708001010 | 81.7709 | 80 | 81.7709 | 81.7949 | 0 | 81.7789 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.0981 | 79.0981 | 160.8018 | 3 | PROCESSED | 57612.0002546296 | 2016-08-12 00:00:22 | 56890 | 2014-08-21 00:00:00 | 56523.6749537037 | 2013-08-19 16:11:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080015 | 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. 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. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 8 | AO8 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708001010/ | Quick Look | ![]() |
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738 | NGC 3516 | 166.6694 | 72.5588 | 165.816381 | 72.829135 | 123.37012 | 57.971175 | 133.25250212 | 42.40656753 | 323.9054 | 56754.7044675926 | 2014-04-07 16:54:26 | 56755.5002777778 | 2014-04-08 12:00:24 | 708006080 | 51.539 | 50 | 51.539 | 51.547 | 0 | 51.555 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0472 | 46.0472 | 68.752 | 1 | PROCESSED | 57614.1922800926 | 2016-08-14 04:36:53 | 56383 | 2013-04-01 00:00:00 | 56817.774849537 | 2014-06-09 18:35:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006080/ | Quick Look | ![]() |
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739 | KAZ 102 | 270.6661 | 67.6374 | 270.701804 | 67.634057 | 77.059679 | 88.893324 | 97.62313354 | 29.55178422 | 2.066 | 53895.6833101852 | 2006-06-09 16:23:58 | 53896.5343055556 | 2006-06-10 12:49:24 | 701012010 | 41.454 | 40 | 41.454 | 41.462 | 41.47 | 41.47 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40.9507 | 40.9507 | 73.5199 | 2 | PROCESSED | 57534.6269328704 | 2016-05-26 15:02:47 | 54394 | 2007-10-21 00:00:00 | 53928.2501157407 | 2006-07-12 06:00:10 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA ISHISAKI | JAP | 1 | AO1 | WHAT IS THE PHYSICAL NATURE OF KAZ 102: AN ENIGMATIC X-RAY HARD RADIO QUIET QSO? | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701012010/ | Quick Look | ![]() |
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740 | 1ES1218+304 | 185.3064 | 30.1169 | 184.679878 | 30.394195 | 171.661841 | 29.481192 | 186.88913956 | 82.72978014 | 298.9428 | 53874.8006365741 | 2006-05-19 19:12:55 | 53876.706412037 | 2006-05-21 16:57:14 | 701025010 | 79.8692 | 80 | 79.8852 | 79.8692 | 79.8852 | 79.8772 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.5118 | 70.5118 | 164.6379 | 2 | PROCESSED | 57534.4292013889 | 2016-05-26 10:18:03 | 54398 | 2007-10-25 00:00:00 | 53927.8564930556 | 2006-07-11 20:33:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701025010/ | Quick Look | ![]() |
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741 | 1ES1426+428 | 217.0716 | 42.6249 | 216.585066 | 42.847682 | 193.182318 | 52.911489 | 77.44668506 | 64.96380656 | 316.1862 | 53902.7388310185 | 2006-06-16 17:43:55 | 53904.2225 | 2006-06-18 05:20:24 | 701026010 | 60.9149 | 60 | 60.9149 | 60.9149 | 60.9149 | 60.9149 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.0911 | 54.0911 | 128.16 | 1 | PROCESSED | 57534.6747800926 | 2016-05-26 16:11:41 | 54400 | 2007-10-27 00:00:00 | 53928.3009143518 | 2006-07-12 07:13:19 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701026010/ | Quick Look | ![]() |
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742 | MRK 501 | 253.4 | 39.7089 | 252.98087 | 39.789378 | 242.4893 | 61.571247 | 63.52834502 | 38.90621529 | 316.9908 | 53934.7872569444 | 2006-07-18 18:53:39 | 53935.7272916667 | 2006-07-19 17:27:18 | 701027010 | 42.4271 | 40 | 42.4389 | 42.4389 | 42.4271 | 42.4351 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.9711 | 39.9711 | 81.2099 | 0 | PROCESSED | 57534.9978587963 | 2016-05-26 23:56:55 | 54408 | 2007-11-04 00:00:00 | 53971.6784259259 | 2006-08-24 16:16:56 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701027010/ | Quick Look | ![]() |
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743 | NGC 2788A | 135.6754 | -68.2181 | 135.519975 | -68.019146 | 206.346244 | -72.761691 | 284.17134554 | -14.14937336 | 282.2863 | 57157.0478819444 | 2015-05-15 01:08:57 | 57158.2230324074 | 2015-05-16 05:21:10 | 710007010 | 42.2339 | 40 | 42.2339 | 42.2339 | 0 | 42.2339 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6656828704 | 2016-08-18 15:58:35 | 57591 | 2016-07-22 00:00:00 | 57224.447650463 | 2015-07-21 10:44:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100009 | 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 four Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. Since their spectra below 10 keV are likely reflection dominated, joint analysis of Suzaku/XIS and Swift/BAT can constrain the absorption and intrinsic luminosity without being much affected by time variability. 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 survey. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSHIHIRO UEDA | JAP | 10 | AO10 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710007010/ | Quick Look | ![]() |
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744 | NGC 4395 | 186.4111 | 33.4884 | 185.79012 | 33.76517 | 170.810459 | 32.904029 | 162.54122992 | 81.55189464 | 303.1476 | 54253.6042013889 | 2007-06-02 14:30:03 | 54256.2981944444 | 2007-06-05 07:09:24 | 702001010 | 101.5075 | 100 | 101.5155 | 101.5075 | 0 | 101.5155 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101.9292 | 101.9292 | 232.7198 | 4 | PROCESSED | 57538.8900694444 | 2016-05-30 21:21:42 | 54745 | 2008-10-06 00:00:00 | 54263.5438194445 | 2007-06-12 13:03:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUO TANAKA | JAP | 2 | AO2 | UNCOVERING THE IMBH ACTIVE NUCLEUS IN THE DWARF SEYFERT GALAXY NGC 4395 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702001010/ | Quick Look | ![]() |
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745 | M33 X8 | 23.4834 | 30.5892 | 22.778431 | 30.333215 | 33.223542 | 19.296261 | 133.64723816 | -31.39681198 | 258.5185 | 55207.0743865741 | 2010-01-11 01:47:07 | 55209.5626157407 | 2010-01-13 13:30:10 | 704016010 | 106.1036 | 100 | 106.1036 | 106.1061 | 0 | 106.1061 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.1053 | 6.1053 | 214.9577 | 1 | PROCESSED | 57550.3046412037 | 2016-06-11 07:18:41 | 55587 | 2011-01-26 00:00:00 | 55218.6414930556 | 2010-01-22 15:23:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 4 | AO4 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704016010/ | Quick Look | ![]() |
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746 | HCG62_W | 192.9973 | -9.0837 | 192.347013 | -8.812069 | 195.480643 | -3.238715 | 303.16227701 | 53.78780217 | 292.9782 | 55405.1509953704 | 2010-07-28 03:37:26 | 55406.9773611111 | 2010-07-29 23:27:24 | 805031010 | 66.947 | 60 | 66.955 | 66.955 | 0 | 66.947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.9972 | 52.9972 | 157.7758 | 1 | PROCESSED | 57552.8094675926 | 2016-06-13 19:25:38 | 55808 | 2011-09-04 00:00:00 | 55441.3150925926 | 2010-09-02 07:33:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050034 | We propose offset observations of groups of galaxies to study the metal distributions up to ~0.5 times of the virial radius. Metal mass to galaxy light ratios (MLRs) for groups are much smaller than those for clusters of galaxies. In order to solve the problem which is important to understand the chemical history of the universe, we need much information of the metal abundance and distributions to the outer region of the groups. Suzaku firstly enable us to measure the metals to such an outer region of groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 5 | AO5 | SEARCH FOR THE METAL DISTRIBUTIONS OF GROUPS OF GALAXIES TO 0.5 R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805031010/ | Quick Look | ![]() |
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747 | OJ 287 QUIESCENT | 133.689 | 20.0482 | 132.974133 | 20.239223 | 130.506959 | 2.538802 | 206.87650629 | 35.78772906 | 283.9125 | 54200.8243055556 | 2007-04-10 19:47:00 | 54203.4654976852 | 2007-04-13 11:10:19 | 702009010 | 102.8441 | 100 | 102.8441 | 102.8441 | 0 | 102.8441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.6244 | 93.6244 | 228.1859 | 12 | PROCESSED | 57538.2031018518 | 2016-05-30 04:52:28 | 54744 | 2008-10-05 00:00:00 | 54210.7303587963 | 2007-04-20 17:31:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 2 | AO2-TOO | MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702009010/ | Quick Look | ![]() |
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748 | SWIFT J0714.2+3518 | 108.5168 | 35.2792 | 107.688726 | 35.365694 | 105.421903 | 12.82422 | 182.49455345 | 19.57130625 | 283.6115 | 57116.9939814815 | 2015-04-04 23:51:20 | 57118.9043634259 | 2015-04-06 21:42:17 | 709007010 | 79.2471 | 80 | 79.2471 | 79.2471 | 0 | 79.2471 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9309027778 | 2016-08-17 22:20:30 | 57565 | 2016-06-26 00:00:00 | 57198.4724074074 | 2015-06-25 11:20:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090019 | 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 two Compton thick AGN candidates in the 70 month 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 | YOSHIHIRO UEDA | JAP | 9 | AO9 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709007010/ | Quick Look | ![]() |
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749 | KUV 00311-1938 | 8.3907 | -19.361 | 7.763877 | -19.636683 | 359.653009 | -21.03622 | 94.15504043 | -81.21658968 | 60.8243 | 56821.2581481482 | 2014-06-13 06:11:44 | 56822.2384606482 | 2014-06-14 05:43:23 | 709013010 | 41.8926 | 40 | 41.8926 | 41.9006 | 0 | 41.9006 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.9853 | 35.9853 | 84.6858 | 0 | PROCESSED | 57615.2401851852 | 2016-08-15 05:45:52 | 57200 | 2015-06-27 00:00:00 | 56833.588900463 | 2014-06-25 14:08:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090088 | Extreme HBL objects are BL Lac objects characterized by their hard TeV gamma-ray spectra, by which the sources are considered as excellent targets to study secondary cascade gamma-ray emission induced by very-high-energy photons or protons from the sources. We propose Suzaku observations of 1ES 0347-121 and KUV 00311-1938 for 60 ks and 40 ks, respectively. The observations can reveal detailed spectral structure around synchrotron peak in the extreme HBLs, which are essential to derive physical parameters such as electron spectrum, magnetic filed strength in the jet. The results will help understating gamma-ray components of both intrinsic jet emission and the secondary cascade emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MASAAKI HAYASHIDA | JAP | 9 | AO9 | SUZAKU OBSERVATIONS OF EXTREME HIGH-FREQUENCY PEAKED BL LAC OBJECTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709013010/ | Quick Look | ![]() |
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750 | NGC 4593 | 189.9133 | -5.3412 | 189.268409 | -5.066685 | 191.201213 | -0.986393 | 297.4806457 | 57.40576161 | 111.8999 | 57017.6624421296 | 2014-12-26 15:53:55 | 57021.7640740741 | 2014-12-30 18:20:16 | 709014040 | 130.3584 | 30 | 130.3904 | 130.3584 | 0 | 130.3824 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5950810185 | 2016-08-17 14:16:55 | 57415 | 2016-01-28 00:00:00 | 57049.4551851852 | 2015-01-27 10:55:28 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014040/ | Quick Look | ![]() |
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751 | A2104N | 235.0318 | -3.1802 | 234.37876 | -3.019346 | 233.471257 | 15.936264 | 2.94593816 | 39.29281704 | 117.689 | 54119.2779166667 | 2007-01-19 06:40:12 | 54119.7522337963 | 2007-01-19 18:03:13 | 801002010 | 18.8424 | 20 | 18.8424 | 18.8424 | 0 | 18.8424 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.6448 | 13.6448 | 40.9779 | 1 | PROCESSED | 57536.8705439815 | 2016-05-28 20:53:35 | 54735 | 2008-09-26 00:00:00 | 54133.3893518518 | 2007-02-02 09:20:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801002010/ | Quick Look | ![]() |
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752 | IGR J12391-1612 | 189.807 | -16.1292 | 189.153193 | -15.854578 | 195.389743 | -10.939243 | 298.65896251 | 46.64122293 | 122.9437 | 54818.9051273148 | 2008-12-18 21:43:23 | 54822.2910648148 | 2008-12-22 06:59:08 | 703007010 | 130.274 | 120 | 130.274 | 130.274 | 0 | 130.274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 111.0893 | 111.0893 | 292.4838 | 2 | PROCESSED | 57545.0634953704 | 2016-06-06 01:31:26 | 55206 | 2010-01-10 00:00:00 | 54840.5288425926 | 2009-01-09 12:41:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 3 | AO3 | X-RAY OBSERVATION OF A COMPTON THICK CANDIDATE, IGR J12391-1612 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703007010/ | Quick Look | ![]() |
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753 | NGC 1313 | 49.5565 | -66.5364 | 49.405687 | -66.717354 | 341.391654 | -74.190914 | 283.40259478 | -44.62074971 | 201.281 | 54805.9606828704 | 2008-12-05 23:03:23 | 54808.2814699074 | 2008-12-08 06:45:19 | 703010010 | 91.4661 | 100 | 91.4981 | 91.4661 | 0 | 91.4981 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.7593 | 78.7593 | 200.4937 | 1 | PROCESSED | 57544.7004861111 | 2016-06-05 16:48:42 | 55188 | 2009-12-23 00:00:00 | 54822.6519328704 | 2008-12-22 15:38:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN OHSUGA | JAP | 3 | AO3 | EXPLORING FE K-LINE ABSORPTION FEATURES FROM AN ULTRALUMINOUS X-RAY SOURCE, NGC 1313 X1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703010010/ | Quick Look | ![]() |
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754 | NGC 454 | 18.511 | -55.3853 | 17.99732 | -55.649778 | 343.260726 | -55.777074 | 296.21074431 | -61.44696878 | 18.3891 | 54950.2291782407 | 2009-04-29 05:30:01 | 54953.4023032407 | 2009-05-02 09:39:19 | 704009010 | 128.9562 | 120 | 128.9562 | 128.9562 | 0 | 128.9562 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.5969 | 114.5969 | 274.1296 | 0 | PROCESSED | 57546.5592361111 | 2016-06-07 13:25:18 | 55342 | 2010-05-26 00:00:00 | 54973.5148842593 | 2009-05-22 12:21:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 4 | AO4 | X-RAY SPECTRAL VARIABILITY OF THE HARD X-RAY BRIGHTEST LOW-MASS SEYFERT 2 NGC 454 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704009010/ | Quick Look | ![]() |
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755 | NGC 507 | 20.9105 | 33.2598 | 20.206045 | 32.999169 | 32.202982 | 22.611804 | 130.6367604 | -29.12969375 | 54.0771 | 53944.6189351852 | 2006-07-28 14:51:16 | 53946.5544444444 | 2006-07-30 13:18:24 | 801017010 | 79.5013 | 80 | 79.5253 | 79.5013 | 79.5253 | 79.5253 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 80.2867 | 80.2867 | 167.17 | 2 | PROCESSED | 57535.1047222222 | 2016-05-27 02:30:48 | 54394 | 2007-10-21 00:00:00 | 53955.7736689815 | 2006-08-08 18:34:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOSUKE SATO | JAP | 1 | AO1 | CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801017010/ | Quick Look | ![]() |
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756 | MRK 18 | 135.5092 | 60.0703 | 134.525486 | 60.267174 | 118.140543 | 40.9961 | 155.86471567 | 39.40052697 | 266.8203 | 55330.5025810185 | 2010-05-14 12:03:43 | 55331.3772106482 | 2010-05-15 09:03:11 | 705001010 | 37.9667 | 40 | 37.9747 | 37.9747 | 0 | 37.9667 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.667 | 34.667 | 75.5539 | 1 | PROCESSED | 57551.5224074074 | 2016-06-12 12:32:16 | 55769 | 2011-07-27 00:00:00 | 55403.0749768518 | 2010-07-26 01:47:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 5 | AO5 | THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705001010/ | Quick Look | ![]() |
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757 | OPHIUCHUS CLUSTER 2 | 257.7375 | -23.3864 | 256.979428 | -23.325463 | 258.749053 | -0.422802 | 0.3572282 | 9.54416529 | 94.9391 | 54181.1423726852 | 2007-03-22 03:25:01 | 54181.825162037 | 2007-03-22 19:48:14 | 801023010 | 24.6782 | 15 | 24.7022 | 24.6942 | 0 | 24.6782 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.2781 | 21.2781 | 58.9879 | 1 | PROCESSED | 57537.9744097222 | 2016-05-29 23:23:09 | 54736 | 2008-09-27 00:00:00 | 54209.5433217593 | 2007-04-19 13:02:23 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801023010/ | Quick Look | ![]() |
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758 | A2319CENTER | 290.3341 | 43.878 | 289.944223 | 43.782148 | 306.012819 | 64.798086 | 75.63759851 | 13.45022652 | 251.6652 | 54035.9326041667 | 2006-10-27 22:22:57 | 54038.1466898148 | 2006-10-30 03:31:14 | 801040010 | 99.5332 | 100 | 99.5492 | 99.5412 | 99.5332 | 99.5492 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.9548 | 93.9548 | 191.268 | 2 | PROCESSED | 57535.9905555556 | 2016-05-27 23:46:24 | 54735 | 2008-09-26 00:00:00 | 54063.5741666667 | 2006-11-24 13:46:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOKAZU TAKIZAWA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE A2319 CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801040010/ | Quick Look | ![]() |
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759 | PERSEUS CL OFFSET | 50.5735 | 41.8053 | 49.742345 | 41.626976 | 59.178685 | 22.492416 | 150.80595618 | -12.75877318 | 65.9956 | 53982.1426736111 | 2006-09-04 03:25:27 | 53982.4377893518 | 2006-09-04 10:30:25 | 801049040 | 10.4206 | 30 | 10.4206 | 10.4206 | 10.4206 | 10.4206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7.5402 | 7.5402 | 25.4679 | 1 | PROCESSED | 57535.4390856482 | 2016-05-27 10:32:17 | 54526 | 2008-03-01 00:00:00 | 54021.0033680556 | 2006-10-13 00:04:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049040/ | Quick Look | ![]() |
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760 | NGC3923 | 177.7599 | -28.8047 | 177.126048 | -28.526534 | 190.367331 | -27.106442 | 287.27787622 | 32.22445477 | 293.1988 | 53899.8430671296 | 2006-06-13 20:14:01 | 53902.7293287037 | 2006-06-16 17:30:14 | 801054010 | 115.82 | 120 | 115.828 | 115.82 | 115.828 | 115.828 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 107.7313 | 107.7313 | 249.3528 | 3 | PROCESSED | 57534.7187731482 | 2016-05-26 17:15:02 | 54394 | 2007-10-21 00:00:00 | 53927.2880902778 | 2006-07-11 06:54:51 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 1 | AO1 | ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801054010/ | Quick Look | ![]() |
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761 | CENTAURUS_A | 201.3411 | -43.072 | 200.607667 | -42.811983 | 217.145584 | -31.383496 | 309.48969514 | 19.36734145 | 290.0008 | 55032.3718634259 | 2009-07-20 08:55:29 | 55033.7683333333 | 2009-07-21 18:26:24 | 704018010 | 62.4328 | 50 | 62.4328 | 62.6888 | 0 | 62.7076 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 55.45 | 55.45 | 120.6499 | 3 | PROCESSED | 57547.9397569444 | 2016-06-08 22:33:15 | 55415 | 2010-08-07 00:00:00 | 55048.3403356482 | 2009-08-05 08:10:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018010/ | Quick Look | ![]() |
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762 | A1631_N | 193.3404 | -15.1138 | 192.682958 | -14.842526 | 198.153884 | -8.661195 | 303.62251983 | 47.75536925 | 113.0007 | 56303.6628356482 | 2013-01-11 15:54:29 | 56304.4904861111 | 2013-01-12 11:46:18 | 807003010 | 28.0433 | 20 | 28.183 | 28.183 | 0 | 28.0433 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 25.3059 | 25.3059 | 71.48 | 1 | PROCESSED | 57608.4621296296 | 2016-08-08 11:05:28 | 56703 | 2014-02-15 00:00:00 | 56337.5115393518 | 2013-02-14 12:16:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807003010/ | Quick Look | ![]() |
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763 | IC 342 X2 | 56.516 | 68.1498 | 55.302778 | 67.99381 | 72.573568 | 46.727351 | 138.08335694 | 10.57829767 | 91.9969 | 55415.9786689815 | 2010-08-07 23:29:17 | 55417.3765625 | 2010-08-09 09:02:15 | 705009010 | 74.379 | 80 | 74.379 | 74.379 | 0 | 74.379 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.1316 | 64.1316 | 120.7679 | 0 | PROCESSED | 57552.9205671296 | 2016-06-13 22:05:37 | 55794 | 2011-08-21 00:00:00 | 55428.1624537037 | 2010-08-20 03:53:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 5 | AO5 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705009010/ | Quick Look | ![]() |
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764 | LEDA 84274 | 220.5853 | 66.0952 | 220.354238 | 66.306919 | 158.410677 | 70.66779 | 106.75984756 | 47.40039166 | 359.2838 | 55331.3858333333 | 2010-05-15 09:15:36 | 55332.0542824074 | 2010-05-16 01:18:10 | 705023010 | 49.465 | 50 | 49.465 | 49.465 | 0 | 49.465 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8385 | 40.8385 | 57.7519 | 1 | PROCESSED | 57551.5334143518 | 2016-06-12 12:48:07 | 55769 | 2011-07-27 00:00:00 | 55403.1228125 | 2010-07-26 02:56:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINKI OYABU | JAP | 5 | AO5 | SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705023010/ | Quick Look | ![]() |
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765 | RXJ1713-3946 | 258.5527 | -40.0289 | 257.68331 | -39.971559 | 260.849002 | -16.950052 | 347.19063141 | -0.73133412 | 268.0015 | 53997.9147569444 | 2006-09-19 21:57:15 | 53998.4425925926 | 2006-09-20 10:37:20 | 501070010 | 20.7442 | 20 | 20.7442 | 20.7522 | 20.7522 | 20.7522 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 22.0266 | 22.0266 | 45.5959 | 1 | PROCESSED | 57535.6347685185 | 2016-05-27 15:14:04 | 54526 | 2008-03-01 00:00:00 | 54021.1763541667 | 2006-10-13 04:13:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501070010/ | Quick Look | ![]() |
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766 | A963S | 154.2641 | 38.9388 | 153.524075 | 39.18875 | 141.373211 | 26.246798 | 182.75442962 | 55.85527134 | 107.1093 | 54432.4435300926 | 2007-11-28 10:38:41 | 54432.9584953704 | 2007-11-28 23:00:14 | 802012010 | 27.7172 | 25 | 27.7252 | 27.7252 | 0 | 27.7172 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.6546 | 25.6546 | 44.492 | 1 | PROCESSED | 57540.6110185185 | 2016-06-01 14:39:52 | 54811 | 2008-12-11 00:00:00 | 54440.9716319444 | 2007-12-06 23:19:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802012010/ | Quick Look | ![]() |
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767 | ABELL 2744 | 3.5397 | -30.3446 | 2.908232 | -30.62262 | 349.980606 | -28.995561 | 9.24871336 | -81.22170813 | 53.4742 | 54239.5874652778 | 2007-05-19 14:05:57 | 54243.7709953704 | 2007-05-23 18:30:14 | 802033010 | 153.2332 | 150 | 153.2412 | 153.2412 | 0 | 153.2332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 133.8631 | 133.8631 | 361.4398 | 2 | PROCESSED | 57538.8170138889 | 2016-05-30 19:36:30 | 54745 | 2008-10-06 00:00:00 | 54248.6974074074 | 2007-05-28 16:44:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUHIRO NAKAZAWA | JAP | 2 | AO2 | HARD X-RAY VIEW OF A DISTANT RADIO-HALO CLUSTER ABELL2744 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802033010/ | Quick Look | ![]() |
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768 | NGC4636_GALACTIC_1 | 192.513 | 5.4558 | 191.878088 | 5.727905 | 189.348778 | 9.962987 | 301.99802564 | 68.32503562 | 300.0459 | 54268.8414930556 | 2007-06-17 20:11:45 | 54269.9307175926 | 2007-06-18 22:20:14 | 802039010 | 41.4997 | 30 | 41.5157 | 41.5077 | 0 | 41.4997 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3371 | 34.3371 | 94.0479 | 0 | PROCESSED | 57553.0490393518 | 2016-06-14 01:10:37 | 54695 | 2008-08-17 00:00:00 | 54319.4765740741 | 2007-08-07 11:26:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802039010/ | Quick Look | ![]() |
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769 | FORNAX_GALACTIC_2 | 49.9904 | -32.0719 | 49.483389 | -32.25188 | 35.195492 | -48.193254 | 230.76086762 | -57.49880076 | 52.7651 | 54280.3368518518 | 2007-06-29 08:05:04 | 54280.9897453704 | 2007-06-29 23:45:14 | 802040010 | 21.0746 | 20 | 21.0826 | 21.0826 | 0 | 21.0746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.131 | 20.131 | 56.3939 | 1 | PROCESSED | 57539.0651967593 | 2016-05-31 01:33:53 | 54696 | 2008-08-18 00:00:00 | 54322.4474537037 | 2007-08-10 10:44:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802040010/ | Quick Look | ![]() |
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770 | N1550_OFFSET | 65.2479 | 2.4086 | 64.596961 | 2.290593 | 63.774789 | -18.807983 | 191.20173857 | -31.56876902 | 90.0005 | 54693.1139351852 | 2008-08-15 02:44:04 | 54694.185 | 2008-08-16 04:26:24 | 803018010 | 41.1447 | 40 | 41.1447 | 41.1447 | 0 | 41.1447 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29.9469 | 29.9469 | 92.508 | 0 | PROCESSED | 57543.3286226852 | 2016-06-04 07:53:13 | 55079 | 2009-09-05 00:00:00 | 54711.3163310185 | 2008-09-02 07:35:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030070 | We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 3 | AO3 | OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803018010/ | Quick Look | ![]() |
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771 | SHAPLEY OFFSET | 204.9135 | -29.8943 | 204.20662 | -29.641044 | 214.142611 | -18.17761 | 315.23466303 | 31.82297967 | 289.7009 | 54665.2119907407 | 2008-07-18 05:05:16 | 54666.4244675926 | 2008-07-19 10:11:14 | 803021010 | 47.2435 | 40 | 47.2435 | 47.2435 | 0 | 47.2435 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.3578 | 38.3578 | 104.7418 | 0 | PROCESSED | 57543.0903356482 | 2016-06-04 02:10:05 | 55049 | 2009-08-06 00:00:00 | 54682.1908680556 | 2008-08-04 04:34:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030089 | We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 3 | AO3 | SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803021010/ | Quick Look | ![]() |
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772 | 1ES 1927+654 | 291.8157 | 65.5862 | 291.743016 | 65.482913 | 3.782751 | 81.150517 | 97.0030083 | 20.97400385 | 83.4311 | 55667.8280092593 | 2011-04-16 19:52:20 | 55669.2425115741 | 2011-04-18 05:49:13 | 706006010 | 71.8889 | 100 | 71.9129 | 71.8889 | 0 | 71.9129 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.6647 | 79.6647 | 122.1919 | 0 | PROCESSED | 57601.5407986111 | 2016-08-01 12:58:45 | 56059 | 2012-05-12 00:00:00 | 55691.2683912037 | 2011-05-10 06:26:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | LUIGI GALLO | JAP | 6 | AO6 | REVEALING THE NATURE OF AN X-RAY ABSORBED SEYFERT 2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706006010/ | Quick Look | ![]() |
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773 | PG 1626+554 | 247.0224 | 55.3701 | 246.753118 | 55.479335 | 214.524979 | 74.372261 | 84.50112094 | 42.16849703 | 200.5289 | 55876.6090046296 | 2011-11-11 14:36:58 | 55877.9341550926 | 2011-11-12 22:25:11 | 706017010 | 60.8488 | 60 | 60.8488 | 60.8488 | 0 | 60.8488 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.1328 | 56.1328 | 114.4639 | 2 | PROCESSED | 57603.7696412037 | 2016-08-03 18:28:17 | 56256 | 2012-11-25 00:00:00 | 55890.6981828704 | 2011-11-25 16:45:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROAKI SAMESHIMA | JAP | 6 | AO6 | X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706017010/ | Quick Look | ![]() |
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774 | TRIANGULUM_AUSTRALIS | 249.6225 | -64.3477 | 248.441517 | -64.24803 | 258.335963 | -41.727543 | 324.61952374 | -11.529112 | 306.6841 | 54750.3809143518 | 2008-10-11 09:08:31 | 54752.6453587963 | 2008-10-13 15:29:19 | 803028010 | 86.0101 | 80 | 86.0421 | 86.0101 | 0 | 86.0481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.9675 | 76.9675 | 195.6378 | 1 | PROCESSED | 57544.1744560185 | 2016-06-05 04:11:13 | 55148 | 2009-11-13 00:00:00 | 54780.7199768518 | 2008-11-10 17:16:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030101 | We propose an 80 ks pointed observation of one of the brightest near-by hot and merging galaxy cluster, Triangulum Australis. Recent Suzaku wide-band spectroscopy reveals a very hot (kT >20 keV) thermal component in several merging clusters (RXJ1347, Abell 3667 and so on). On the other hand, relaxed cluster (such as Abell 1060 and Centaurus) show no evidence of such component. These results suggests that the very-hot component is the key aspects of merging cluster. Triangulum Australis is a bright (f ~ 1e-10 cgs), mildly hot (kT ~ 9 keV) and relatively compact (size ~20x20 arcmin2) shaped cluster. ASCA detected a hot region in the center and to the east (Markevitch et al. 1996). Combination of these characteristics makes this cluster the best candidate for our research. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SHO OKUYAMA | JAP | 3 | AO3 | SEARCH FOR VERY-HIGH TEMPERATURE COMPONENT IN A NEAR-BY CLUSTER, TRIANGULUM AUSTRALIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803028010/ | Quick Look | ![]() |
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775 | A2029_3 | 227.6311 | 5.4874 | 227.010378 | 5.676114 | 223.4982 | 22.349991 | 6.05366388 | 50.47243927 | 112.9537 | 55224.9801041667 | 2010-01-28 23:31:21 | 55225.6140509259 | 2010-01-29 14:44:14 | 804024030 | 17.9095 | 22 | 17.9175 | 17.9255 | 0 | 17.9095 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.9268 | 8.9268 | 54.7659 | 0 | PROCESSED | 57550.4118865741 | 2016-06-11 09:53:07 | 55637 | 2011-03-17 00:00:00 | 55270.9888425926 | 2010-03-15 23:43:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024030/ | Quick Look | ![]() |
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776 | FILAMENT OF GALAXIES | 238.8797 | 27.1312 | 238.361126 | 27.276131 | 228.364873 | 46.172986 | 43.89595297 | 49.28386381 | 298.9982 | 55406.9857060185 | 2010-07-29 23:39:25 | 55408.8592939815 | 2010-07-31 20:37:23 | 805029010 | 73.9387 | 80 | 73.9501 | 73.9447 | 0 | 73.9387 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66.4045 | 66.4045 | 161.8557 | 1 | PROCESSED | 57552.8140972222 | 2016-06-13 19:32:18 | 55791 | 2011-08-18 00:00:00 | 55418.4520717593 | 2010-08-10 10:50:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050032 | Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAJIME KAWAHARA | JAP | 5 | AO5 | SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805029010/ | Quick Look | ![]() |
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777 | ESO 565-G019 | 143.6802 | -21.9346 | 143.106087 | -21.711094 | 154.563677 | -34.141633 | 253.87283017 | 21.67453181 | 298.0016 | 56067.8709259259 | 2012-05-20 20:54:08 | 56069.9022222222 | 2012-05-22 21:39:12 | 707013010 | 78.9239 | 80 | 78.9239 | 78.9319 | 0 | 78.9319 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.1211 | 71.1211 | 175.4878 | 2 | PROCESSED | 57605.5328935185 | 2016-08-05 12:47:22 | 56448 | 2013-06-05 00:00:00 | 56079.3396643518 | 2012-06-01 08:09:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | POSHAK GANDHI | JAP | 7 | AO7 | WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707013010/ | Quick Look | ![]() |
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778 | A478 OFFSET D | 63.1009 | 10.3754 | 62.415271 | 10.247963 | 63.081843 | -10.587617 | 182.33525373 | -28.5396849 | 259.0002 | 55612.7107986111 | 2011-02-20 17:03:33 | 55613.7362731482 | 2011-02-21 17:40:14 | 805004010 | 47.1066 | 45 | 47.1066 | 47.1066 | 0 | 47.1066 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 42.161 | 42.161 | 88.5959 | 1 | PROCESSED | 57601.0027314815 | 2016-08-01 00:03:56 | 56018 | 2012-04-01 00:00:00 | 55649.2441203704 | 2011-03-29 05:51:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | ANDREW FABIAN | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805004010/ | Quick Look | ![]() |
779 | A222/223 BRIDGE | 24.4438 | -12.9141 | 23.829522 | -13.168194 | 17.57702 | -21.440022 | 162.54430913 | -72.12239011 | 224.9995 | 55555.161099537 | 2010-12-25 03:51:59 | 55557.4654861111 | 2010-12-27 11:10:18 | 805035010 | 101.2149 | 100 | 101.2843 | 101.2149 | 0 | 101.2843 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.9171 | 88.9171 | 199.0699 | 4 | PROCESSED | 57554.5537268518 | 2016-06-15 13:17:22 | 55961 | 2012-02-04 00:00:00 | 55595.1387847222 | 2011-02-03 03:19:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050035 | We propose to observe the unusual X-ray bridge connecting the two clusters of galaxies Abell 222 and Abell 223 (z=0.21). XMM observation showed the temperature to be 0.9 keV, interpreted as due to WHIM. Suzaku will observe the temperature distribution over the bridge region, which will tell us the origin of the bridge to be either WHIM or merger onset. Merger process should indicate a characteristic temperature increase. Redshifted oxygen lines, if detected, will be the clear evidence of WHIM. Joint study with weak lensing analysis will show us spatial offset of the dark matter against baryons, helping us to constrain dark matter properties. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAORI HENMI | JAP | 5 | AO5 | ORIGIN OF THE X-RAY BRIDGE CONNECTING THE CLUSTERS OF GALAXIES ABELL 222 AND ABELL 223 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805035010/ | Quick Look | ![]() |
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780 | ABELL1835 OFFSET3 | 210.0673 | 2.8311 | 209.433725 | 3.072798 | 206.943622 | 14.143739 | 340.00426802 | 60.64916276 | 306.4895 | 55385.4673611111 | 2010-07-08 11:13:00 | 55386.9855555556 | 2010-07-09 23:39:12 | 805039010 | 53.6971 | 50 | 53.7201 | 53.7131 | 0 | 53.6971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.8377 | 44.8377 | 131.1598 | 3 | PROCESSED | 57552.5941087963 | 2016-06-13 14:15:31 | 55779 | 2011-08-06 00:00:00 | 55411.2395717593 | 2010-08-03 05:44:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NOBUHIRO OKABE | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805039010/ | Quick Look | ![]() |
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781 | ABELL1835 OFFSET4 | 210.2225 | 3.0556 | 209.589504 | 3.296921 | 207.010904 | 14.408613 | 340.51868842 | 60.75430015 | 304.9986 | 55390.9913194444 | 2010-07-13 23:47:30 | 55392.4001736111 | 2010-07-15 09:36:15 | 805040010 | 48.8185 | 50 | 48.8265 | 48.8265 | 0 | 48.8185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9631 | 43.9631 | 121.6839 | 4 | PROCESSED | 57552.6731828704 | 2016-06-13 16:09:23 | 55793 | 2011-08-20 00:00:00 | 55427.1333796296 | 2010-08-19 03:12:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NOBUHIRO OKABE | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805040010/ | Quick Look | ![]() |
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782 | ESO 119-G008 | 72.2547 | -57.6544 | 72.033322 | -57.73981 | 38.878903 | -77.915205 | 266.66680471 | -38.87724734 | 324.43 | 56411.0111458333 | 2013-04-29 00:16:03 | 56413.2355787037 | 2013-05-01 05:39:14 | 708004010 | 100.5873 | 100 | 100.5953 | 100.5953 | 0 | 100.5873 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.7614 | 103.7614 | 192.1719 | 3 | PROCESSED | 57611.2384375 | 2016-08-11 05:43:21 | 56837 | 2014-06-29 00:00:00 | 56475.7648611111 | 2013-07-02 18:21:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080027 | At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | POSHAK GANDHI | JAP | 8 | AO8 | THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708004010/ | Quick Look | ![]() |
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783 | NGC 3516 | 166.7239 | 72.5839 | 165.871383 | 72.854298 | 123.356587 | 58.000243 | 133.21571384 | 42.39397937 | 129.7498 | 56600.2605671296 | 2013-11-04 06:15:13 | 56601.215474537 | 2013-11-05 05:10:17 | 708006060 | 46.2 | 50 | 46.2 | 46.2 | 0 | 46.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.1764 | 45.1764 | 82.502 | 1 | PROCESSED | 57613.2009722222 | 2016-08-13 04:49:24 | 56383 | 2013-04-01 00:00:00 | 56646.7076041667 | 2013-12-20 16:58:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006060/ | Quick Look | ![]() |
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784 | CENA N LOBE 3 | 201.1567 | -39.315 | 200.435438 | -39.054679 | 215.153584 | -28.04573 | 309.90401242 | 23.10702351 | 110.949 | 56316.327349537 | 2013-01-24 07:51:23 | 56318.4140046296 | 2013-01-26 09:56:10 | 807134010 | 81.984 | 75 | 81.992 | 81.992 | 0 | 81.984 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.8838 | 73.8838 | 180.2478 | 2 | PROCESSED | 57608.6528356482 | 2016-08-08 15:40:05 | 56708 | 2014-02-20 00:00:00 | 56342.7001157407 | 2013-02-19 16:48:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070127 | Radio source Centaurus A is the closest active galaxy in the Universe (3.7 Mpc). It is surrounded by poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose Chandra follow-up of four regions in the Southern and Northern lobes where Suzaku time was allocated. We also propose joint Chandra-Suzaku observation toward interacting filamentary region where ASCA found a hint of X-ray emission. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in inhomogeneous and multi-phase plasma. The obtained results are guaranteed to improve our knowledge regarding not only the Centaurus A, but all jetted active galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | YASUYUKI TANAKA | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES OF CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807134010/ | Quick Look | ![]() |
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785 | NGC 2300 OFFSET | 116.7261 | 85.6829 | 112.689891 | 85.799301 | 94.232742 | 62.638745 | 127.68344404 | 28.08274711 | 339.9009 | 55235.4123148148 | 2010-02-08 09:53:44 | 55235.7606365741 | 2010-02-08 18:15:19 | 804031010 | 19.196 | 20 | 19.196 | 19.196 | 0 | 19.196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.1477 | 17.1477 | 30.0879 | 0 | PROCESSED | 57550.5104282407 | 2016-06-11 12:15:01 | 55633 | 2011-03-13 00:00:00 | 55266.1898148148 | 2010-03-11 04:33:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804031010/ | Quick Look | ![]() |
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786 | NGC 3998 | 179.4698 | 55.4443 | 178.823114 | 55.722594 | 149.626555 | 48.892783 | 138.19460038 | 60.06850959 | 319.2188 | 56780.8797569445 | 2014-05-03 21:06:51 | 56782.5966898148 | 2014-05-05 14:19:14 | 709002010 | 80.6754 | 80 | 80.6754 | 80.6754 | 0 | 80.6754 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.8901 | 76.8901 | 148.2858 | 0 | PROCESSED | 57615.0693981482 | 2016-08-15 01:39:56 | 57159 | 2015-05-17 00:00:00 | 56793.5775 | 2014-05-16 13:51:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090017 | 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. 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. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709002010/ | Quick Look | ![]() |
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787 | NGC2110 | 88.0489 | -7.4533 | 87.444745 | -7.464256 | 87.748433 | -30.879563 | 212.92425635 | -16.54269345 | 269.0605 | 57101.7987152778 | 2015-03-20 19:10:09 | 57103.3044328704 | 2015-03-22 07:18:23 | 709011010 | 45.6257 | 50 | 45.6257 | 49.4936 | 0 | 49.5096 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8483564815 | 2016-08-17 20:21:38 | 57558 | 2016-06-19 00:00:00 | 57190.4658333333 | 2015-06-17 11:10:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090062 | We propose to observe the Seyfert galaxy NGC2110 twice every half year, which showed a big flare by a factor of around 5 against the normal state around 2012 December. We can observe the echo history following the flare in a time scale of years, and then measure the reflection spectrum very accurately to constrain the geometry of the reflection torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YASUSHI FUKAZAWA | JAP | 9 | AO9 | X-RAY ECHO OF THE BIG FLARE OF SEYFERT GALAXY NGC2110 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709011010/ | Quick Look | ![]() |
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788 | OPHIUCHUS CLUSTER BG | 257.0147 | -25.0612 | 256.247464 | -24.996818 | 258.237934 | -2.148508 | 358.58755189 | 9.10838139 | 89.7146 | 54183.5662268518 | 2007-03-24 13:35:22 | 54183.9169444444 | 2007-03-24 22:00:24 | 801030010 | 15.2983 | 15 | 15.3063 | 15.3063 | 0 | 15.2983 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6351 | 14.6351 | 30.296 | 0 | PROCESSED | 57537.9841898148 | 2016-05-29 23:37:14 | 54736 | 2008-09-27 00:00:00 | 54209.5187384259 | 2007-04-19 12:26:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801030010/ | Quick Look | ![]() |
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789 | FORNAX OFFSET2 | 54.357 | -35.2813 | 53.876494 | -35.444531 | 38.536942 | -52.548461 | 236.43807346 | -53.85479755 | 63.6004 | 54663.2151388889 | 2008-07-16 05:09:48 | 54664.1793287037 | 2008-07-17 04:18:14 | 803007010 | 40.6477 | 30 | 40.678 | 40.6717 | 0 | 40.6477 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8358 | 34.8358 | 83.2979 | 0 | PROCESSED | 57595.6271875 | 2016-07-26 15:03:09 | 55188 | 2009-12-23 00:00:00 | 54822.5201736111 | 2008-12-22 12:29:03 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803007010/ | Quick Look | ![]() |
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790 | RXCJ0243.6-4834 | 40.9015 | -48.5654 | 40.467277 | -48.776586 | 11.225079 | -59.344649 | 265.11995755 | -59.50535864 | 228.2843 | 55191.5472685185 | 2009-12-26 13:08:04 | 55192.0001967593 | 2009-12-27 00:00:17 | 804001010 | 13.2059 | 10 | 13.2139 | 13.2059 | 0 | 13.2219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.5448 | 10.5448 | 39.1299 | 0 | PROCESSED | 57549.9594097222 | 2016-06-10 23:01:33 | 55575 | 2011-01-14 00:00:00 | 55209.1119328704 | 2010-01-13 02:41:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804001010/ | Quick Look | ![]() |
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791 | MACSJ0717.5+3547 | 109.4283 | 37.7329 | 108.583729 | 37.823554 | 105.833167 | 15.353649 | 180.28338253 | 21.07400371 | 90.0014 | 55841.8814699074 | 2011-10-07 21:09:19 | 55844.0440046296 | 2011-10-10 01:03:22 | 806006010 | 100.5473 | 100 | 100.5473 | 100.5553 | 0 | 100.5553 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.847 | 93.847 | 186.8279 | 1 | PROCESSED | 57603.4085763889 | 2016-08-03 09:48:21 | 56240 | 2012-11-09 00:00:00 | 55872.2982523148 | 2011-11-07 07:09:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060016 | MACSJ0717.5+3547 is a forming hot cluster located at z=0.55. Chandra observation resolved a >20 keV hot component near its center, in addition to the average ICM temperature of 11.6 keV. With the most luminous radio halo observed to date, the cluster is in a moment of major merging event. It is also associated with a stream of galaxies oriented to the south east. We propose a Suzaku observation with an exposure of 100 ks, aiming at; confirming the bright > 20 keV component, the very hot component (e.g. Nakazawa+ 2010) evidencing the strong merger, and obtain temperature map of the dim diffuse X-ray observed to the south east and the south west to resolve the nature of these emission. With these observation, merging orientation and phase in this very hot cluster can be resolved. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAZUHIRO NAKAZAWA | JAP | 6 | AO6 | OBSERVING THE FORMATION EPOCH OF A HOT CLUSTER : SUZAKU OBSERVATION OF MACSJ0717.5+3547 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806006010/ | Quick Look | ![]() |
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792 | COMA OUTSKIRTS5 | 193.6628 | 28.7109 | 193.057562 | 28.981718 | 179.928046 | 31.541197 | 98.9627641 | 88.26548083 | 115.9998 | 55903.9110532407 | 2011-12-08 21:51:55 | 55904.722349537 | 2011-12-09 17:20:11 | 806024010 | 31.635 | 30 | 31.659 | 31.651 | 0 | 31.635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.4491 | 29.4491 | 70.0899 | 0 | PROCESSED | 57604.0811226852 | 2016-08-04 01:56:49 | 56284 | 2012-12-23 00:00:00 | 55915.2478587963 | 2011-12-20 05:56:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806024010/ | Quick Look | ![]() |
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793 | AWM7 WEST OFFSET | 43.2295 | 41.594 | 42.421509 | 41.389857 | 53.412323 | 23.911285 | 146.06522235 | -15.7568529 | 90.4999 | 53953.2407060185 | 2006-08-06 05:46:37 | 53954.2343171296 | 2006-08-07 05:37:25 | 801037010 | 39.8177 | 40 | 39.8497 | 39.8177 | 39.8497 | 39.8497 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.1089 | 38.1089 | 85.8359 | 1 | PROCESSED | 57535.2509375 | 2016-05-27 06:01:21 | 54394 | 2007-10-21 00:00:00 | 54020.7562384259 | 2006-10-12 18:08:59 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801037010/ | Quick Look | ![]() |
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794 | A2256 | 256.0138 | 78.7112 | 256.73222 | 78.776756 | 102.386288 | 77.234603 | 111.08264828 | 31.72462704 | 207.9671 | 54049.8560069445 | 2006-11-10 20:32:39 | 54052.0834722222 | 2006-11-13 02:00:12 | 801061010 | 95.5111 | 100 | 95.5111 | 95.5111 | 0 | 95.5111 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.5789 | 103.5789 | 192.4418 | 4 | PROCESSED | 57536.1203009259 | 2016-05-28 02:53:14 | 54456 | 2007-12-22 00:00:00 | 54089.4338425926 | 2006-12-20 10:24:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801061010/ | Quick Look | ![]() |
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795 | FORNAX CLUSTER N30' | 54.7324 | -34.9521 | 54.250694 | -35.113851 | 39.207877 | -52.359999 | 235.87381769 | -53.55297023 | 245 | 54479.2031134259 | 2008-01-14 04:52:29 | 54480.3542708333 | 2008-01-15 08:30:09 | 802021010 | 55.8107 | 53 | 55.8107 | 55.8107 | 0 | 55.8107 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.3441 | 58.3441 | 99.4438 | 2 | PROCESSED | 57541.3134259259 | 2016-06-02 07:31:20 | 54864 | 2009-02-02 00:00:00 | 54490.3658680556 | 2008-01-25 08:46:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 2 | AO2 | DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802021010/ | Quick Look | ![]() |
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796 | NGC 4636 NORTH | 190.6832 | 3.0555 | 190.045327 | 3.32935 | 188.609453 | 7.038209 | 297.61641621 | 65.83736523 | 111.9967 | 54441.2091087963 | 2007-12-07 05:01:07 | 54443.0530555556 | 2007-12-09 01:16:24 | 802022010 | 71.4294 | 67 | 0 | 71.4294 | 0 | 71.4294 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 61.781 | 61.781 | 159.3101 | 3 | PROCESSED | 57540.8428703704 | 2016-06-01 20:13:44 | 55000 | 2009-06-18 00:00:00 | 54633.6943402778 | 2008-06-16 16:39:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 2 | AO2 | DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802022010/ | Quick Look | ![]() |
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797 | THE MOON | 142.9239 | 10.1507 | 142.252683 | 10.371816 | 141.955643 | -4.265217 | 222.87402657 | 40.10832518 | 105.6986 | 56975.5846296296 | 2014-11-14 14:01:52 | 56975.7154166667 | 2014-11-14 17:10:12 | 809001230 | 5.1848 | 45 | 5.1848 | 5.2128 | 0 | 5.2208 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7753009259 | 2016-08-16 18:36:26 | 57358 | 2015-12-02 00:00:00 | 56992.4173148148 | 2014-12-01 10:00:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001230/ | Quick Look | ![]() |
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798 | A2052_GALACTIC_1 | 225.6293 | 8.2927 | 225.017778 | 8.488428 | 220.521255 | 24.436359 | 7.81905694 | 53.73503279 | 292.5625 | 54295.7150810185 | 2007-07-14 17:09:43 | 54296.5765509259 | 2007-07-15 13:50:14 | 802038010 | 33.7334 | 30 | 33.7334 | 33.7334 | 0 | 33.7334 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.5272 | 30.5272 | 74.4239 | 1 | PROCESSED | 57539.2674305556 | 2016-05-31 06:25:06 | 54709 | 2008-08-31 00:00:00 | 54339.4114583333 | 2007-08-27 09:52:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802038010/ | Quick Look | ![]() |
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799 | ABELL 3395 | 96.7698 | -54.5043 | 96.516816 | -54.472103 | 108.474853 | -77.510268 | 263.27498484 | -25.21804833 | 150.0003 | 54815.4865046296 | 2008-12-15 11:40:34 | 54817.3168865741 | 2008-12-17 07:36:19 | 803020010 | 104.3469 | 100 | 104.3469 | 104.3469 | 0 | 104.3469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.661 | 81.661 | 158.1299 | 3 | PROCESSED | 57545.0306828704 | 2016-06-06 00:44:11 | 55210 | 2010-01-14 00:00:00 | 54840.5412268518 | 2009-01-09 12:59:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030078 | We propose to observe a merging cluster Abell 3395 with Suzaku for 100 ks. Abell 3395 has two X-ray emission peaks in the ICM, and they can have a large velocity difference of 3000 km/s at maximum. From the line shift of iron K line, we detect the bulk motion of the ICM, and compare it with the velocity distribution of galaxies. The difference of velocity distributions between the ICM and galaxies reflects the difference of their cross sections during the cluster merging. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 3 | AO3 | COMPARISON BETWEEN VELOCITY DISTRIBUTIONS OF ICM AND GALAXIES IN A MERGING CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803020010/ | Quick Look | ![]() |
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800 | RXCJ2157.4-0747 NW | 329.1863 | -7.8673 | 328.525365 | -8.105597 | 328.55802 | 4.374692 | 49.60582387 | -44.43308021 | 249.9998 | 56972.0423726852 | 2014-11-11 01:01:01 | 56972.5418171296 | 2014-11-11 13:00:13 | 809020010 | 23.1307 | 20 | 23.1307 | 23.1307 | 0 | 23.1307 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7608101852 | 2016-08-16 18:15:34 | 57352 | 2015-11-26 00:00:00 | 56986.4053819444 | 2014-11-25 09:43:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809020010/ | Quick Look | ![]() |
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801 | A1631_W | 193.0037 | -15.2462 | 192.346534 | -14.974562 | 197.903914 | -8.910337 | 303.13836962 | 47.6253175 | 112.9992 | 56305.7238541667 | 2013-01-13 17:22:21 | 56306.3738194444 | 2013-01-14 08:58:18 | 807006010 | 21.0052 | 20 | 21.0212 | 21.0052 | 0 | 21.027 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.5999 | 18.5999 | 56.1539 | 0 | PROCESSED | 57608.4939351852 | 2016-08-08 11:51:16 | 56703 | 2014-02-15 00:00:00 | 56337.5213541667 | 2013-02-14 12:30:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807006010/ | Quick Look | ![]() |
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802 | PERSEUS F_2 | 49.9481 | 41.7834 | 49.118842 | 41.602757 | 58.6868 | 22.59977 | 150.42037818 | -13.03556783 | 257.3692 | 56324.1634259259 | 2013-02-01 03:55:20 | 56324.4342939815 | 2013-02-01 10:25:23 | 807019010 | 17.2086 | 15 | 17.2156 | 17.2156 | 0 | 17.2086 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.5555 | 18.5555 | 23.3999 | 0 | PROCESSED | 57610.4952314815 | 2016-08-10 11:53:08 | 56731 | 2014-03-15 00:00:00 | 56365.4862731482 | 2013-03-14 11:40:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807019010/ | Quick Look | ![]() |
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803 | PERSEUS S1_2 | 49.8718 | 41.2522 | 49.04624 | 41.071281 | 58.468323 | 22.105155 | 150.6720925 | -13.51034913 | 256.4607 | 56333.5592939815 | 2013-02-10 13:25:23 | 56334.2077546296 | 2013-02-11 04:59:10 | 807020010 | 24.4245 | 25 | 24.4485 | 24.4245 | 0 | 24.4485 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23.7447 | 23.7447 | 55.9999 | 0 | PROCESSED | 57610.5627083333 | 2016-08-10 13:30:18 | 56731 | 2014-03-15 00:00:00 | 56365.492662037 | 2013-03-14 11:49:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807020010/ | Quick Look | ![]() |
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804 | ABELL 3395 N | 96.6064 | -54.3394 | 96.351199 | -54.307997 | 107.885857 | -77.369468 | 263.07484149 | -25.27687082 | 220.9999 | 56329.4933449074 | 2013-02-06 11:50:25 | 56330.7758564815 | 2013-02-07 18:37:14 | 807031010 | 46.9751 | 45 | 46.98 | 46.9751 | 0 | 46.9861 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.0083 | 42.0083 | 110.7998 | 2 | PROCESSED | 57610.5772337963 | 2016-08-10 13:51:13 | 56715 | 2014-02-27 00:00:00 | 56349.5329398148 | 2013-02-26 12:47:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070072 | We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO TANAKA | JAP | 7 | AO7 | INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807031010/ | Quick Look | ![]() |
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805 | ABELL 3395 S | 96.923 | -54.6479 | 96.67195 | -54.614958 | 109.024535 | -77.630718 | 263.45062321 | -25.16108018 | 230.2008 | 56339.3357060185 | 2013-02-16 08:03:25 | 56340.1778703704 | 2013-02-17 04:16:08 | 807032010 | 47.1849 | 45 | 47.1849 | 47.1849 | 0 | 47.1849 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.7509 | 49.7509 | 72.7539 | 2 | PROCESSED | 57610.6116898148 | 2016-08-10 14:40:50 | 56717 | 2014-03-01 00:00:00 | 56349.6397569444 | 2013-02-26 15:21:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070072 | We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO TANAKA | JAP | 7 | AO7 | INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807032010/ | Quick Look | ![]() |
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806 | CENA LOBE BGD2 | 197.06 | -39.3239 | 196.354066 | -39.057193 | 211.892811 | -29.411895 | 306.47248435 | 23.43231323 | 291.4078 | 56123.1069212963 | 2012-07-15 02:33:58 | 56123.5835300926 | 2012-07-15 14:00:17 | 807043010 | 21.2772 | 20 | 21.2772 | 21.2772 | 0 | 21.2772 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.4729 | 19.4729 | 41.1679 | 0 | PROCESSED | 57606.6117476852 | 2016-08-06 14:40:55 | 56018 | 2012-04-01 00:00:00 | 56142.2269675926 | 2012-08-03 05:26:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807043010/ | Quick Look | ![]() |
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807 | A2219 | 250.0709 | 46.72 | 249.708198 | 46.815683 | 232.227971 | 67.561681 | 72.64070926 | 41.481603 | 57.4824 | 54924.5730787037 | 2009-04-03 13:45:14 | 54927.1154282407 | 2009-04-06 02:46:13 | 804011010 | 106.6481 | 100 | 106.6481 | 106.6481 | 0 | 106.659 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.7986 | 114.7986 | 219.6398 | 2 | PROCESSED | 57546.0936921296 | 2016-06-07 02:14:55 | 55324 | 2010-05-08 00:00:00 | 54949.5242939815 | 2009-04-28 12:34:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040011 | We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAOMI OTA | JAP | 4 | AO4 | SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804011010/ | Quick Look | ![]() |
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808 | A2029_1 | 227.7409 | 5.7498 | 227.121161 | 5.938119 | 223.529064 | 22.632778 | 6.48668362 | 50.54283023 | 112.9511 | 55224.0253819444 | 2010-01-28 00:36:33 | 55224.3328703704 | 2010-01-28 07:59:20 | 804024010 | 7.6925 | 10 | 7.6925 | 7.7079 | 0 | 7.7005 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.6083 | 4.6083 | 26.5639 | 1 | PROCESSED | 57550.3752314815 | 2016-06-11 09:00:20 | 55612 | 2011-02-20 00:00:00 | 55245.2966203704 | 2010-02-18 07:07:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024010/ | Quick Look | ![]() |
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809 | GALACTIC CENTER GC10 | 266.4308 | -29.5343 | 265.632731 | -29.515028 | 266.867639 | -6.131965 | 359.50116476 | -0.33080245 | 109.7996 | 54171.9994097222 | 2007-03-12 23:59:09 | 54172.6529976852 | 2007-03-13 15:40:19 | 501055010 | 27.2257 | 25 | 27.2257 | 27.2497 | 0 | 27.2337 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1819 | 21.1819 | 56.4539 | 0 | PROCESSED | 57537.6665740741 | 2016-05-29 15:59:52 | 54736 | 2008-09-27 00:00:00 | 54182.3161342593 | 2007-03-23 07:35:14 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501055010/ | Quick Look | ![]() |
810 | NGC2841 | 140.401 | 51.0226 | 139.538295 | 51.235726 | 125.597618 | 33.622725 | 166.8971148 | 44.0746119 | 94.9994 | 55518.5609259259 | 2010-11-18 13:27:44 | 55519.8036342593 | 2010-11-19 19:17:14 | 805028010 | 85.5269 | 80 | 85.5429 | 85.5269 | 0 | 85.5429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.375 | 59.375 | 107.3518 | 1 | PROCESSED | 57554.1596180556 | 2016-06-15 03:49:51 | 55898 | 2011-12-03 00:00:00 | 55530.1645949074 | 2010-11-30 03:57:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050028 | We propose a 80 ksec observation of an edge-on nearby spiral galaxy, NGC 2841 and the halo region. The expected temperature of the halo is ∼0.5 keV, and the characteristics enable Suzku to study the gas properties out to intergalactic space in a reliable way. We aim to obtain the temperature in the halo region within ∼5%, and hopefully an evidence for the gas dynamics not only between the disk and the halo region, but also between the halo and the intergalactic medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IKUYUKI MITSUISHI | JAP | 5 | AO5 | STUDY OF X-RAY HALO OF AN EDGE-ON GALAXY NGC 2841 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805028010/ | Quick Look | ![]() |
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811 | A133_W | 15.4513 | -21.8877 | 14.840059 | -22.156478 | 5.012562 | -26.12974 | 147.70952455 | -84.25382555 | 44.9935 | 55354.0979513889 | 2010-06-07 02:21:03 | 55355.296099537 | 2010-06-08 07:06:23 | 805019010 | 50.0449 | 50 | 50.0449 | 50.0449 | 0 | 50.0449 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2813 | 41.2813 | 103.4758 | 0 | PROCESSED | 57551.9211689815 | 2016-06-12 22:06:29 | 55765 | 2011-07-23 00:00:00 | 55393.3189467593 | 2010-07-16 07:39:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805019010/ | Quick Look | ![]() |
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812 | NGC 253 | 11.8603 | -25.2295 | 11.246067 | -25.502313 | 0.06066 | -27.714636 | 97.43086004 | -87.9001973 | 242.9983 | 55544.0947685185 | 2010-12-14 02:16:28 | 55546.9460763889 | 2010-12-16 22:42:21 | 805018010 | 101.0026 | 100 | 101.0026 | 101.0026 | 0 | 101.0026 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.6689 | 82.6689 | 246.3359 | 1 | PROCESSED | 57554.5316203704 | 2016-06-15 12:45:32 | 55975 | 2012-02-18 00:00:00 | 55607.3286111111 | 2011-02-15 07:53:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050015 | Suzaku observations of a hot halo of nearby, edge-on starburst galaxy, NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by a previous offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and dynamics of the galaxy outflow to the intergalactic space. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORIKO YAMASAKI | JAP | 5 | AO5 | SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805018010/ | Quick Look | ![]() |
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813 | A3667_SE | 303.4605 | -57.0338 | 302.458448 | -57.1853 | 291.78529 | -36.098363 | 340.61636005 | -33.57067764 | 74.2668 | 55298.167349537 | 2010-04-12 04:00:59 | 55299.2716435185 | 2010-04-13 06:31:10 | 805036010 | 66.2872 | 50 | 66.2952 | 66.2872 | 0 | 66.2872 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.249 | 51.249 | 95.3978 | 1 | PROCESSED | 57551.2001967593 | 2016-06-12 04:48:17 | 55675 | 2011-04-24 00:00:00 | 55309.2055324074 | 2010-04-23 04:55:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050039 | We propose an additional offset pointing of Abell 3667, one of the nearest, typical merging cluster. Using the 3 observations pointed along the merger axis on AO-1, we detected a possible super hot component around the cluster center (Nakazawa et al. 2009). To identify the existence and location of this component, we propose to observe the South-East Relic region, about 17 f south to the original southern-most pointing. This observation aims at verifying and locating the super hot component in this cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 5 | AO5 | TRACING THE POSSIBLE SUPER-HOT COMPONENT IN THE MERGING CLUSTER ABELL 3667 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805036010/ | Quick Look | ![]() |
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814 | ABELL1835 OFFSET1 | 210.441 | 2.9038 | 209.807683 | 3.144591 | 207.277058 | 14.34402 | 340.72312739 | 60.50812136 | 306.2398 | 55382.6847453704 | 2010-07-05 16:26:02 | 55384.1217361111 | 2010-07-07 02:55:18 | 805037010 | 49.4391 | 50 | 49.4471 | 49.4391 | 0 | 49.4471 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.0599 | 43.0599 | 124.1398 | 1 | PROCESSED | 57552.5235532407 | 2016-06-13 12:33:55 | 55807 | 2011-09-03 00:00:00 | 55441.2415856482 | 2010-09-02 05:47:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NOBUHIRO OKABE | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805037010/ | Quick Look | ![]() |
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815 | CYGNUS A SUB | 299.7227 | 40.8585 | 299.290982 | 40.72139 | 317.590165 | 59.487138 | 76.23979532 | 5.91406977 | 241.0006 | 56615.3145717593 | 2013-11-19 07:32:59 | 56616.3224189815 | 2013-11-20 07:44:17 | 808016010 | 42.5204 | 40 | 42.5284 | 42.5284 | 0 | 42.5204 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.9173 | 38.9173 | 87.0719 | 1 | PROCESSED | 57613.3640625 | 2016-08-13 08:44:15 | 56995 | 2014-12-04 00:00:00 | 56629.6679050926 | 2013-12-03 16:01:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080018 | We have observed a merging cluster Cygnus A in the Suzaku GO-3 with 45ks. This observation confirmed a hot region between the main and sub components. Furthermore, we found a gas velocity shift between the main and sub by about 2500 km/s. We believe that these are colliding with each other. The current result are limited by statistics and systematic uncertainty. To improve the accurary of the measurement and complete our study, we propose two additional observations located the main and sub components at the center of the FOV. These will provide the best chance to look into a merging cluster "in motion". | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 8 | AO8 | CYGNUS A CLUSTER: THE BEST MERGING SYSTEM FOR THE SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808016010/ | Quick Look | ![]() |
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816 | NGC1550_BGD | 66.1553 | 2.4144 | 65.504252 | 2.300401 | 64.719628 | -18.959095 | 191.78857248 | -30.8138174 | 260.0006 | 56697.3550694444 | 2014-02-09 08:31:18 | 56698.0418634259 | 2014-02-10 01:00:17 | 808061010 | 31.1456 | 30 | 31.1536 | 31.1536 | 0 | 31.1456 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8043171296 | 2016-08-13 19:18:13 | 57102 | 2015-03-21 00:00:00 | 56736.7213425926 | 2014-03-20 17:18:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080110 | We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TORU SASAKI | JAP | 8 | AO8 | STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808061010/ | Quick Look | ![]() |
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817 | THE MOON | 137.2637 | 11.2624 | 136.584895 | 11.465744 | 136.302979 | -4.908841 | 218.49853071 | 35.60818154 | 285.3989 | 56784.0743402778 | 2014-05-07 01:47:03 | 56784.198125 | 2014-05-07 04:45:18 | 809001050 | 5.7625 | 45 | 5.7705 | 5.7625 | 0 | 5.7785 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.371 | 4.371 | 10.6879 | 1 | PROCESSED | 57615.062337963 | 2016-08-15 01:29:46 | 57218 | 2015-07-15 00:00:00 | 56852.5744328704 | 2014-07-14 13:47:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001050/ | Quick Look | ![]() |
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818 | THE MOON | 24.3624 | 9.7895 | 23.702448 | 9.535235 | 26.139692 | -0.327211 | 141.30582848 | -51.43331262 | 73.7995 | 56857.0209259259 | 2014-07-19 00:30:08 | 56857.1515856482 | 2014-07-19 03:38:17 | 809001140 | 4.2907 | 45 | 4.2907 | 4.2907 | 0 | 4.2907 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4055439815 | 2016-08-15 09:43:59 | 57267 | 2015-09-02 00:00:00 | 56902.7022685185 | 2014-09-02 16:51:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001140/ | Quick Look | ![]() |
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819 | THE MOON | 139.925 | 10.5889 | 139.25032 | 10.800859 | 139.007269 | -4.769046 | 220.6720528 | 37.66748388 | 105.6998 | 56975.3249305556 | 2014-11-14 07:47:54 | 56975.4487615741 | 2014-11-14 10:46:13 | 809001210 | 3.5246 | 45 | 3.5246 | 3.5246 | 0 | 3.5246 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.771412037 | 2016-08-16 18:30:50 | 57358 | 2015-12-02 00:00:00 | 56992.4131018518 | 2014-12-01 09:54:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001210/ | Quick Look | ![]() |
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820 | THE MOON | 144.4436 | 10.011 | 143.773859 | 10.236526 | 143.42105 | -3.916716 | 223.94276709 | 41.37428155 | 105.6999 | 56975.7165856482 | 2014-11-14 17:11:53 | 56975.8473611111 | 2014-11-14 20:20:12 | 809001240 | 6.2192 | 45 | 6.2192 | 6.2272 | 0 | 6.2512 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7771412037 | 2016-08-16 18:39:05 | 57358 | 2015-12-02 00:00:00 | 56992.4178703704 | 2014-12-01 10:01:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001240/ | Quick Look | ![]() |
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821 | THE MOON | 330.3821 | -8.1914 | 329.721062 | -8.43265 | 329.560437 | 3.662364 | 50.06648816 | -45.61675095 | 252.3 | 56989.8522685185 | 2014-11-28 20:27:16 | 56989.9654976852 | 2014-11-28 23:10:19 | 809001280 | 4.7272 | 45 | 4.7272 | 4.7272 | 0 | 4.7272 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.401712963 | 2016-08-17 09:38:28 | 57415 | 2016-01-28 00:00:00 | 57002.4419444445 | 2014-12-11 10:36:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001280/ | Quick Look | ![]() |
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822 | THE MOON | 332.0733 | -7.3936 | 331.41518 | -7.63885 | 331.413251 | 3.82441 | 52.31004503 | -46.62982693 | 251.0013 | 56989.9669444444 | 2014-11-28 23:12:24 | 56990.1008449074 | 2014-11-29 02:25:13 | 809001290 | 4.227 | 45 | 4.227 | 4.2506 | 0 | 4.235 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4062962963 | 2016-08-17 09:45:04 | 57415 | 2016-01-28 00:00:00 | 57002.4422453704 | 2014-12-11 10:36:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001290/ | Quick Look | ![]() |
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823 | CEN_A_LOBE_N2 | 201.2142 | -42.0778 | 200.484454 | -41.817568 | 216.546241 | -30.52743 | 309.53774085 | 20.36490033 | 292.2294 | 56861.2578587963 | 2014-07-23 06:11:19 | 56862.6946990741 | 2014-07-24 16:40:22 | 809003010 | 52.1427 | 50 | 52.1507 | 52.1427 | 0 | 52.1587 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.3107 | 19.3107 | 40.0719 | 0 | PROCESSED | 57615.4510648148 | 2016-08-15 10:49:32 | 57242 | 2015-08-08 00:00:00 | 56875.1594560185 | 2014-08-06 03:49:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809003010/ | Quick Look | ![]() |
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824 | RXJ1713-3946_ID2 | 258.3083 | -40.2394 | 257.437413 | -40.180894 | 260.672603 | -17.175399 | 346.91054647 | -0.70324775 | 87.0013 | 55243.7284722222 | 2010-02-16 17:29:00 | 55244.1258564815 | 2010-02-17 03:01:14 | 504028010 | 19.0093 | 20 | 19.0093 | 19.0173 | 0 | 19.0173 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.8263 | 11.8263 | 34.3319 | 0 | PROCESSED | 57550.6004976852 | 2016-06-11 14:24:43 | 55622 | 2011-03-02 00:00:00 | 55256.0518171296 | 2010-03-01 01:14:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504028010/ | Quick Look | ![]() |
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825 | N23_DEML71 | 76.4544 | -67.9572 | 76.483575 | -68.02238 | 338.831134 | -84.597327 | 278.75688601 | -34.83345845 | 297.0986 | 56021.0207986111 | 2012-04-04 00:29:57 | 56023.6043402778 | 2012-04-06 14:30:15 | 807008010 | 101.9614 | 100 | 101.9614 | 101.9614 | 0 | 101.9614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.0031 | 99.0031 | 223.204 | 1 | PROCESSED | 57605.1620023148 | 2016-08-05 03:53:17 | 56401 | 2013-04-19 00:00:00 | 56034.2910069444 | 2012-04-17 06:59:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070036 | Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYUKI UCHIDA | JAP | 7 | AO7 | FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807008010/ | Quick Look | ![]() |
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826 | CEN_A_LOBE_N4 | 200.0149 | -42.0781 | 199.290063 | -41.815855 | 215.61315 | -30.91319 | 308.59567712 | 20.47867303 | 294.4884 | 56864.2718634259 | 2014-07-26 06:31:29 | 56865.6863194444 | 2014-07-27 16:28:18 | 809005010 | 49.4215 | 50 | 49.4215 | 50.3093 | 0 | 50.3093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.7711 | 14.7711 | 31.0519 | 0 | PROCESSED | 57615.4593055556 | 2016-08-15 11:01:24 | 57242 | 2015-08-08 00:00:00 | 56875.2119675926 | 2014-08-06 05:05:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809005010/ | Quick Look | ![]() |
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827 | A3112W | 49.1257 | -44.1666 | 48.689569 | -44.349648 | 25.156648 | -58.765875 | 252.9579492 | -56.34974536 | 40.0005 | 56834.0356481482 | 2014-06-26 00:51:20 | 56835.5486458333 | 2014-06-27 13:10:03 | 809025010 | 48.949 | 45 | 48.949 | 48.949 | 0 | 48.949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.966 | 11.966 | 40.6069 | 2 | PROCESSED | 57615.3397685185 | 2016-08-15 08:09:16 | 57249 | 2015-08-15 00:00:00 | 56881.2363078704 | 2014-08-12 05:40:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809025010/ | Quick Look | ![]() |
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828 | FJ0846+5326 | 131.5564 | 53.4343 | 130.632054 | 53.617254 | 118.481008 | 34.023671 | 164.73615985 | 38.37651034 | 277.0006 | 56764.8665393518 | 2014-04-17 20:47:49 | 56766.1148032407 | 2014-04-19 02:45:19 | 809037010 | 44.7166 | 45 | 44.7166 | 44.7166 | 0 | 44.7166 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9585416667 | 2016-08-14 23:00:18 | 57145 | 2015-05-03 00:00:00 | 56782.5079976852 | 2014-05-05 12:11:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809037010/ | Quick Look | ![]() |
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829 | CENA LOBE 1 | 201.4716 | -38.9356 | 200.750271 | -38.675827 | 215.22462 | -27.598918 | 310.226071 | 23.44775478 | 285.9999 | 56117.7018287037 | 2012-07-09 16:50:38 | 56119.8959953704 | 2012-07-11 21:30:14 | 807040010 | 84.161 | 80 | 84.161 | 84.161 | 0 | 84.161 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.2838 | 72.2838 | 188.7955 | 3 | PROCESSED | 57606.6375347222 | 2016-08-06 15:18:03 | 56018 | 2012-04-01 00:00:00 | 56159.3425925926 | 2012-08-20 08:13:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807040010/ | Quick Look | ![]() |
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830 | CENA LOBE 2 | 201.7887 | -39.7611 | 201.063779 | -39.501882 | 215.867616 | -28.245975 | 310.35734609 | 22.59512331 | 290.5003 | 56122.1648958333 | 2012-07-14 03:57:27 | 56122.4584490741 | 2012-07-14 11:00:10 | 807041020 | 12.9463 | 80 | 12.9463 | 12.9463 | 0 | 12.9463 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.6518 | 12.6518 | 25.3519 | 0 | PROCESSED | 57606.6009027778 | 2016-08-06 14:25:18 | 56018 | 2012-04-01 00:00:00 | 56142.1626736111 | 2012-08-03 03:54:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807041020/ | Quick Look | ![]() |
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831 | A2256N | 256.1941 | 78.9961 | 256.949832 | 79.060716 | 101.697267 | 76.992175 | 111.38046428 | 31.59001765 | 219.8042 | 56234.8690625 | 2012-11-03 20:51:27 | 56236.1877083333 | 2012-11-05 04:30:18 | 807024010 | 62.2855 | 60 | 62.2855 | 62.2855 | 0 | 62.2855 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 76.5361 | 76.5361 | 113.9039 | 0 | PROCESSED | 57607.9455555556 | 2016-08-07 22:41:36 | 56630 | 2013-12-04 00:00:00 | 56260.5238657407 | 2012-11-29 12:34:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070058 | We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 7 | AO7 | THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807024010/ | Quick Look | ![]() |
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832 | MRK421 | 166.1418 | 38.2711 | 165.447021 | 38.540933 | 151.207571 | 29.566146 | 179.67525089 | 65.03258412 | 111.0988 | 54803.7278240741 | 2008-12-03 17:28:04 | 54805.9480324074 | 2008-12-05 22:45:10 | 703020010 | 101.3075 | 100 | 101.3315 | 101.3075 | 0 | 101.3315 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.5148 | 65.5148 | 191.7877 | 3 | PROCESSED | 57544.7029398148 | 2016-06-05 16:52:14 | 55188 | 2009-12-23 00:00:00 | 54818.7659837963 | 2008-12-18 18:23:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 3 | AO3 | STUDY OF HARD X-RAY EVOLUTION FROM THE BRIGHTEST BLAZAR JET. | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703020010/ | Quick Look | ![]() |
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833 | AWM7 27' SOUTH | 43.6454 | 41.2726 | 42.837995 | 41.069836 | 53.624746 | 23.507895 | 146.50839268 | -15.89370788 | 257.401 | 55975.6646296296 | 2012-02-18 15:57:04 | 55976.5071180556 | 2012-02-19 12:10:15 | 806009010 | 34.9735 | 30 | 34.9815 | 34.9735 | 0 | 34.9735 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.6452 | 33.6452 | 72.7819 | 1 | PROCESSED | 57604.6468055556 | 2016-08-04 15:31:24 | 56361 | 2013-03-10 00:00:00 | 55994.9781828704 | 2012-03-08 23:28:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806009010/ | Quick Look | ![]() |
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834 | MS 1512.4+3647 | 228.6059 | 36.6198 | 228.120322 | 36.804723 | 210.693369 | 51.882401 | 59.43888584 | 58.40149096 | 128.9265 | 54463.6508449074 | 2007-12-29 15:37:13 | 54469.6946527778 | 2008-01-04 16:40:18 | 802034010 | 268.8898 | 200 | 268.9458 | 268.8898 | 0 | 268.9458 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.4803 | 47.4803 | 102.8019 | 2 | PROCESSED | 57541.0217476852 | 2016-06-02 00:31:19 | 54909 | 2009-03-19 00:00:00 | 54542.2596296296 | 2008-03-17 06:13:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MADOKA KAWAHARADA | JAP | 2 | AO2 | EVOLUTION STUDY ON AMOUNT OF METALS IN THE ICM USING A DISTANT CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802034010/ | Quick Look | ![]() |
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835 | CTB109 NORTHEAST | 345.764 | 59.0015 | 345.238644 | 58.732029 | 24.240732 | 56.810585 | 109.36320905 | -0.98507066 | 252.0025 | 55910.0815393518 | 2011-12-15 01:57:25 | 55910.7522106482 | 2011-12-15 18:03:11 | 506039010 | 30.4058 | 30 | 30.4058 | 30.4058 | 0 | 30.4058 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.7473 | 30.7473 | 57.9219 | 1 | PROCESSED | 57604.1437268518 | 2016-08-04 03:26:58 | 56289 | 2012-12-28 00:00:00 | 55921.9865277778 | 2011-12-26 23:40:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506039010/ | Quick Look | ![]() |
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836 | THE MOON | 344.0153 | -3.4 | 343.369759 | -3.667219 | 343.958901 | 3.149835 | 68.62224539 | -53.63365394 | 247.8502 | 56990.8695717593 | 2014-11-29 20:52:11 | 56991.0002546296 | 2014-11-30 00:00:22 | 809001360 | 4.8998 | 45 | 4.8998 | 4.8998 | 0 | 4.8998 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4137615741 | 2016-08-17 09:55:49 | 57415 | 2016-01-28 00:00:00 | 57007.4035648148 | 2014-12-16 09:41:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001360/ | Quick Look | ![]() |
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837 | CIZA J2242 OFFSET | 339.3149 | 52.6806 | 338.804058 | 52.420641 | 11.931322 | 54.574747 | 103.28112871 | -4.99517915 | 17.9944 | 55772.8222337963 | 2011-07-30 19:44:01 | 55774.1446180556 | 2011-08-01 03:28:15 | 806002010 | 55.9134 | 60 | 55.9356 | 55.9134 | 0 | 55.9134 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.1891 | 73.1891 | 114.2 | 2 | PROCESSED | 57602.7241666667 | 2016-08-02 17:22:48 | 56162 | 2012-08-23 00:00:00 | 55792.2422222222 | 2011-08-19 05:48:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060014 | Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | SHO NISHINO | JAP | 6 | AO6 | SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806002010/ | Quick Look | ![]() |
838 | FILAMENT JUNCTION 2 | 149.2538 | 26.1497 | 148.542222 | 26.388047 | 142.296251 | 12.813389 | 204.13118538 | 51.20952403 | 290.4949 | 55699.3618402778 | 2011-05-18 08:41:03 | 55701.114849537 | 2011-05-20 02:45:23 | 806004010 | 70.1591 | 70 | 70.1591 | 70.1671 | 0 | 70.1671 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.3295 | 63.3295 | 151.4357 | 1 | PROCESSED | 57602.1051851852 | 2016-08-02 02:31:28 | 56092 | 2012-06-14 00:00:00 | 55722.7303356482 | 2011-06-10 17:31:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806004010/ | Quick Look | ![]() |
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839 | 1A1742-294(GCBGD1) | 266.5239 | -29.5135 | 265.725945 | -29.49468 | 266.948574 | -6.109181 | 359.5610912 | -0.38914955 | 264.8673 | 53643.1880092593 | 2005-09-30 04:30:44 | 53643.2536921296 | 2005-09-30 06:05:19 | 100037020 | 3.273 | 5 | 3.281 | 3.273 | 3.2887 | 3.281 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.0911 | 3.0911 | 5.6719 | 0 | PROCESSED | 57527.4425347222 | 2016-05-19 10:37:15 | 54247 | 2007-05-27 00:00:00 | 54035.5547453704 | 2006-10-27 13:18:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037020/ | Quick Look | ![]() |
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840 | GALACTIC CENTER GC9 | 266.6299 | -29.2499 | 265.833607 | -29.231598 | 267.035089 | -5.843458 | 359.83430056 | -0.33104727 | 109.8001 | 54171.3410532407 | 2007-03-12 08:11:07 | 54171.9988888889 | 2007-03-12 23:58:24 | 501054010 | 26.1044 | 25 | 26.1044 | 26.1044 | 0 | 26.1044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.5424 | 23.5424 | 56.8299 | 0 | PROCESSED | 57537.6542013889 | 2016-05-29 15:42:03 | 54736 | 2008-09-27 00:00:00 | 54182.2954166667 | 2007-03-23 07:05:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501054010/ | Quick Look | ![]() |
841 | VERJ2019_P3 | 304.792 | 36.828 | 304.322431 | 36.670095 | 321.385407 | 54.239801 | 74.98489793 | 0.41476969 | 250.4389 | 56971.0428009259 | 2014-11-10 01:01:38 | 56972.0349537037 | 2014-11-11 00:50:20 | 509030010 | 41.0715 | 40 | 41.0795 | 41.0715 | 0 | 41.0875 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7632175926 | 2016-08-16 18:19:02 | 57352 | 2015-11-26 00:00:00 | 56982.4314467593 | 2014-11-21 10:21:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090120 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 9 | AO9 | SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509030010/ | Quick Look | ![]() |
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842 | AWM7 SE1 | 44.3556 | 41.1876 | 43.546511 | 40.987213 | 54.148816 | 23.260587 | 147.03812428 | -15.71286613 | 256.9997 | 56706.6681828704 | 2014-02-18 16:02:11 | 56707.1284953704 | 2014-02-19 03:05:02 | 808025010 | 16.8194 | 15 | 16.8194 | 16.8434 | 0 | 16.8274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.321 | 15.321 | 39.7619 | 0 | PROCESSED | 57613.8533912037 | 2016-08-13 20:28:53 | 57085 | 2015-03-04 00:00:00 | 56719.747662037 | 2014-03-03 17:56:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808025010/ | Quick Look | ![]() |
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843 | WESTERLUND1_3 | 252.0931 | -46.1953 | 251.177246 | -46.107555 | 256.5618 | -23.584825 | 339.43313351 | -0.79934014 | 282.1087 | 55462.25625 | 2010-09-23 06:09:00 | 55463.3946296296 | 2010-09-24 09:28:16 | 505051010 | 50.2046 | 50 | 50.2046 | 50.2046 | 0 | 50.2046 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.7966 | 40.7966 | 98.3438 | 1 | PROCESSED | 57553.5465162037 | 2016-06-14 13:06:59 | 55840 | 2011-10-06 00:00:00 | 55474.0771180556 | 2010-10-05 01:51:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505051010/ | Quick Look | ![]() |
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844 | AWM7 BGD | 41.6937 | 42.4876 | 40.885444 | 42.278459 | 52.542503 | 25.125109 | 144.58796377 | -15.48250354 | 257.001 | 56707.9150810185 | 2014-02-19 21:57:43 | 56708.3828587963 | 2014-02-20 09:11:19 | 808027010 | 20.4971 | 20 | 20.5011 | 20.5051 | 0 | 20.4971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.116 | 22.116 | 40.41 | 0 | PROCESSED | 57613.8622106482 | 2016-08-13 20:41:35 | 57086 | 2015-03-05 00:00:00 | 56720.6154976852 | 2014-03-04 14:46:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808027010/ | Quick Look | ![]() |
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845 | NGC 5044 | 198.8504 | -16.3899 | 198.183934 | -16.125889 | 203.593771 | -7.791309 | 311.2339251 | 46.09520433 | 290.0016 | 53918.7631712963 | 2006-07-02 18:18:58 | 53919.3600115741 | 2006-07-03 08:38:25 | 801046010 | 19.7466 | 20 | 19.7466 | 19.7466 | 19.7466 | 19.7466 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.9716 | 17.9716 | 51.562 | 1 | PROCESSED | 57534.8255208333 | 2016-05-26 19:48:45 | 54394 | 2007-10-21 00:00:00 | 53930.6133217593 | 2006-07-14 14:43:11 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801046010/ | Quick Look | ![]() |
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846 | ASO0147 | 98.4346 | 6.5402 | 97.762331 | 6.579413 | 98.750752 | -16.644923 | 205.09585789 | -0.932863 | 292.0552 | 54931.9181481482 | 2009-04-10 22:02:08 | 54932.5036921296 | 2009-04-11 12:05:19 | 504047010 | 24.0413 | 20 | 24.0413 | 24.0413 | 0 | 24.0413 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.2409 | 23.2409 | 50.562 | 1 | PROCESSED | 57546.1122685185 | 2016-06-07 02:41:40 | 55324 | 2010-05-08 00:00:00 | 54949.5271180556 | 2009-04-28 12:39:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504047010/ | Quick Look | ![]() |
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847 | THE MOON | 17.8678 | 7.6685 | 17.216041 | 7.403045 | 19.391263 | 0.083978 | 131.57870726 | -54.86656285 | 73.8004 | 56856.4839814815 | 2014-07-18 11:36:56 | 56856.6565162037 | 2014-07-18 15:45:23 | 809001100 | 8.2482 | 45 | 8.2642 | 8.2482 | 0 | 8.2642 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3962962963 | 2016-08-15 09:30:40 | 57233 | 2015-07-30 00:00:00 | 56867.7358912037 | 2014-07-29 17:39:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001100/ | Quick Look | ![]() |
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848 | THE MOON | 27.6562 | 10.6142 | 26.991894 | 10.366866 | 29.46244 | -0.715898 | 145.72862444 | -49.61972993 | 73.8014 | 56857.2778935185 | 2014-07-19 06:40:10 | 56857.4015856482 | 2014-07-19 09:38:17 | 809001160 | 6.3331 | 45 | 6.3411 | 6.3411 | 0 | 6.3331 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4093287037 | 2016-08-15 09:49:26 | 57267 | 2015-09-02 00:00:00 | 56902.690775463 | 2014-09-02 16:34:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001160/ | Quick Look | ![]() |
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849 | CEN_A_LOBE_N1 | 201.8136 | -42.0782 | 201.081414 | -41.819016 | 217.012441 | -30.336854 | 310.00727378 | 20.30096505 | 292.0832 | 56859.7082060185 | 2014-07-21 16:59:49 | 56861.2571990741 | 2014-07-23 06:10:22 | 809002010 | 50.3801 | 50 | 50.3881 | 50.3881 | 0 | 50.3801 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.4775 | 11.4775 | 24.4719 | 0 | PROCESSED | 57615.4533333333 | 2016-08-15 10:52:48 | 57242 | 2015-08-08 00:00:00 | 56875.1360185185 | 2014-08-06 03:15:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809002010/ | Quick Look | ![]() |
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850 | M17 | 275.2076 | -16.1829 | 274.486266 | -16.206429 | 275.030512 | 7.16685 | 15.0906551 | -0.7606192 | 110.1996 | 53805.8263425926 | 2006-03-11 19:49:56 | 53808.5349421296 | 2006-03-14 12:50:19 | 501003010 | 102.7021 | 100 | 102.7101 | 102.7101 | 102.7021 | 102.7101 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 92.5661 | 92.5661 | 233.9678 | 4 | PROCESSED | 57533.2492939815 | 2016-05-25 05:58:59 | 54394 | 2007-10-21 00:00:00 | 53905.822662037 | 2006-06-19 19:44:38 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASAHIRO TSUJIMOTO | JAP | 1 | AO1 | XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501003010/ | Quick Look | ![]() |
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851 | A3112BG | 50.3312 | -44.7001 | 49.902687 | -44.878678 | 26.087437 | -59.659599 | 253.38993788 | -55.36648392 | 25.002 | 56828.7830208333 | 2014-06-20 18:47:33 | 56829.3648611111 | 2014-06-21 08:45:24 | 809028010 | 13.041 | 30 | 13.041 | 13.041 | 0 | 24.268 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.199 | 20.199 | 50.2559 | 0 | PROCESSED | 57615.2871064815 | 2016-08-15 06:53:26 | 57394 | 2016-01-07 00:00:00 | 56873.1992824074 | 2014-08-04 04:46:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809028010/ | Quick Look | ![]() |
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852 | FJ0854+4908_OFFSET | 133.7467 | 48.8373 | 132.873661 | 49.028229 | 121.743576 | 30.102388 | 170.52256786 | 40.09070343 | 275.4911 | 56776.9674074074 | 2014-04-29 23:13:04 | 56777.6286805556 | 2014-04-30 15:05:18 | 809039010 | 31.9155 | 30 | 31.9155 | 31.9155 | 0 | 31.9155 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.928 | 28.928 | 57.1259 | 0 | PROCESSED | 57615.0205555556 | 2016-08-15 00:29:36 | 57218 | 2015-07-15 00:00:00 | 56852.6002546296 | 2014-07-14 14:24:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809039010/ | Quick Look | ![]() |
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853 | FJ1336+3553 | 203.9051 | 36.0067 | 203.345869 | 36.26171 | 185.165039 | 42.045012 | 79.05269341 | 77.07938329 | 299.9994 | 56835.5627546296 | 2014-06-27 13:30:22 | 56836.6564814815 | 2014-06-28 15:45:20 | 809040010 | 49.8464 | 50 | 49.8464 | 49.8464 | 0 | 49.8464 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3306828704 | 2016-08-15 07:56:11 | 57212 | 2015-07-09 00:00:00 | 56846.5971180556 | 2014-07-08 14:19:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809040010/ | Quick Look | ![]() |
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854 | CTB 37B | 258.4918 | -38.2006 | 257.636889 | -38.143005 | 260.643359 | -15.13191 | 348.64561092 | 0.37683278 | 270.1267 | 53974.0604976852 | 2006-08-27 01:27:07 | 53976.2398032407 | 2006-08-29 05:45:19 | 501007010 | 82.8151 | 80 | 82.8711 | 82.8151 | 82.8791 | 82.8631 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.8603 | 68.8603 | 188.2779 | 2 | PROCESSED | 57535.4428703704 | 2016-05-27 10:37:44 | 54526 | 2008-03-01 00:00:00 | 54053.4840162037 | 2006-11-14 11:36:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 1 | AO1 | UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501007010/ | Quick Look | ![]() |
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855 | (L,B)=(0.25,-0.27) | 266.8068 | -28.8823 | 266.012807 | -28.864862 | 267.181973 | -5.472426 | 0.22878525 | -0.27253682 | 265.3343 | 54343.5232986111 | 2007-08-31 12:33:33 | 54346.7919560185 | 2007-09-03 19:00:25 | 502022010 | 134.7904 | 133 | 134.7984 | 134.8064 | 0 | 134.7904 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116.8425 | 116.8425 | 282.3759 | 1 | PROCESSED | 57539.9810185185 | 2016-05-31 23:32:40 | 54724 | 2008-09-15 00:00:00 | 54356.5238657407 | 2007-09-13 12:34:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKESHI TSURU | JAP | 2 | AO2 | GLOBAL STRUCTURES OF THE GALACTIC CENTER DIFFUSE X-RAY PLASMA (GCDX) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502022010/ | Quick Look | ![]() |
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856 | RS OPH | 267.5535 | -6.6951 | 266.880129 | -6.681587 | 267.45304 | 16.723864 | 19.81011082 | 10.37967032 | 94.9072 | 55987.2608796296 | 2012-03-01 06:15:40 | 55988.855 | 2012-03-02 20:31:12 | 406033010 | 69.386 | 100 | 69.386 | 69.386 | 0 | 69.386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.0899 | 60.0899 | 137.7198 | 0 | PROCESSED | 57604.8300810185 | 2016-08-04 19:55:19 | 56375 | 2013-03-24 00:00:00 | 56008.324224537 | 2012-03-22 07:46:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | DAI TAKEI | JAP | 6 | AO6 | OBSERVATION OF A RECURRENT NOVA REMNANT RS OPHIUCHI | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406033010/ | Quick Look | ![]() |
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857 | FORNAX OFFSET1 | 54.5865 | -35.7706 | 54.109381 | -35.93292 | 38.512958 | -53.072025 | 237.25707491 | -53.65522298 | 45.0001 | 54662.3087962963 | 2008-07-15 07:24:40 | 54663.2106365741 | 2008-07-16 05:03:19 | 803006010 | 35.2402 | 30 | 35.2482 | 35.2402 | 0 | 35.2513 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.441 | 30.441 | 77.9179 | 0 | PROCESSED | 57543.0490393518 | 2016-06-04 01:10:37 | 55055 | 2009-08-12 00:00:00 | 54686.1787384259 | 2008-08-08 04:17:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803006010/ | Quick Look | ![]() |
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858 | UGC5101 | 144.0189 | 61.4178 | 143.073331 | 61.641673 | 122.524313 | 43.933823 | 152.38145034 | 42.89433298 | 112.6892 | 54039.7635300926 | 2006-10-31 18:19:29 | 54040.396087963 | 2006-11-01 09:30:22 | 701002020 | 42.166 | 35 | 42.166 | 42.174 | 42.182 | 42.182 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.5589 | 33.5589 | 54.6519 | 0 | PROCESSED | 57536.0043518518 | 2016-05-28 00:06:16 | 54735 | 2008-09-26 00:00:00 | 54063.3945949074 | 2006-11-24 09:28:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002020/ | Quick Look | ![]() |
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859 | PKS 0558-504 | 89.9334 | -50.4402 | 89.629898 | -50.441281 | 89.86386 | -73.882062 | 257.95215413 | -28.57698713 | 210.2147 | 54119.7661805556 | 2007-01-19 18:23:18 | 54120.3203009259 | 2007-01-20 07:41:14 | 701011030 | 21.2563 | 20 | 21.2563 | 21.2563 | 0 | 21.2563 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.1145 | 19.1145 | 47.87 | 0 | PROCESSED | 57536.8847916667 | 2016-05-28 21:14:06 | 54735 | 2008-09-26 00:00:00 | 54133.3934259259 | 2007-02-02 09:26:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011030/ | Quick Look | ![]() |
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860 | V2487 OPH | 262.9946 | -19.3061 | 262.257209 | -19.270365 | 263.364925 | 3.973676 | 6.53905762 | 7.73892052 | 274.1277 | 55478.2880439815 | 2010-10-09 06:54:47 | 55479.5827893518 | 2010-10-10 13:59:13 | 405021010 | 56.3076 | 50 | 56.3156 | 56.3076 | 0 | 56.3236 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.358 | 51.358 | 111.832 | 2 | PROCESSED | 57553.6771875 | 2016-06-14 16:15:09 | 55854 | 2011-10-20 00:00:00 | 55488.179224537 | 2010-10-19 04:18:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | JAP | 5 | AO5 | SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405021010/ | Quick Look | ![]() |
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861 | SWIFT J1628.1+5145 | 246.9541 | 51.8388 | 246.639575 | 51.948443 | 220.797096 | 71.358115 | 79.81767806 | 42.92326404 | 60.2479 | 53840.7843518518 | 2006-04-15 18:49:28 | 53841.3904976852 | 2006-04-16 09:22:19 | 701016010 | 23.589 | 20 | 23.605 | 23.597 | 23.589 | 23.597 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.6261 | 20.6261 | 52.3599 | 2 | PROCESSED | 57533.4625231482 | 2016-05-25 11:06:02 | 54394 | 2007-10-21 00:00:00 | 53905.7494444444 | 2006-06-19 17:59:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701016010/ | Quick Look | ![]() |
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862 | PERSEUS OFFSET-E | 49.943 | 41.2145 | 49.117489 | 41.033844 | 58.512606 | 22.054116 | 150.73941272 | -13.51227041 | 269.9995 | 55615.1921180556 | 2011-02-23 04:36:39 | 55615.8335416667 | 2011-02-23 20:00:18 | 805045010 | 27.4595 | 25 | 27.4755 | 27.4595 | 0 | 27.4755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.5296 | 25.5296 | 55.3919 | 0 | PROCESSED | 57601.0240856482 | 2016-08-01 00:34:41 | 55996 | 2012-03-10 00:00:00 | 55628.1301157407 | 2011-03-08 03:07:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805045010/ | Quick Look | ![]() |
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863 | SS 433 | 287.9531 | 4.9906 | 287.335307 | 4.906206 | 290.183209 | 27.182001 | 39.69950989 | -2.2379409 | 78.6445 | 53829.6109606482 | 2006-04-04 14:39:47 | 53830.5327662037 | 2006-04-05 12:47:11 | 401003010 | 38.6767 | 40 | 38.6767 | 38.6767 | 38.6767 | 38.6767 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.2411 | 28.2411 | 79.634 | 1 | PROCESSED | 57533.395162037 | 2016-05-25 09:29:02 | 54394 | 2007-10-21 00:00:00 | 53906.1478125 | 2006-06-20 03:32:51 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401003010/ | Quick Look | ![]() |
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864 | NGC1386 | 54.1629 | -35.9533 | 53.686009 | -36.117288 | 37.868182 | -53.108166 | 237.58696036 | -53.99184818 | 64.5172 | 54309.0884259259 | 2007-07-28 02:07:20 | 54310.1668402778 | 2007-07-29 04:00:15 | 702002010 | 55.5226 | 50 | 55.5226 | 55.5306 | 0 | 55.5306 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.5213 | 47.5213 | 93.1439 | 1 | PROCESSED | 57539.3619907407 | 2016-05-31 08:41:16 | 54707 | 2008-08-29 00:00:00 | 54339.0775115741 | 2007-08-27 01:51:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702002010/ | Quick Look | ![]() |
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865 | HESS J1837-069 | 279.4395 | -6.8651 | 278.765532 | -6.909152 | 279.755327 | 16.256333 | 25.2664546 | -0.10276403 | 102.6144 | 54164.5341898148 | 2007-03-05 12:49:14 | 54165.4286342593 | 2007-03-06 10:17:14 | 401026010 | 42.1911 | 40 | 42.1911 | 42.1991 | 0 | 42.2071 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7021 | 37.7021 | 77.2599 | 1 | PROCESSED | 57537.6010185185 | 2016-05-29 14:25:28 | 54750 | 2008-10-11 00:00:00 | 54171.2613425926 | 2007-03-12 06:16:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 1 | AO1 | INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401026010/ | Quick Look | ![]() |
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866 | 1RXS J070407.9+26250 | 106.0316 | 26.4199 | 105.25762 | 26.494968 | 104.352906 | 3.774212 | 190.26714041 | 14.29962915 | 96.1437 | 54749.1266319444 | 2008-10-10 03:02:21 | 54750.3682175926 | 2008-10-11 08:50:14 | 403003010 | 53.5519 | 50 | 53.5519 | 53.5519 | 0 | 53.5519 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.1405 | 41.1405 | 107.2319 | 0 | PROCESSED | 57544.1456944445 | 2016-06-05 03:29:48 | 55148 | 2009-11-13 00:00:00 | 54780.5445949074 | 2008-11-10 13:04:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MANABU ISHIDA | JAP | 3 | AO3 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403003010/ | Quick Look | ![]() |
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867 | GC16 | 267.4868 | -29.3131 | 266.689954 | -29.298954 | 267.787562 | -5.891312 | 0.16607902 | -1.00376926 | 260.5335 | 54383.6397800926 | 2007-10-10 15:21:17 | 54384.0419444444 | 2007-10-11 01:00:24 | 502004010 | 19.873 | 20 | 19.873 | 19.8903 | 0 | 19.8743 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.8321 | 18.8321 | 34.736 | 0 | PROCESSED | 57540.2356597222 | 2016-06-01 05:39:21 | 54771 | 2008-11-01 00:00:00 | 54402.5680208333 | 2007-10-29 13:37:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502004010/ | Quick Look | ![]() |
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868 | NGC3393 | 162.075 | -25.2139 | 161.475136 | -24.949432 | 174.292392 | -30.103718 | 270.6699706 | 29.83420275 | 292.9271 | 54243.7827662037 | 2007-05-23 18:47:11 | 54245.1876041667 | 2007-05-25 04:30:09 | 702004010 | 55.227 | 50 | 55.227 | 55.227 | 0 | 55.227 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.255 | 48.255 | 121.3699 | 4 | PROCESSED | 57538.7560416667 | 2016-05-30 18:08:42 | 54745 | 2008-10-06 00:00:00 | 54255.6532986111 | 2007-06-04 15:40:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702004010/ | Quick Look | ![]() |
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869 | N132D | 81.4727 | -69.6025 | 81.573639 | -69.643574 | 312.317041 | -85.606179 | 280.24276086 | -32.71811202 | 53.1485 | 53597.9869444444 | 2005-08-15 23:41:12 | 53598.2398958333 | 2005-08-16 05:45:27 | 100002050 | 0 | 7 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6873263889 | 2016-05-12 16:29:45 | 54247 | 2007-05-27 00:00:00 | 54230.4157291667 | 2007-05-10 09:58:39 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD HV ON WITH N132D | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002050/ | Quick Look | ![]() |
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870 | WR140 | 305.1135 | 43.9272 | 304.692033 | 43.76792 | 327.425445 | 60.56194 | 80.98919394 | 4.21991141 | 90.2945 | 54565.231400463 | 2008-04-09 05:33:13 | 54565.7224305556 | 2008-04-09 17:20:18 | 403033010 | 21.6253 | 20 | 21.6253 | 21.6253 | 0 | 21.6253 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.6055 | 18.6055 | 42.4159 | 2 | PROCESSED | 57542.2656828704 | 2016-06-03 06:22:35 | 54953 | 2009-05-02 00:00:00 | 54580.4185648148 | 2008-04-24 10:02:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITOMO MAEDA | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403033010/ | Quick Look | ![]() |
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871 | GALACTIC CENTER GC11 | 266.231 | -29.8182 | 265.431151 | -29.797955 | 266.700372 | -6.420209 | 359.16839231 | -0.33075371 | 109.7993 | 54172.6536111111 | 2007-03-13 15:41:12 | 54173.2086111111 | 2007-03-14 05:00:24 | 501056010 | 26.5374 | 25 | 26.5454 | 26.5454 | 0 | 26.5374 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2789 | 25.2789 | 47.946 | 0 | PROCESSED | 57537.6702199074 | 2016-05-29 16:05:07 | 54736 | 2008-09-27 00:00:00 | 54182.3328125 | 2007-03-23 07:59:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501056010/ | Quick Look | ![]() |
872 | 1RXSJ013106.4+612035 | 22.8032 | 61.3371 | 21.96963 | 61.079753 | 49.605162 | 46.981158 | 127.68400105 | -1.16712133 | 215.0025 | 55993.5664930556 | 2012-03-07 13:35:45 | 55993.889837963 | 2012-03-07 21:21:22 | 406034020 | 12.1737 | 8 | 12.1737 | 12.1737 | 0 | 12.1737 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.897 | 17.897 | 27.9219 | 0 | PROCESSED | 57604.8011574074 | 2016-08-04 19:13:40 | 56374 | 2013-03-23 00:00:00 | 56008.1191782407 | 2012-03-22 02:51:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMITSU TAKAHASHI | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406034020/ | Quick Look | ![]() |
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873 | FORNAX A W-LOBE S | 50.358 | -37.3109 | 49.88075 | -37.489463 | 32.300433 | -53.110983 | 240.40250552 | -56.92779805 | 62.5011 | 55012.4989930556 | 2009-06-30 11:58:33 | 55013.9619675926 | 2009-07-01 23:05:14 | 804038010 | 52.4253 | 50 | 52.4333 | 52.4333 | 0 | 52.4253 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.7121 | 11.7121 | 36.36 | 1 | PROCESSED | 57547.7267013889 | 2016-06-08 17:26:27 | 55393 | 2010-07-16 00:00:00 | 55026.4458564815 | 2009-07-14 10:42:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MAKOTO TASHIRO | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804038010/ | Quick Look | ![]() |
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874 | 4U 0142+61 | 26.4803 | 61.7944 | 25.612931 | 61.544346 | 52.126454 | 46.446482 | 129.32255084 | -0.39946076 | 40.959 | 54325.1695949074 | 2007-08-13 04:04:13 | 54327.5209259259 | 2007-08-15 12:30:08 | 402013010 | 99.6744 | 100 | 99.6744 | 99.6744 | 0 | 99.6744 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101.6096 | 101.6096 | 203.1297 | 4 | PROCESSED | 57549.823900463 | 2016-06-10 19:46:25 | 54730 | 2008-09-21 00:00:00 | 54347.6221296296 | 2007-09-04 14:55:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TERUAKI ENOTO | JAP | 2 | AO2 | THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402013010/ | Quick Look | ![]() |
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875 | PSR B1259-63 | 195.6594 | -63.8834 | 194.870087 | -63.614735 | 227.713942 | -50.940493 | 304.16424752 | -1.0384525 | 292.9998 | 54330.0581481482 | 2007-08-18 01:23:44 | 54330.6877777778 | 2007-08-18 16:30:24 | 402014070 | 20.4812 | 20 | 20.4812 | 20.4812 | 0 | 20.4829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4703 | 19.4703 | 54.364 | 0 | PROCESSED | 57539.6 | 2016-05-31 14:24:00 | 54724 | 2008-09-15 00:00:00 | 54356.2228472222 | 2007-09-13 05:20:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014070/ | Quick Look | ![]() |
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876 | GC_LARGEPROJECT7 | 265.6744 | -30.0704 | 264.873054 | -30.047455 | 266.222278 | -6.685926 | 358.7007591 | -0.05229538 | 265.9998 | 54725.0356365741 | 2008-09-16 00:51:19 | 54727.1975 | 2008-09-18 04:44:24 | 503013010 | 104.769 | 100 | 104.777 | 104.777 | 0 | 104.769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.9013 | 93.9013 | 186.7098 | 3 | PROCESSED | 57543.8883564815 | 2016-06-04 21:19:14 | 54557 | 2008-04-01 00:00:00 | 54780.5885532407 | 2008-11-10 14:07:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503013010/ | Quick Look | ![]() |
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877 | VELA JR P4 | 132.5157 | -45.5453 | 132.084337 | -45.3579 | 158.164513 | -59.340232 | 265.43667302 | -0.97855833 | 347.0031 | 54286.1062847222 | 2007-07-05 02:33:03 | 54286.4480787037 | 2007-07-05 10:45:14 | 502026010 | 10.9724 | 10 | 10.9724 | 10.9724 | 0 | 10.9724 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.2959 | 11.2959 | 29.5119 | 1 | PROCESSED | 57539.0994791667 | 2016-05-31 02:23:15 | 54759 | 2008-10-20 00:00:00 | 54328.4405787037 | 2007-08-16 10:34:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502026010/ | Quick Look | ![]() |
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878 | GC_LARGEPROJECT12 | 264.5602 | -31.5978 | 263.749148 | -31.569439 | 265.310572 | -8.245043 | 356.8985011 | -0.05173107 | 288.0843 | 54733.394375 | 2008-09-24 09:27:54 | 54733.9377777778 | 2008-09-24 22:30:24 | 503018010 | 29.4012 | 50 | 29.4125 | 29.4125 | 0 | 29.4012 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.6716 | 26.6716 | 46.942 | 0 | PROCESSED | 57543.9951851852 | 2016-06-04 23:53:04 | 54557 | 2008-04-01 00:00:00 | 54780.4814583333 | 2008-11-10 11:33:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018010/ | Quick Look | ![]() |
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879 | GC_LARGEPROJECT14 | 264.2413 | -32.0163 | 263.427554 | -31.98639 | 265.053396 | -8.67384 | 356.39993487 | -0.04727305 | 95.7088 | 54883.0527199074 | 2009-02-21 01:15:55 | 54884.7911342593 | 2009-02-22 18:59:14 | 503020010 | 61.0441 | 50 | 61.0681 | 61.0441 | 0 | 61.0601 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.7185 | 51.7185 | 150.1319 | 1 | PROCESSED | 57545.6307175926 | 2016-06-06 15:08:14 | 54557 | 2008-04-01 00:00:00 | 54895.6029166667 | 2009-03-05 14:28:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503020010/ | Quick Look | ![]() |
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880 | MARS-P10 | 103.2518 | 25.125 | 102.483772 | 25.186994 | 101.989505 | 2.233931 | 190.42954859 | 11.48582895 | 298.135 | 54560.0767708333 | 2008-04-04 01:50:33 | 54560.16 | 2008-04-04 03:50:24 | 403006100 | 3.7716 | 100 | 3.7956 | 3.7716 | 0 | 3.796 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.0014 | 4.0014 | 7.1839 | 0 | PROCESSED | 57542.0546527778 | 2016-06-03 01:18:42 | 54953 | 2009-05-02 00:00:00 | 54577.1537847222 | 2008-04-21 03:41:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006100/ | Quick Look | ![]() |
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881 | GX 339-4 | 255.7297 | -48.7352 | 254.782436 | -48.66432 | 259.586148 | -25.80756 | 338.99220289 | -4.30584956 | 108.3513 | 54920.4773958333 | 2009-03-30 11:27:27 | 54921.5216435185 | 2009-03-31 12:31:10 | 403011030 | 39.6384 | 40 | 39.6633 | 39.6384 | 0 | 39.6633 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0686 | 35.0686 | 90.186 | 0 | PROCESSED | 57545.9795601852 | 2016-06-06 23:30:34 | 55330 | 2010-05-14 00:00:00 | 54931.0610416667 | 2009-04-10 01:27:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011030/ | Quick Look | ![]() |
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882 | VELA JR P21 | 133.1972 | -46.3295 | 132.769289 | -46.139656 | 159.781258 | -59.750169 | 266.34323773 | -1.11269222 | 347.0005 | 54651.5833680556 | 2008-07-04 14:00:03 | 54652.0557175926 | 2008-07-05 01:20:14 | 503033010 | 14.2872 | 10 | 14.2952 | 14.2872 | 0 | 14.3032 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.0665 | 12.0665 | 40.8019 | 1 | PROCESSED | 57542.9629398148 | 2016-06-03 23:06:38 | 55036 | 2009-07-24 00:00:00 | 54665.3234375 | 2008-07-18 07:45:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503033010/ | Quick Look | ![]() |
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883 | VELA JR P36 | 133.0606 | -47.2239 | 132.639922 | -47.034529 | 160.606122 | -60.550234 | 266.97132611 | -1.75647675 | 346.9998 | 54656.5145833333 | 2008-07-09 12:21:00 | 54656.9168634259 | 2008-07-09 22:00:17 | 503048010 | 11.1226 | 10 | 11.1306 | 11.1226 | 0 | 11.1386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.3838 | 9.3838 | 34.7499 | 1 | PROCESSED | 57543.0132175926 | 2016-06-04 00:19:02 | 55037 | 2009-07-25 00:00:00 | 54670.2692361111 | 2008-07-23 06:27:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503048010/ | Quick Look | ![]() |
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884 | IRAS 05262+4432 | 82.4599 | 44.6406 | 81.547278 | 44.601887 | 84.24873 | 21.350791 | 165.01766257 | 5.72021917 | 78.2999 | 54721.6357523148 | 2008-09-12 15:15:29 | 54723.406412037 | 2008-09-14 09:45:14 | 703019010 | 82.086 | 80 | 82.0975 | 82.094 | 0 | 82.086 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.9075 | 70.9075 | 152.9541 | 0 | PROCESSED | 57543.8409490741 | 2016-06-04 20:10:58 | 55148 | 2009-11-13 00:00:00 | 54780.4562037037 | 2008-11-10 10:56:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITO HABA | JAP | 3 | AO3 | SUZAKU VIEW OF OBSCURED NARROW-LINE SEYFERT 1 GALAXY IRAS 05262+4432 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703019010/ | Quick Look | ![]() |
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885 | MARS-P24 | 103.8389 | 25.0556 | 103.07157 | 25.120373 | 102.525763 | 2.214408 | 190.72046804 | 11.94011608 | 298.3401 | 54561.2433680556 | 2008-04-05 05:50:27 | 54561.3265509259 | 2008-04-05 07:50:14 | 403006240 | 3.423 | 100 | 3.423 | 3.423 | 0 | 3.423 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.511 | 2.511 | 7.1839 | 0 | PROCESSED | 57542.0844328704 | 2016-06-03 02:01:35 | 54953 | 2009-05-02 00:00:00 | 54578.1234375 | 2008-04-22 02:57:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006240/ | Quick Look | ![]() |
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886 | CYGNUS LOOP (P23) | 312.4772 | 32.3587 | 311.966597 | 32.171629 | 327.828669 | 47.6396 | 75.1675214 | -7.32455162 | 61.8892 | 54620.7530439815 | 2008-06-03 18:04:23 | 54621.1473842593 | 2008-06-04 03:32:14 | 503059010 | 19.457 | 15 | 19.457 | 19.457 | 0 | 19.457 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.2771 | 17.2771 | 34.0639 | 0 | PROCESSED | 57542.7106944444 | 2016-06-03 17:03:24 | 55003 | 2009-06-21 00:00:00 | 54636.2328240741 | 2008-06-19 05:35:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503059010/ | Quick Look | ![]() |
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887 | GX 339-4 | 255.6944 | -48.7333 | 254.747207 | -48.662254 | 259.560211 | -25.808209 | 338.97952784 | -4.28620483 | 84.7264 | 54908.0786226852 | 2009-03-18 01:53:13 | 54908.9613310185 | 2009-03-18 23:04:19 | 403011010 | 43.0408 | 40 | 43.0554 | 43.0408 | 0 | 43.0614 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.3914 | 35.3914 | 76.2579 | 1 | PROCESSED | 57545.8736458333 | 2016-06-06 20:58:03 | 55330 | 2010-05-14 00:00:00 | 54917.4333796296 | 2009-03-27 10:24:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403011010/ | Quick Look | ![]() |
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888 | ABELL 2199 CENTER | 247.1922 | 39.484 | 246.76294 | 39.592842 | 233.179095 | 60.039777 | 62.84241749 | 43.66620611 | 252.3681 | 54009.2972222222 | 2006-10-01 07:08:00 | 54009.8967361111 | 2006-10-01 21:31:18 | 801056010 | 24.9282 | 25 | 25.4799 | 24.9282 | 25.4799 | 25.4799 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.519 | 20.519 | 51.7939 | 1 | PROCESSED | 57535.7247453704 | 2016-05-27 17:23:38 | 54735 | 2008-09-26 00:00:00 | 54021.2246990741 | 2006-10-13 05:23:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801056010/ | Quick Look | ![]() |
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889 | VW HYI | 62.3036 | -71.2936 | 62.394189 | -71.422866 | 322.02345 | -79.107148 | 284.88553906 | -38.13260514 | 212.7427 | 55924.6383796296 | 2011-12-29 15:19:16 | 55925.1806828704 | 2011-12-30 04:20:11 | 406009020 | 16.1593 | 20 | 16.1593 | 16.1593 | 0 | 16.1593 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.7587 | 13.7587 | 46.8519 | 0 | PROCESSED | 57604.2667939815 | 2016-08-04 06:24:11 | 56313 | 2013-01-21 00:00:00 | 55945.9133912037 | 2012-01-19 21:55:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009020/ | Quick Look | ![]() |
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890 | CYGNUS LOOP (P28) | 313.4797 | 29.8934 | 312.955126 | 29.702774 | 327.568716 | 45.03529 | 73.77252886 | -9.54040793 | 49.1005 | 54600.0501273148 | 2008-05-14 01:12:11 | 54600.5334953704 | 2008-05-14 12:48:14 | 503064010 | 18.1693 | 15 | 18.1773 | 18.1853 | 0 | 18.1693 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.443 | 16.443 | 41.756 | 0 | PROCESSED | 57542.5291898148 | 2016-06-03 12:42:02 | 54975 | 2009-05-24 00:00:00 | 54609.1904282407 | 2008-05-23 04:34:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503064010/ | Quick Look | ![]() |
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891 | IGR J17303-0601 | 262.5864 | -5.9814 | 261.916828 | -5.94387 | 262.267561 | 17.260409 | 17.93788623 | 15.02149808 | 100.7922 | 54878.4233217593 | 2009-02-16 10:09:35 | 54879.3355787037 | 2009-02-17 08:03:14 | 403026010 | 32.9635 | 30 | 32.9635 | 32.9635 | 0 | 32.9635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.7559 | 27.7559 | 78.818 | 2 | PROCESSED | 57545.5746990741 | 2016-06-06 13:47:34 | 55325 | 2010-05-09 00:00:00 | 54893.4381018518 | 2009-03-03 10:30:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403026010/ | Quick Look | ![]() |
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892 | AE AQUARII | 310.0451 | -0.9346 | 309.400522 | -1.112531 | 312.21962 | 16.830556 | 45.22328928 | -24.45613885 | 265.1622 | 55120.7618518518 | 2009-10-16 18:17:04 | 55124.2265393518 | 2009-10-20 05:26:13 | 404001010 | 160.4546 | 160 | 161.4519 | 161.7209 | 0 | 160.4546 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136.0715 | 136.0715 | 299.3277 | 3 | PROCESSED | 57548.9948958333 | 2016-06-09 23:52:39 | 55503 | 2010-11-03 00:00:00 | 55134.5588194444 | 2009-10-30 13:24:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | JAP | 4 | AO4 | SUZAKU, H.E.S.S., OPTICAL SIMULTANEOUS OBSERVATION OF THE WHITE DWARF PULSAR, AE AQUARII | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404001010/ | Quick Look | ![]() |
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893 | Z CAM | 126.2993 | 73.0997 | 124.910098 | 73.261749 | 106.122719 | 51.687472 | 141.39550179 | 32.62975748 | 289.0998 | 54931.1187152778 | 2009-04-10 02:50:57 | 54931.9092476852 | 2009-04-10 21:49:19 | 404022010 | 37.663 | 35 | 37.663 | 37.663 | 0 | 37.663 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.5329 | 36.5329 | 68.2899 | 0 | PROCESSED | 57546.1159722222 | 2016-06-07 02:47:00 | 55324 | 2010-05-08 00:00:00 | 54949.4517824074 | 2009-04-28 10:50:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404022010/ | Quick Look | ![]() |
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894 | NGC 4686 | 191.5508 | 54.5121 | 190.986823 | 54.785056 | 159.09559 | 52.489361 | 124.58283765 | 62.59936814 | 342.6621 | 54946.7002777778 | 2009-04-25 16:48:24 | 54947.7564699074 | 2009-04-26 18:09:19 | 704015010 | 44.8459 | 40 | 44.8539 | 44.8459 | 0 | 44.8459 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.3275 | 42.3275 | 91.232 | 0 | PROCESSED | 57546.4795717593 | 2016-06-07 11:30:35 | 55339 | 2010-05-23 00:00:00 | 54973.9296875 | 2009-05-22 22:18:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704015010/ | Quick Look | ![]() |
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895 | 3C 35 | 18.0181 | 49.4424 | 17.27928 | 49.177164 | 38.209927 | 38.103766 | 126.37585323 | -13.29131796 | 245.0044 | 55200.6165509259 | 2010-01-04 14:47:50 | 55202.466875 | 2010-01-06 11:12:18 | 704019010 | 84.7566 | 80 | 85.0286 | 84.7566 | 0 | 85.0206 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66.3143 | 66.3143 | 147.5778 | 2 | PROCESSED | 57550.0615277778 | 2016-06-11 01:28:36 | 55584 | 2011-01-23 00:00:00 | 55218.1479050926 | 2010-01-22 03:32:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 4 | AO4 | SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704019010/ | Quick Look | ![]() |
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896 | AO PSC | 343.7945 | -3.1271 | 343.149274 | -3.394015 | 343.859558 | 3.486369 | 68.69841137 | -53.28578539 | 60.9461 | 55004.4934143518 | 2009-06-22 11:50:31 | 55005.3328587963 | 2009-06-23 07:59:19 | 404033010 | 39.6544 | 40 | 39.6544 | 39.6624 | 0 | 39.6624 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.6834 | 35.6834 | 72.5179 | 0 | PROCESSED | 57547.6306481482 | 2016-06-08 15:08:08 | 55385 | 2010-07-08 00:00:00 | 55018.165474537 | 2009-07-06 03:58:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404033010/ | Quick Look | ![]() |
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897 | 1150+497 | 178.3624 | 49.5318 | 177.710529 | 49.809967 | 153.770918 | 43.67464 | 145.51949415 | 64.97605225 | 131.4133 | 55512.7136805556 | 2010-11-12 17:07:42 | 55514.1042824074 | 2010-11-14 02:30:10 | 705003010 | 105.6558 | 100 | 105.7118 | 105.6558 | 0 | 105.7198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.6438 | 84.6438 | 120.128 | 1 | PROCESSED | 57554.1053356482 | 2016-06-15 02:31:41 | 55892 | 2011-11-27 00:00:00 | 55524.2197337963 | 2010-11-24 05:16:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMI SETA | JAP | 5 | AO5 | SUZAKU OBSERVATION OF AN FE-LINE BLAZAR 1150+497 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705003010/ | Quick Look | ![]() |
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898 | GC SGR D NORTH | 266.9758 | -27.7178 | 266.189062 | -27.7012 | 267.305981 | -4.305004 | 1.30220378 | 0.20283685 | 108.7992 | 54173.2100578704 | 2007-03-14 05:02:29 | 54174.7883564815 | 2007-03-15 18:55:14 | 501058010 | 63.2422 | 63 | 63.2502 | 63.2422 | 0 | 63.2582 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.1479 | 51.1479 | 136.3519 | 0 | PROCESSED | 57537.7302546296 | 2016-05-29 17:31:34 | 54735 | 2008-09-26 00:00:00 | 54182.440462963 | 2007-03-23 10:34:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501058010/ | Quick Look | ![]() |
899 | ASO0431 | 286.9632 | 6.0295 | 286.350421 | 5.949691 | 289.23811 | 28.344266 | 40.16756672 | -0.88470452 | 90.0004 | 54936.153287037 | 2009-04-15 03:40:44 | 54936.8141666667 | 2009-04-15 19:32:24 | 504043010 | 24.5222 | 20 | 24.5222 | 24.5222 | 0 | 24.5222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.105 | 18.105 | 57.0739 | 0 | PROCESSED | 57546.1491087963 | 2016-06-07 03:34:43 | 55324 | 2010-05-08 00:00:00 | 54949.5652777778 | 2009-04-28 13:34:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504043010/ | Quick Look | ![]() |
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900 | EMS1535 | 345.6918 | 44.7374 | 345.120256 | 44.468031 | 9.799428 | 45.696922 | 103.4061071 | -13.97501662 | 63.3944 | 55373.2448611111 | 2010-06-26 05:52:36 | 55374.0174768518 | 2010-06-27 00:25:10 | 705016010 | 42.3955 | 40 | 42.4035 | 42.3955 | 0 | 42.4035 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.7545 | 42.7545 | 66.7539 | 0 | PROCESSED | 57552.4062268518 | 2016-06-13 09:44:58 | 55772 | 2011-07-30 00:00:00 | 55404.2240625 | 2010-07-27 05:22:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705016010/ | Quick Look | ![]() |
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901 | SCO X-1 | 245.0164 | -15.3926 | 244.30666 | -15.273445 | 245.822043 | 5.976116 | 359.32713596 | 23.91560488 | 98.4296 | 57090.7847685185 | 2015-03-09 18:50:04 | 57093.0903703704 | 2015-03-12 02:10:08 | 409025010 | 84.7086 | 50 | 0 | 0 | 0 | 84.7086 | 0 | 0 | 0 | 1 | 1 | 0 | 0 | 35.3772 | 35.3772 | 194.5699 | 0 | PROCESSED | 57617.8306365741 | 2016-08-17 19:56:07 | 57481 | 2016-04-03 00:00:00 | 57115.4052777778 | 2015-04-03 09:43:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090108 | We propose 50 ks observation of the bright LMXB Sco X-1 (Z source) to search high energy emission above 50 keV and study Fe-K emission/absorption lines. With the combination of XIS and HXD, these properties can be studied with identifying the state of the source. Since Sco X-1 is so bright, the pointing is offset by ~15 arcmin from XIS nominal position. | GALACTIC POINT SOURCES | 4 | A | HIROMITSU TAKAHASHI | JAP | 9 | AO9 | SUZAKU OBSERVATION OF THE BRIGHTEST LMXB SCO X-1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409025010/ | Quick Look | ![]() |
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902 | SAGITTARIUS A* | 266.4154 | -29.0072 | 265.620691 | -28.987862 | 266.840925 | -5.605376 | 359.94411521 | -0.04477398 | 105.699 | 56752.451400463 | 2014-04-05 10:50:01 | 56752.9848611111 | 2014-04-05 23:38:12 | 408017090 | 22.1668 | 20 | 22.1668 | 23.5591 | 0 | 23.5701 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8745 | 18.8745 | 46.0878 | 1 | PROCESSED | 57614.1690740741 | 2016-08-14 04:03:28 | 57134 | 2015-04-22 00:00:00 | 56768.7215856482 | 2014-04-21 17:19:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017090/ | Quick Look | ![]() |
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903 | PSR J2055+2539 | 313.957 | 25.6505 | 313.412506 | 25.458222 | 325.920666 | 40.944888 | 70.67687842 | -12.53222207 | 262.3229 | 55498.1479398148 | 2010-10-29 03:33:02 | 55498.9578356482 | 2010-10-29 22:59:17 | 405015010 | 31.1069 | 30 | 31.1069 | 31.1069 | 0 | 31.1069 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.4581 | 21.4581 | 69.9679 | 0 | PROCESSED | 57553.8967592593 | 2016-06-14 21:31:20 | 55890 | 2011-11-25 00:00:00 | 55523.9927314815 | 2010-11-23 23:49:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405015010/ | Quick Look | ![]() |
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904 | RXJ1713-3946 | 257.9704 | -39.5791 | 257.105134 | -39.519003 | 260.343852 | -16.539668 | 347.29183097 | -0.10508063 | 267.9995 | 53989.172025463 | 2006-09-11 04:07:43 | 53989.5306365741 | 2006-09-11 12:44:07 | 501063010 | 18.422 | 20 | 18.422 | 18.422 | 18.422 | 18.422 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.7597 | 17.7597 | 30.9719 | 1 | PROCESSED | 57535.5249537037 | 2016-05-27 12:35:56 | 54526 | 2008-03-01 00:00:00 | 54021.1086458333 | 2006-10-13 02:36:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501063010/ | Quick Look | ![]() |
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905 | RIM5 | 311.5286 | 30.6813 | 311.011535 | 30.497677 | 325.775502 | 46.411023 | 73.33464134 | -7.73161485 | 255.8951 | 55155.3611689815 | 2009-11-20 08:40:05 | 55155.7953356482 | 2009-11-20 19:05:17 | 504009010 | 15.8502 | 15 | 15.8502 | 15.8502 | 0 | 15.8502 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2891 | 12.2891 | 37.5039 | 0 | PROCESSED | 57549.4934259259 | 2016-06-10 11:50:32 | 55534 | 2010-12-04 00:00:00 | 55166.4265277778 | 2009-12-01 10:14:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504009010/ | Quick Look | ![]() |
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906 | SWIFT J1834.9-0846 | 278.7285 | -8.7724 | 278.045132 | -8.813015 | 278.89774 | 14.398942 | 23.24882887 | -0.35409613 | 264.9986 | 56582.3041319444 | 2013-10-17 07:17:57 | 56583.3335300926 | 2013-10-18 08:00:17 | 408015010 | 35.9317 | 40 | 38.1117 | 38.1117 | 0 | 35.9317 | 2 | 2 | 0 | 3 | 1 | 0 | 0 | 31.9264 | 31.9264 | 88.9319 | 1 | PROCESSED | 57613.0148726852 | 2016-08-13 00:21:25 | 56967 | 2014-11-06 00:00:00 | 56601.6309953704 | 2013-11-05 15:08:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080040 | Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. | GALACTIC POINT SOURCES | 4 | B | TERUAKI ENOTO | JAP | 8 | AO8 | ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408015010/ | Quick Look | ![]() |
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907 | NGC6251_LOBE | 246.4248 | 82.6439 | 247.78516 | 82.752174 | 100.137256 | 73.058322 | 116.00587189 | 31.32598662 | 26.9674 | 55666.2760069444 | 2011-04-15 06:37:27 | 55667.0258564815 | 2011-04-16 00:37:14 | 706003010 | 38.0779 | 40 | 38.0779 | 38.0779 | 0 | 38.0779 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.5276 | 37.5276 | 64.784 | 0 | PROCESSED | 57601.5103356482 | 2016-08-01 12:14:53 | 56058 | 2012-05-11 00:00:00 | 55690.9897685185 | 2011-05-09 23:45:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706003010/ | Quick Look | ![]() |
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908 | NGC6251_LOBE_BGD2 | 245.3877 | 82.3337 | 246.650515 | 82.446813 | 101.124392 | 73.239187 | 115.79036875 | 31.61025625 | 299.99 | 55789.4176967593 | 2011-08-16 10:01:29 | 55789.6225 | 2011-08-16 14:56:24 | 706005020 | 11.178 | 10 | 11.178 | 11.178 | 0 | 11.178 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.788 | 9.788 | 17.6879 | 0 | PROCESSED | 57602.7824421296 | 2016-08-02 18:46:43 | 56173 | 2012-09-03 00:00:00 | 55805.1871527778 | 2011-09-01 04:29:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706005020/ | Quick Look | ![]() |
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909 | PSR J0726-2612 | 111.531 | -26.2114 | 111.017873 | -26.110384 | 119.169713 | -47.49417 | 240.07877209 | -4.64696128 | 117.9984 | 55881.5691782407 | 2011-11-16 13:39:37 | 55882.6252546296 | 2011-11-17 15:00:22 | 406012010 | 43.757 | 100 | 43.757 | 43.792 | 0 | 43.792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.7288 | 39.7288 | 91.2278 | 0 | PROCESSED | 57603.8172685185 | 2016-08-03 19:36:52 | 56264 | 2012-12-03 00:00:00 | 55895.2388078704 | 2011-11-30 05:43:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINPEI SHIBATA | JAP | 6 | AO6 | CAN HIGH MAGNETIC FIELD RADIO PULSARS BE THE MAGNETAR ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406012010/ | Quick Look | ![]() |
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910 | A2142 OFFSET1 | 239.3897 | 27.3899 | 238.873146 | 27.532705 | 228.881511 | 46.554196 | 44.41448178 | 48.88746657 | 283.7323 | 54316.0523726852 | 2007-08-04 01:15:25 | 54317.0211226852 | 2007-08-05 00:30:25 | 802030010 | 37.6227 | 30 | 37.6307 | 37.6227 | 0 | 37.6307 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.6677 | 29.6677 | 83.6879 | 1 | PROCESSED | 57539.4231134259 | 2016-05-31 10:09:17 | 54723 | 2008-09-14 00:00:00 | 54347.3816087963 | 2007-09-04 09:09:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYA OHASHI | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802030010/ | Quick Look | ![]() |
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911 | MRK 520 | 330.1768 | 10.545 | 329.561779 | 10.304216 | 336.215385 | 21.249415 | 69.38972894 | -34.038497 | 250.5002 | 56258.8186458333 | 2012-11-27 19:38:51 | 56260.6571412037 | 2012-11-29 15:46:17 | 407014010 | 79.7795 | 80 | 79.7795 | 79.7875 | 0 | 79.7955 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.641 | 77.641 | 158.8258 | 1 | PROCESSED | 57608.1523263889 | 2016-08-08 03:39:21 | 56644 | 2013-12-18 00:00:00 | 56275.7255555556 | 2012-12-14 17:24:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEIKO MATSUTA | JAP | 7 | AO7 | MRK 520 : A NEW COMPTON-THICK AGN? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407014010/ | Quick Look | ![]() |
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912 | IGR J17091-3624 | 257.2807 | -36.4071 | 256.440218 | -36.343795 | 259.493682 | -13.428104 | 349.52434208 | 2.21333885 | 90.7245 | 56342.7065162037 | 2013-02-19 16:57:23 | 56344.8856828704 | 2013-02-21 21:15:23 | 407037020 | 81.9467 | 80 | 81.9467 | 81.9467 | 0 | 81.9467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.871 | 72.871 | 188.26 | 1 | PROCESSED | 57610.6944212963 | 2016-08-10 16:39:58 | 56728 | 2014-03-12 00:00:00 | 56363.6146990741 | 2013-03-12 14:45:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUTAKA YAMAOKA | JAP | 7 | AO7 | SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407037020/ | Quick Look | ![]() |
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913 | ANTLIA CLUSTER | 157.5092 | -35.3277 | 156.944615 | -35.070958 | 175.726148 | -40.891834 | 272.94647188 | 19.18131972 | 90.0004 | 54423.2458796296 | 2007-11-19 05:54:04 | 54425.0211111111 | 2007-11-21 00:30:24 | 802035010 | 65.9528 | 60 | 65.9608 | 65.9608 | 0 | 65.9528 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.1064 | 58.1064 | 153.3638 | 2 | PROCESSED | 57540.5835185185 | 2016-06-01 14:00:16 | 54801 | 2008-12-01 00:00:00 | 54433.3905092593 | 2007-11-29 09:22:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAO KITAGUCHI | JAP | 2 | AO2 | SUZAKU OBSERVATION OF NON-CD ANTLIA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802035010/ | Quick Look | ![]() |
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914 | SWIFT J0709.4-3559 | 107.3109 | -36.0226 | 106.863563 | -35.940797 | 116.901156 | -57.856606 | 247.327711 | -12.25710974 | 260.0142 | 55653.0945601852 | 2011-04-02 02:16:10 | 55655.0640393518 | 2011-04-04 01:32:13 | 706008010 | 81.1739 | 80 | 81.1739 | 81.1739 | 0 | 81.1739 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.4621 | 61.4621 | 170.1239 | 2 | PROCESSED | 57601.393287037 | 2016-08-01 09:26:20 | 56037 | 2012-04-20 00:00:00 | 55670.2451967593 | 2011-04-19 05:53:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 6 | AO6 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706008010/ | Quick Look | ![]() |
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915 | ASO0304 | 213.3355 | -62.0808 | 212.410984 | -61.846899 | 236.335934 | -45.096122 | 312.3597658 | -0.71761471 | 280.2937 | 55036.9044907407 | 2009-07-24 21:42:28 | 55038.1453935185 | 2009-07-26 03:29:22 | 504054010 | 44.2485 | 40 | 44.2485 | 44.2485 | 0 | 44.2485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0839 | 41.0839 | 107.2018 | 1 | PROCESSED | 57547.9369791667 | 2016-06-08 22:29:15 | 55415 | 2010-08-07 00:00:00 | 55048.3203819444 | 2009-08-05 07:41:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504054010/ | Quick Look | ![]() |
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916 | X 1630-472 | 248.5014 | -47.3935 | 247.58039 | -47.289358 | 254.085874 | -25.131659 | 336.90846442 | 0.25253242 | 88.6317 | 57073.2374884259 | 2015-02-20 05:41:59 | 57074.4111805556 | 2015-02-21 09:52:06 | 409007010 | 6.1528 | 40 | 6.165 | 6.1823 | 0 | 6.1528 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6570023148 | 2016-08-17 15:46:05 | 57454 | 2016-03-07 00:00:00 | 57087.4573032407 | 2015-03-06 10:58:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | 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 | YOSHIHIRO UEDA | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409007010/ | Quick Look | ![]() |
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917 | AWM7 EAST OFFSET | 44.9753 | 41.5792 | 44.161968 | 41.380907 | 54.762228 | 23.48981 | 147.26183994 | -15.14450792 | 259.3934 | 54492.7386458333 | 2008-01-27 17:43:39 | 54494.7016087963 | 2008-01-29 16:50:19 | 802044010 | 85.6177 | 80 | 85.6177 | 85.6177 | 0 | 85.6177 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.6003 | 80.6003 | 169.5838 | 1 | PROCESSED | 57541.4783333333 | 2016-06-02 11:28:48 | 54888 | 2009-02-26 00:00:00 | 54515.5758796296 | 2008-02-19 13:49:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA ISHISAKI | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802044010/ | Quick Look | ![]() |
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918 | 4U 0614+091 | 94.2788 | 9.1363 | 93.59351 | 9.155405 | 94.360649 | -14.24001 | 200.87717258 | -3.36522944 | 89.7995 | 56579.4227314815 | 2013-10-14 10:08:44 | 56580.8314351852 | 2013-10-15 19:57:16 | 408009010 | 33.687 | 60 | 33.687 | 34.6474 | 0 | 34.9366 | 3 | 4 | 0 | 4 | 1 | 0 | 0 | 57.7016 | 57.7016 | 121.6639 | 0 | PROCESSED | 57612.9715393518 | 2016-08-12 23:19:01 | 57144 | 2015-05-02 00:00:00 | 56601.6144791667 | 2013-11-05 14:44:51 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080028 | We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB. | GALACTIC POINT SOURCES | 4 | B | SATOSHI SUGITA | JAP | 8 | AO8 | THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408009010/ | Quick Look | ![]() |
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919 | SAGITTARIUS A* | 266.415 | -29.006 | 265.620299 | -28.98666 | 266.840543 | -5.604185 | 359.94495727 | -0.04385023 | 107.0004 | 56744.9007523148 | 2014-03-28 21:37:05 | 56745.6238541667 | 2014-03-29 14:58:21 | 408017080 | 20.4818 | 20 | 20.4917 | 20.5036 | 0 | 20.4818 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 19.7498 | 19.7498 | 62.4719 | 1 | PROCESSED | 57614.1384837963 | 2016-08-14 03:19:25 | 57121 | 2015-04-09 00:00:00 | 56756.7635185185 | 2014-04-09 18:19:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017080/ | Quick Look | ![]() |
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920 | AWM7 SOUTH OFFSET | 43.219 | 40.631 | 42.416618 | 40.42683 | 53.072384 | 23.000071 | 146.52769464 | -16.61135361 | 257.3934 | 54494.7028703704 | 2008-01-29 16:52:08 | 54496.618275463 | 2008-01-31 14:50:19 | 802045010 | 31.2959 | 0 | 31.3039 | 31.3039 | 0 | 31.2959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.2298 | 78.2298 | 165.4718 | 1 | PROCESSED | 57541.4808796296 | 2016-06-02 11:32:28 | 54888 | 2009-02-26 00:00:00 | 54515.1834837963 | 2008-02-19 04:24:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA ISHISAKI | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802045010/ | Quick Look | ![]() |
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921 | AWM7 45' SOUTH | 43.6476 | 40.9695 | 42.841958 | 40.766746 | 53.522914 | 23.219545 | 146.6593781 | -16.15981584 | 257.4009 | 55974.8888078704 | 2012-02-17 21:19:53 | 55975.6641087963 | 2012-02-18 15:56:19 | 806010010 | 34.3602 | 35 | 34.3602 | 34.3602 | 0 | 34.3602 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.0155 | 32.0155 | 66.978 | 1 | PROCESSED | 57604.6274768518 | 2016-08-04 15:03:34 | 56361 | 2013-03-10 00:00:00 | 55994.9866319444 | 2012-03-08 23:40:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806010010/ | Quick Look | ![]() |
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922 | PG 1322+659 | 200.9787 | 65.7065 | 200.558033 | 65.966727 | 149.375947 | 63.481771 | 117.62442893 | 51.08576313 | 141.5827 | 55892.4154050926 | 2011-11-27 09:58:11 | 55894.0862268518 | 2011-11-29 02:04:10 | 706018010 | 81.6869 | 80 | 81.7109 | 81.6869 | 0 | 81.7109 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.9168 | 78.9168 | 144.3439 | 2 | PROCESSED | 57603.9954513889 | 2016-08-03 23:53:27 | 56274 | 2012-12-13 00:00:00 | 55907.1929282407 | 2011-12-12 04:37:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROAKI SAMESHIMA | JAP | 6 | AO6 | X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706018010/ | Quick Look | ![]() |
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923 | RX J1633+4718 | 248.3661 | 47.3315 | 248.006234 | 47.43491 | 228.796037 | 67.698232 | 73.56753068 | 42.5999019 | 136.9343 | 55939.8747337963 | 2012-01-13 20:59:37 | 55940.8307407407 | 2012-01-14 19:56:16 | 706027030 | 44.1271 | 40 | 44.1271 | 44.1271 | 0 | 44.1271 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.9578 | 38.9578 | 82.592 | 0 | PROCESSED | 57604.3578703704 | 2016-08-04 08:35:20 | 56331 | 2013-02-08 00:00:00 | 55960.228587963 | 2012-02-03 05:29:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027030/ | Quick Look | ![]() |
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924 | V1223 SGR | 283.7576 | -31.1629 | 282.952803 | -31.227217 | 281.857553 | -8.28711 | 4.95796111 | -14.35306818 | 89.5992 | 56757.9023611111 | 2014-04-10 21:39:24 | 56761.5211111111 | 2014-04-14 12:30:24 | 408019020 | 150.7683 | 60 | 150.7763 | 150.7763 | 0 | 150.7683 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 146.3158 | 146.3158 | 312.6057 | 3 | PROCESSED | 57614.3279976852 | 2016-08-14 07:52:19 | 57152 | 2015-05-10 00:00:00 | 56789.7985648148 | 2014-05-12 19:09:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080086 | A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS. | GALACTIC POINT SOURCES | 4 | B | TAKAYUKI YUASA | JAP | 8 | AO8 | DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408019020/ | Quick Look | ![]() |
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925 | 4C+74.26 | 310.7114 | 75.111 | 310.85824 | 74.929178 | 50.846162 | 74.615216 | 108.98584774 | 19.50187948 | 247.6342 | 55888.5409027778 | 2011-11-23 12:58:54 | 55890.613275463 | 2011-11-25 14:43:07 | 706028010 | 101.4125 | 100 | 101.4125 | 101.4125 | 0 | 101.4125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 117.8827 | 117.8827 | 179.0297 | 2 | PROCESSED | 57603.9949074074 | 2016-08-03 23:52:40 | 56269 | 2012-12-08 00:00:00 | 55901.2441203704 | 2011-12-06 05:51:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROFUMI NODA | JAP | 6 | AO6 | STUSY OF BROAD IRON LINE OF 4C+74.26 TO ESTIMATE THE SPIN OF CENTRAL SUPER MASSIVE BLACK HOLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706028010/ | Quick Look | ![]() |
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926 | A2199_FE | 248.2855 | 39.6383 | 247.85907 | 39.742227 | 234.702574 | 60.442801 | 63.09452591 | 42.82923772 | 143.2418 | 56662.5581597222 | 2014-01-05 13:23:45 | 56663.4606944444 | 2014-01-06 11:03:24 | 808051010 | 40.3548 | 40 | 40.3708 | 40.3548 | 0 | 40.3712 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39.8119 | 39.8119 | 77.9679 | 1 | PROCESSED | 57613.7559490741 | 2016-08-13 18:08:34 | 57085 | 2015-03-04 00:00:00 | 56719.7506597222 | 2014-03-03 18:00:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080067 | We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 8 | AO8 | COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808051010/ | Quick Look | ![]() |
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927 | SAGITTARIUS A* | 266.415 | -29.0097 | 265.620276 | -28.99036 | 266.840636 | -5.607884 | 359.94179901 | -0.04577777 | 105.7704 | 57095.3193171296 | 2015-03-14 07:39:49 | 57096.4952777778 | 2015-03-15 11:53:12 | 409011030 | 25.5496 | 20 | 25.5496 | 47.3551 | 0 | 47.3522 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7910763889 | 2016-08-17 18:59:09 | 56748 | 2014-04-01 00:00:00 | 57111.394525463 | 2015-03-30 09:28:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409011030/ | Quick Look | ![]() |
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928 | CYGNUS_LOOP_P12 | 313.7421 | 31.2725 | 313.223564 | 31.080937 | 328.639569 | 46.215284 | 74.99964096 | -8.84356964 | 62.1405 | 53864.7943055556 | 2006-05-09 19:03:48 | 53865.1391087963 | 2006-05-10 03:20:19 | 501029010 | 13.5426 | 10 | 13.5426 | 13.5426 | 13.5426 | 13.5426 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.1567 | 2.1567 | 29.78 | 1 | PROCESSED | 57534.2604166667 | 2016-05-26 06:15:00 | 54394 | 2007-10-21 00:00:00 | 53914.0447916667 | 2006-06-28 01:04:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501029010/ | Quick Look | ![]() |
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929 | 3EGJ1234 1318_1 | 188.0173 | -13.3363 | 187.367898 | -13.060386 | 192.646727 | -9.069223 | 295.70141073 | 49.26333697 | 109.7313 | 54081.3723032407 | 2006-12-12 08:56:07 | 54081.9273032407 | 2006-12-12 22:15:19 | 801031010 | 19.4098 | 20 | 19.4178 | 19.4178 | 0 | 19.4098 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.7228 | 18.7228 | 47.9499 | 1 | PROCESSED | 57536.3099768518 | 2016-05-28 07:26:22 | 54735 | 2008-09-26 00:00:00 | 54094.2359722222 | 2006-12-25 05:39:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOMONORI TOTANI | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801031010/ | Quick Look | ![]() |
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930 | 3EGJ1234 1318_2 | 188.017 | -13.0869 | 187.367769 | -12.810986 | 192.545784 | -8.84065 | 295.65674578 | 49.51103665 | 109.9322 | 54081.9277777778 | 2006-12-12 22:16:00 | 54082.7766087963 | 2006-12-13 18:38:19 | 801032010 | 30.9427 | 30 | 30.9667 | 30.9587 | 0 | 30.9427 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.083 | 26.083 | 73.3339 | 1 | PROCESSED | 57536.3393055556 | 2016-05-28 08:08:36 | 54735 | 2008-09-26 00:00:00 | 54094.2665740741 | 2006-12-25 06:23:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOMONORI TOTANI | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801032010/ | Quick Look | ![]() |
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931 | SNR 0509-67.5 | 77.3855 | -67.5341 | 77.403087 | -67.594899 | 342.98809 | -84.999306 | 278.15788525 | -34.58671131 | 68.6442 | 53965.2623032407 | 2006-08-18 06:17:43 | 53966.1640509259 | 2006-08-19 03:56:14 | 501041010 | 51.2762 | 50 | 51.2762 | 51.2762 | 51.2762 | 51.2762 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50.8294 | 50.8294 | 77.89 | 1 | PROCESSED | 57535.3081365741 | 2016-05-27 07:23:43 | 54526 | 2008-03-01 00:00:00 | 54020.7617592593 | 2006-10-12 18:16:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI NAKAJIMA | JAP | 1 | AO1 | NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501041010/ | Quick Look | ![]() |
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932 | GALACTIC CENTER | 265.9791 | -28.902 | 265.18515 | -28.880549 | 266.454701 | -5.510331 | 359.8343278 | 0.33569605 | 108.8002 | 54169.6271990741 | 2007-03-10 15:03:10 | 54170.1633564815 | 2007-03-11 03:55:14 | 501046010 | 25.211 | 25 | 25.227 | 25.211 | 0 | 25.243 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0087 | 25.0087 | 46.2919 | 0 | PROCESSED | 57537.6350925926 | 2016-05-29 15:14:32 | 54736 | 2008-09-27 00:00:00 | 54179.4773842593 | 2007-03-20 11:27:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501046010/ | Quick Look | ![]() |
933 | GALACTIC CENTER | 265.7083 | -29.9322 | 264.907837 | -29.909421 | 266.247634 | -6.546909 | 358.83372455 | -0.00453222 | 269.0002 | 54017.5695486111 | 2006-10-09 13:40:09 | 54018.2808333333 | 2006-10-10 06:44:24 | 501051010 | 21.869 | 20 | 21.877 | 21.877 | 21.869 | 21.877 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.1322 | 21.1322 | 61.4459 | 0 | PROCESSED | 57535.8166435185 | 2016-05-27 19:35:58 | 54735 | 2008-09-26 00:00:00 | 54053.5109953704 | 2006-11-14 12:15:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501051010/ | Quick Look | ![]() |
934 | W44 | 284.0351 | 1.3886 | 283.400736 | 1.32257 | 285.389988 | 24.082424 | 34.70383121 | -0.41279271 | 90.6817 | 55296.8229513889 | 2010-04-10 19:45:03 | 55298.1591898148 | 2010-04-12 03:49:14 | 505004010 | 61.1433 | 60 | 61.1513 | 61.1433 | 0 | 61.1513 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.7129 | 53.7129 | 115.3999 | 2 | PROCESSED | 57551.2065625 | 2016-06-12 04:57:27 | 55287 | 2010-04-01 00:00:00 | 55313.4281597222 | 2010-04-27 10:16:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505004010/ | Quick Look | ![]() |
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935 | RXJ1713-3946 | 258.5534 | -39.7289 | 257.686429 | -39.671569 | 260.823727 | -16.651038 | 347.43430559 | -0.55631777 | 267.9997 | 53991.0497337963 | 2006-09-13 01:11:37 | 53991.4460300926 | 2006-09-13 10:42:17 | 501068010 | 21.0015 | 20 | 21.0175 | 21.0095 | 21.0015 | 21.0255 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.2093 | 21.2093 | 34.2339 | 1 | PROCESSED | 57535.5599537037 | 2016-05-27 13:26:20 | 54526 | 2008-03-01 00:00:00 | 54021.2424537037 | 2006-10-13 05:49:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501068010/ | Quick Look | ![]() |
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936 | CYGNUS LOOP 8 | 313.6776 | 30.8178 | 313.157016 | 30.626468 | 328.307341 | 45.819556 | 74.60811536 | -9.08900254 | 81.5524 | 55306.7979398148 | 2010-04-20 19:09:02 | 55307.2786689815 | 2010-04-21 06:41:17 | 505016010 | 23.5534 | 21 | 23.5614 | 23.5534 | 0 | 23.5694 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.1989 | 20.1989 | 41.5279 | 0 | PROCESSED | 57551.2800462963 | 2016-06-12 06:43:16 | 55287 | 2010-04-01 00:00:00 | 55364.2401967593 | 2010-06-17 05:45:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505016010/ | Quick Look | ![]() |
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937 | L168_B53 | 153.7378 | 48.0763 | 152.957538 | 48.325063 | 136.571096 | 34.402104 | 167.64470811 | 53.18666692 | 109.5667 | 55519.8069328704 | 2010-11-19 19:21:59 | 55521.5828356482 | 2010-11-21 13:59:17 | 505058010 | 79.4999 | 80 | 79.4999 | 79.4999 | 0 | 79.4999 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.6619 | 35.6619 | 153.4218 | 1 | PROCESSED | 57554.2060763889 | 2016-06-15 04:56:45 | 55898 | 2011-12-03 00:00:00 | 55530.2748842593 | 2010-11-30 06:35:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NORIO SEKIYA | JAP | 5 | AO5 | DARK PATCH IN THE GALACTIC HALO X-RAY EMISSION AND ITS POSSIBLE RELATION TO RADIO SYNCHROTRON RADIATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505058010/ | Quick Look | ![]() |
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938 | DEM L 199 | 81.6473 | -68.8371 | 81.71922 | -68.877404 | 320.411618 | -86.105475 | 279.33316137 | -32.78488249 | 187.7916 | 55551.3246759259 | 2010-12-21 07:47:32 | 55552.146099537 | 2010-12-22 03:30:23 | 505042010 | 51.7434 | 50 | 51.7564 | 51.7434 | 0 | 51.7564 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.2079 | 48.2079 | 70.9659 | 0 | PROCESSED | 57554.4832523148 | 2016-06-15 11:35:53 | 55961 | 2012-02-04 00:00:00 | 55593.2050231482 | 2011-02-01 04:55:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI NAKAJIMA | JAP | 5 | AO5 | UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505042010/ | Quick Look | ![]() |
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939 | G12.0-0.1 | 273.0232 | -18.6277 | 272.288654 | -18.640604 | 272.865066 | 4.782958 | 11.94868379 | -0.09019508 | 259.2908 | 54375.5953819444 | 2007-10-02 14:17:21 | 54376.9863310185 | 2007-10-03 23:40:19 | 502001010 | 53.7521 | 53 | 53.7521 | 53.7521 | 0 | 53.7521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.183 | 47.183 | 120.172 | 1 | PROCESSED | 57540.1741898148 | 2016-06-01 04:10:50 | 54751 | 2008-10-12 00:00:00 | 54403.1207986111 | 2007-10-30 02:53:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHIGEO YAMAUCHI | JAP | 2 | AO2 | SUZAKU OBSERVATION OF G12.0-0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502001010/ | Quick Look | ![]() |
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940 | RCW86_SOUTH | 220.8315 | -62.6734 | 219.843557 | -62.461116 | 241.073682 | -44.079198 | 315.37853465 | -2.53716675 | 96.1597 | 54862.1182291667 | 2009-01-31 02:50:15 | 54863.3647569445 | 2009-02-01 08:45:15 | 503003010 | 54.8181 | 50 | 54.8181 | 54.8181 | 0 | 54.8341 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.3483 | 47.3483 | 107.6848 | 1 | PROCESSED | 57545.4382175926 | 2016-06-06 10:31:02 | 55329 | 2010-05-13 00:00:00 | 54880.5892361111 | 2009-02-18 14:08:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503003010/ | Quick Look | ![]() |
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941 | MRK 1073 | 48.7401 | 42.0969 | 47.912237 | 41.911835 | 57.846592 | 23.153427 | 149.47083071 | -13.26071681 | 81.0781 | 53949.235162037 | 2006-08-02 05:38:38 | 53949.3834722222 | 2006-08-02 09:12:12 | 701007010 | 3.4746 | 40 | 3.4746 | 3.4806 | 3.4786 | 3.4766 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4.1358 | 4.1358 | 12.806 | 0 | PROCESSED | 57535.0684375 | 2016-05-27 01:38:33 | 54735 | 2008-09-26 00:00:00 | 54132.9684490741 | 2007-02-01 23:14:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007010/ | Quick Look | ![]() |
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942 | VELA JR P20 | 133.6175 | -46.3272 | 133.188109 | -46.13587 | 160.261964 | -59.591088 | 266.52787238 | -0.88873335 | 346.9997 | 54651.2368402778 | 2008-07-04 05:41:03 | 54651.5828009259 | 2008-07-04 13:59:14 | 503032010 | 16.8237 | 10 | 16.8237 | 16.8317 | 0 | 16.8317 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.7982 | 14.7982 | 29.8879 | 0 | PROCESSED | 57542.9499074074 | 2016-06-03 22:47:52 | 55036 | 2009-07-24 00:00:00 | 54665.3228125 | 2008-07-18 07:44:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503032010/ | Quick Look | ![]() |
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943 | W49B | 287.7847 | 9.1157 | 287.186344 | 9.032042 | 290.655059 | 31.28998 | 43.28157058 | -0.18360003 | 89.2671 | 54919.1063888889 | 2009-03-29 02:33:12 | 54920.4689583333 | 2009-03-30 11:15:18 | 503084010 | 52.1549 | 40 | 52.1549 | 52.1549 | 0 | 52.1549 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9512 | 43.9512 | 117.7099 | 2 | PROCESSED | 57547.7422685185 | 2016-06-08 17:48:52 | 55330 | 2010-05-14 00:00:00 | 54931.3622106482 | 2009-04-10 08:41:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TORU TAMAGAWA | JAP | 3 | AO3 | IS W49B A REMNANT OF AN ANOMALOUS TYPE IA SUPERNOVA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503084010/ | Quick Look | ![]() |
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944 | GAMMACYGNI_NWSHELL1 | 304.9359 | 40.8711 | 304.492598 | 40.71257 | 324.526393 | 57.885883 | 78.38707497 | 2.60425327 | 82.9977 | 55664.4219675926 | 2011-04-13 10:07:38 | 55665.3022222222 | 2011-04-14 07:15:12 | 506017010 | 39.0271 | 40 | 39.0271 | 39.0271 | 0 | 39.0271 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.6965 | 37.6965 | 76.052 | 0 | PROCESSED | 57601.5010416667 | 2016-08-01 12:01:30 | 56058 | 2012-05-11 00:00:00 | 55690.9556597222 | 2011-05-09 22:56:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 6 | AO6 | SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506017010/ | Quick Look | ![]() |
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945 | SWIFT J0911.2+4533 | 137.9062 | 45.5305 | 137.073312 | 45.735684 | 126.030873 | 27.898314 | 174.70874001 | 43.11152809 | 111.3983 | 54764.185787037 | 2008-10-25 04:27:32 | 54766.2105787037 | 2008-10-27 05:03:14 | 703008010 | 93.879 | 80 | 93.879 | 93.879 | 0 | 93.895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.2256 | 80.2256 | 174.9298 | 4 | PROCESSED | 57544.2883564815 | 2016-06-05 06:55:14 | 55148 | 2009-11-13 00:00:00 | 54782.4040625 | 2008-11-12 09:41:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 3 | AO3 | THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703008010/ | Quick Look | ![]() |
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946 | VELA JR P6 | 133.325 | -45.4847 | 132.890485 | -45.294415 | 159.041125 | -58.989018 | 265.75161327 | -0.50306307 | 347.0024 | 54286.7508449074 | 2007-07-05 18:01:13 | 54286.9863888889 | 2007-07-05 23:40:24 | 502028010 | 11.5072 | 10 | 11.5312 | 11.5232 | 0 | 11.5072 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.2579 | 8.2579 | 20.3439 | 0 | PROCESSED | 57539.1055324074 | 2016-05-31 02:31:58 | 54696 | 2008-08-18 00:00:00 | 54328.3854166667 | 2007-08-16 09:15:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502028010/ | Quick Look | ![]() |
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947 | Q0827+243 | 127.7159 | 24.1868 | 126.975524 | 24.355663 | 124.075193 | 5.096736 | 200.01721235 | 31.87611482 | 114.1438 | 54766.2156828704 | 2008-10-27 05:10:35 | 54767.3363310185 | 2008-10-28 08:04:19 | 703003010 | 48.2277 | 40 | 48.2277 | 48.2277 | 0 | 48.2277 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3031 | 39.3031 | 96.8001 | 0 | PROCESSED | 57544.2665625 | 2016-06-05 06:23:51 | 54557 | 2008-04-01 00:00:00 | 54788.24125 | 2008-11-18 05:47:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703003010/ | Quick Look | ![]() |
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948 | 3C454.3 | 343.4943 | 16.1419 | 342.876691 | 15.875412 | 351.363443 | 21.32571 | 86.11034311 | -38.19103065 | 250.8076 | 54792.3878703704 | 2008-11-22 09:18:32 | 54793.6884143518 | 2008-11-23 16:31:19 | 703006010 | 46.9239 | 40 | 46.9239 | 46.9239 | 0 | 46.9239 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.344 | 43.344 | 112.3139 | 2 | PROCESSED | 57544.5029976852 | 2016-06-05 12:04:19 | 54557 | 2008-04-01 00:00:00 | 54811.7229050926 | 2008-12-11 17:20:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703006010/ | Quick Look | ![]() |
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949 | CTB1_SW | 359.716 | 62.4332 | 359.080854 | 62.154888 | 37.143182 | 54.514989 | 116.89133919 | 0.1796486 | 252.1748 | 55924.1262037037 | 2011-12-29 03:01:44 | 55924.6251736111 | 2011-12-29 15:00:15 | 506034010 | 28.9419 | 50 | 28.9419 | 28.9499 | 0 | 28.9499 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.385 | 25.385 | 43.108 | 0 | PROCESSED | 57604.2594675926 | 2016-08-04 06:13:38 | 56313 | 2013-01-21 00:00:00 | 55972.6473958333 | 2012-02-15 15:32:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA NAKASHIMA | JAP | 6 | AO6 | NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506034010/ | Quick Look | ![]() |
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950 | A1689-OFFSET1 | 198.0484 | -1.2633 | 197.406048 | -0.99812 | 197.124113 | 5.910782 | 313.73996571 | 61.17214089 | 289.9985 | 54670.1962962963 | 2008-07-23 04:42:40 | 54671.3488773148 | 2008-07-24 08:22:23 | 803024010 | 47.0703 | 40 | 47.0703 | 47.0813 | 0 | 47.0783 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.3283 | 36.3283 | 99.5439 | 1 | PROCESSED | 57543.121412037 | 2016-06-04 02:54:50 | 55076 | 2009-09-02 00:00:00 | 54707.0796180556 | 2008-08-29 01:54:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803024010/ | Quick Look | ![]() |
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951 | SWIFT J0959.5-2258 | 149.843 | -22.8716 | 149.261565 | -22.631568 | 161.273539 | -32.730158 | 259.02796733 | 24.98206567 | 303.2834 | 54635.9091087963 | 2008-06-18 21:49:07 | 54636.8148611111 | 2008-06-19 19:33:24 | 703013010 | 43.6634 | 40 | 43.6714 | 43.6794 | 0 | 43.6634 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4061 | 42.4061 | 78.2379 | 0 | PROCESSED | 57542.8554861111 | 2016-06-03 20:31:54 | 55016 | 2009-07-04 00:00:00 | 54650.0591782407 | 2008-07-03 01:25:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703013010/ | Quick Look | ![]() |
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952 | RXJ1713-3946_ID4 | 258.9125 | -40.0131 | 258.042933 | -39.957471 | 261.134722 | -16.911926 | 347.36417887 | -0.94594655 | 86.0017 | 55244.4787384259 | 2010-02-17 11:29:23 | 55244.8903587963 | 2010-02-17 21:22:07 | 504030010 | 22.1534 | 20 | 22.1774 | 22.1694 | 0 | 22.1534 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.7193 | 19.7193 | 35.5579 | 1 | PROCESSED | 57550.6146412037 | 2016-06-11 14:45:05 | 55622 | 2011-03-02 00:00:00 | 55256.0824768518 | 2010-03-01 01:58:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504030010/ | Quick Look | ![]() |
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953 | A2029_5 | 227.4808 | 5.8608 | 226.861375 | 6.050047 | 223.225848 | 22.663782 | 6.38223601 | 50.81650996 | 112.9567 | 55226.2508912037 | 2010-01-30 06:01:17 | 55226.875162037 | 2010-01-30 21:00:14 | 804024050 | 21.891 | 22 | 21.891 | 21.891 | 0 | 21.891 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.3419 | 14.3419 | 53.936 | 0 | PROCESSED | 57550.432337963 | 2016-06-11 10:22:34 | 55638 | 2011-03-18 00:00:00 | 55272.0370717593 | 2010-03-17 00:53:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024050/ | Quick Look | ![]() |
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954 | FERMI_BUBBLE_S4 | 331.467 | -46.3468 | 330.684504 | -46.590536 | 315.761845 | -32.186623 | 351.15250978 | -52.26066971 | 44.0063 | 56036.1354976852 | 2012-04-19 03:15:07 | 56036.5905324074 | 2012-04-19 14:10:22 | 507012010 | 21.1637 | 20 | 21.1717 | 21.1637 | 0 | 21.1718 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.3816 | 15.3816 | 39.3039 | 0 | PROCESSED | 57605.2132291667 | 2016-08-05 05:07:03 | 56434 | 2013-05-22 00:00:00 | 56068.6280671296 | 2012-05-21 15:04:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507012010/ | Quick Look | ![]() |
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955 | GC_SOUTH_3 | 268.18 | -29.2061 | 267.383741 | -29.195321 | 268.393759 | -5.775192 | 0.56701913 | -1.46906711 | 273.9841 | 56205.6096412037 | 2012-10-05 14:37:53 | 56206.6341898148 | 2012-10-06 15:13:14 | 507030010 | 51.7418 | 50 | 51.7498 | 51.7498 | 0 | 51.7418 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.1911 | 52.1911 | 88.5159 | 0 | PROCESSED | 57607.309537037 | 2016-08-07 07:25:44 | 56595 | 2013-10-30 00:00:00 | 56226.549212963 | 2012-10-26 13:10:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507030010/ | Quick Look | ![]() |
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956 | G32.8-0.1 SOUTH | 282.8163 | -0.2514 | 282.174201 | -0.311644 | 283.889842 | 22.573278 | 32.68848527 | -0.07620379 | 74.5004 | 56038.7902430556 | 2012-04-21 18:57:57 | 56039.916087963 | 2012-04-22 21:59:10 | 507036010 | 52.2324 | 50 | 52.2404 | 52.2324 | 0 | 52.2484 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2432 | 50.2432 | 97.268 | 1 | PROCESSED | 57605.2444560185 | 2016-08-05 05:52:01 | 56421 | 2013-05-09 00:00:00 | 56055.0208564815 | 2012-05-08 00:30:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507036010/ | Quick Look | ![]() |
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957 | SWIFT J0501.9-3239 | 79.8743 | -32.7041 | 79.409754 | -32.754183 | 74.820458 | -55.614502 | 236.069923 | -32.60257079 | 297.9191 | 54567.6584259259 | 2008-04-11 15:48:08 | 54568.8788194444 | 2008-04-12 21:05:30 | 703014010 | 41.2985 | 40 | 41.2985 | 41.2985 | 0 | 41.2985 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.4342 | 36.4342 | 105.4259 | 0 | PROCESSED | 57542.3107291667 | 2016-06-03 07:27:27 | 54953 | 2009-05-02 00:00:00 | 54580.5155208333 | 2008-04-24 12:22:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703014010/ | Quick Look | ![]() |
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958 | SWIFT J0134.1-3625 | 23.4345 | -36.4661 | 22.87514 | -36.722141 | 4.413021 | -42.266283 | 261.71382804 | -77.05672525 | 34.1001 | 54606.6796180556 | 2008-05-20 16:18:39 | 54607.8390277778 | 2008-05-21 20:08:12 | 703016010 | 48.5116 | 40 | 48.5196 | 48.5116 | 0 | 48.5276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2927 | 41.2927 | 100.1498 | 0 | PROCESSED | 57542.6141898148 | 2016-06-03 14:44:26 | 54985 | 2009-06-03 00:00:00 | 54616.4068402778 | 2008-05-30 09:45:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703016010/ | Quick Look | ![]() |
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959 | SWIFT J0444.1+2813 | 71.029 | 28.2793 | 70.24739 | 28.187015 | 73.273115 | 5.933796 | 172.68057795 | -11.38105828 | 85.0234 | 54719.7173958333 | 2008-09-10 17:13:03 | 54721.6306944445 | 2008-09-12 15:08:12 | 703021010 | 81.2986 | 80 | 81.2986 | 81.2986 | 0 | 81.2986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.7654 | 67.7654 | 165.3039 | 0 | PROCESSED | 57543.831087963 | 2016-06-04 19:56:46 | 55148 | 2009-11-13 00:00:00 | 54780.4776736111 | 2008-11-10 11:27:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 3 | AO3 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703021010/ | Quick Look | ![]() |
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960 | SGR B | 266.8769 | -28.4429 | 266.085661 | -28.425809 | 267.234018 | -5.031789 | 0.6365241 | -0.09758916 | 267.0001 | 56556.6453472222 | 2013-09-21 15:29:18 | 56559.2640740741 | 2013-09-24 06:20:16 | 508018010 | 101.9558 | 100 | 101.9558 | 101.9558 | 0 | 101.9558 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.894 | 87.894 | 226.2438 | 0 | PROCESSED | 57612.7499768518 | 2016-08-12 17:59:58 | 56956 | 2014-10-26 00:00:00 | 56588.5828125 | 2013-10-23 13:59:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080043 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508018010/ | Quick Look | ![]() |
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961 | JUPITER | 104.5549 | 23.0543 | 103.799265 | 23.122478 | 103.371966 | 0.286476 | 192.85746904 | 11.70034918 | 267.1462 | 56767.7816087963 | 2014-04-20 18:45:31 | 56768.1147916667 | 2014-04-21 02:45:18 | 508023130 | 10.0906 | 160 | 10.0986 | 10.0986 | 0 | 10.0906 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9649652778 | 2016-08-14 23:09:33 | 57212 | 2015-07-09 00:00:00 | 56782.5091782407 | 2014-05-05 12:13:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023130/ | Quick Look | ![]() |
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962 | AWM7 EAST OFFSET | 44.0318 | 41.5949 | 43.221288 | 41.393422 | 54.035202 | 23.723269 | 146.61375919 | -15.47239178 | 90.4995 | 53952.2676967593 | 2006-08-05 06:25:29 | 53953.2398611111 | 2006-08-06 05:45:24 | 801036010 | 38.5361 | 40 | 38.5361 | 38.5361 | 38.5361 | 38.5361 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37.541 | 37.541 | 83.9599 | 0 | PROCESSED | 57535.0870138889 | 2016-05-27 02:05:18 | 54394 | 2007-10-21 00:00:00 | 54020.7498726852 | 2006-10-12 17:59:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801036010/ | Quick Look | ![]() |
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963 | G359.0-0.9 S | 266.8698 | -30.3116 | 266.066627 | -30.294444 | 267.268772 | -6.900137 | 359.03431589 | -1.05952932 | 101.9997 | 56724.8167013889 | 2014-03-08 19:36:03 | 56726.0627662037 | 2014-03-10 01:30:23 | 508059010 | 53.4961 | 50 | 53.4961 | 53.5031 | 0 | 53.5201 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 47.9921 | 47.9921 | 107.6559 | 1 | PROCESSED | 57614.0007175926 | 2016-08-14 00:01:02 | 57106 | 2015-03-25 00:00:00 | 56740.7217013889 | 2014-03-24 17:19:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508059010/ | Quick Look | ![]() |
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964 | FJ0854+4908 | 133.7471 | 49.1347 | 132.871607 | 49.325626 | 121.634271 | 30.384389 | 170.1345398 | 40.07327965 | 275.4931 | 56775.9268865741 | 2014-04-28 22:14:43 | 56776.9669328704 | 2014-04-29 23:12:23 | 809038010 | 43.4713 | 45 | 43.4713 | 43.4713 | 0 | 43.4713 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2119 | 40.2119 | 89.8479 | 1 | PROCESSED | 57615.0216666667 | 2016-08-15 00:31:12 | 57214 | 2015-07-11 00:00:00 | 56848.6454166667 | 2014-07-10 15:29:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809038010/ | Quick Look | ![]() |
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965 | CTB109 SOUTHWEST | 345.0971 | 58.7572 | 344.575762 | 58.488555 | 23.478605 | 56.879692 | 108.94859975 | -1.06655489 | 252.0045 | 55909.1993287037 | 2011-12-14 04:47:02 | 55910.0807407407 | 2011-12-15 01:56:16 | 506038010 | 41.3824 | 40 | 41.3904 | 41.3824 | 0 | 41.3984 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.779 | 38.779 | 76.1358 | 0 | PROCESSED | 57604.1454282407 | 2016-08-04 03:29:25 | 56289 | 2012-12-28 00:00:00 | 55921.9811574074 | 2011-12-26 23:32:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506038010/ | Quick Look | ![]() |
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966 | W49B | 287.784 | 9.1149 | 287.185641 | 9.031245 | 290.654125 | 31.289286 | 43.28054167 | -0.18335704 | 82.0063 | 57131.6619444445 | 2015-04-19 15:53:12 | 57133.5779513889 | 2015-04-21 13:52:15 | 509001040 | 67.3182 | 400 | 67.3182 | 67.3182 | 0 | 67.3262 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0264699074 | 2016-08-18 00:38:07 | 56748 | 2014-04-01 00:00:00 | 57224.4531481482 | 2015-07-21 10:52:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001040/ | Quick Look | ![]() |
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967 | VELA PWN GEV1 | 127.6995 | -44.6062 | 127.276202 | -44.43674 | 151.392903 | -60.265182 | 262.61398048 | -3.09706524 | 119.7191 | 56985.3954282407 | 2014-11-24 09:29:25 | 56985.8502546296 | 2014-11-24 20:24:22 | 509011010 | 19.1492 | 15 | 19.1572 | 19.1652 | 0 | 19.1492 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8102893518 | 2016-08-16 19:26:49 | 57365 | 2015-12-09 00:00:00 | 57009.4123726852 | 2014-12-18 09:53:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509011010/ | Quick Look | ![]() |
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968 | G166.0+4.3_NW | 81.4339 | 42.9094 | 80.537947 | 42.865797 | 83.349134 | 19.666732 | 166.05797128 | 4.14809941 | 85.1436 | 56920.3100347222 | 2014-09-20 07:26:27 | 56921.2397106482 | 2014-09-21 05:45:11 | 509023010 | 39.7982 | 40 | 39.7982 | 42.0339 | 0 | 42.0259 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5613078704 | 2016-08-16 13:28:17 | 57298 | 2015-10-03 00:00:00 | 56940.6722569444 | 2014-10-10 16:08:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509023010/ | Quick Look | ![]() |
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969 | MRK421 | 166.0521 | 38.1644 | 165.357194 | 38.434126 | 151.189395 | 29.439264 | 179.96763761 | 64.99940635 | 318.3733 | 53853.2821412037 | 2006-04-28 06:46:17 | 53854.2711226852 | 2006-04-29 06:30:25 | 701024010 | 41.4709 | 40 | 41.4789 | 41.4709 | 41.4789 | 41.4789 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.7033 | 34.7033 | 85.4301 | 1 | PROCESSED | 57533.6140162037 | 2016-05-25 14:44:11 | 54394 | 2007-10-21 00:00:00 | 53908.0343055556 | 2006-06-22 00:49:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701024010/ | Quick Look | ![]() |
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970 | CIZA J1358.9-4750_SW | 209.5053 | -47.9232 | 208.715208 | -47.679899 | 225.712458 | -33.34381 | 314.31638856 | 13.47131455 | 293 | 56882.719537037 | 2014-08-13 17:16:08 | 56883.5528356482 | 2014-08-14 13:16:05 | 509027010 | 42.0308 | 40 | 42.0308 | 42.0548 | 0 | 42.0388 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.0109 | 7.0109 | 14.276 | 0 | PROCESSED | 57616.4982175926 | 2016-08-16 11:57:26 | 57267 | 2015-09-02 00:00:00 | 56898.5152662037 | 2014-08-29 12:21:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509027010/ | Quick Look | ![]() |
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971 | VELA JR P34 | 132.1138 | -46.9499 | 131.694344 | -46.763927 | 159.20149 | -60.674913 | 266.35035002 | -2.0812575 | 347.0005 | 54656.0096990741 | 2008-07-09 00:13:58 | 54656.2634143518 | 2008-07-09 06:19:19 | 503046010 | 11.0421 | 10 | 11.0581 | 11.0421 | 0 | 11.0581 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.1306 | 11.1306 | 21.916 | 0 | PROCESSED | 57543.0076967593 | 2016-06-04 00:11:05 | 55037 | 2009-07-25 00:00:00 | 54670.2236342593 | 2008-07-23 05:22:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503046010/ | Quick Look | ![]() |
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972 | VELA JR P37 | 132.6136 | -47.1701 | 132.194095 | -46.982326 | 160.029329 | -60.672793 | 266.73640279 | -1.95651055 | 346.9993 | 54656.9174768518 | 2008-07-09 22:01:10 | 54657.2418287037 | 2008-07-10 05:48:14 | 503049010 | 12.5294 | 10 | 12.5414 | 12.5294 | 0 | 12.5454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.8527 | 12.8527 | 28.02 | 0 | PROCESSED | 57543.0205671296 | 2016-06-04 00:29:37 | 55037 | 2009-07-25 00:00:00 | 54670.278900463 | 2008-07-23 06:41:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503049010/ | Quick Look | ![]() |
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973 | AWM7 NW1 | 42.8658 | 41.9211 | 42.057041 | 41.715759 | 53.244699 | 24.307791 | 145.6578115 | -15.59334332 | 257 | 56705.5358680556 | 2014-02-17 12:51:39 | 56705.8668287037 | 2014-02-17 20:48:14 | 808023010 | 14.8576 | 15 | 14.8896 | 14.8576 | 0 | 14.8736 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0088 | 11.0088 | 28.5839 | 1 | PROCESSED | 57613.8366550926 | 2016-08-13 20:04:47 | 57085 | 2015-03-04 00:00:00 | 56719.7185532407 | 2014-03-03 17:14:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808023010/ | Quick Look | ![]() |
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974 | WESTERLUND 2 | 156.0088 | -57.7448 | 155.54834 | -57.490842 | 195.724597 | -59.560466 | 284.2643696 | -0.3172737 | 343.7602 | 54687.6527199074 | 2008-08-09 15:39:55 | 54689.327962963 | 2008-08-11 07:52:16 | 503053010 | 73.67 | 100 | 73.67 | 73.67 | 0 | 73.67 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5776 | 86.5776 | 144.7298 | 0 | PROCESSED | 57543.2480555556 | 2016-06-04 05:57:12 | 55252 | 2010-02-25 00:00:00 | 54706.476412037 | 2008-08-28 11:26:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503053010/ | Quick Look | ![]() |
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975 | WESTERLUND 2 | 155.9878 | -57.7462 | 155.527496 | -57.492284 | 195.71117 | -59.569482 | 284.25564056 | -0.32444098 | 166.5036 | 54866.5949189815 | 2009-02-04 14:16:41 | 54867.1669444444 | 2009-02-05 04:00:24 | 503053020 | 33.4924 | 30 | 33.5004 | 33.4924 | 0 | 33.5004 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.073 | 32.073 | 49.4159 | 1 | PROCESSED | 57545.4584606482 | 2016-06-06 11:00:11 | 55329 | 2010-05-13 00:00:00 | 54880.5574189815 | 2009-02-18 13:22:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503053020/ | Quick Look | ![]() |
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976 | PKS1258-321 | 195.0396 | -32.3625 | 194.354396 | -32.09316 | 206.904154 | -23.820406 | 305.06853624 | 30.47306853 | 293.0551 | 55027.0059259259 | 2009-07-15 00:08:32 | 55027.6050231482 | 2009-07-15 14:31:14 | 704007010 | 28.4607 | 20 | 28.4607 | 28.7327 | 0 | 28.7274 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 24.0275 | 24.0275 | 51.7559 | 0 | PROCESSED | 57547.8136921296 | 2016-06-08 19:31:43 | 55406 | 2010-07-29 00:00:00 | 55040.1188657407 | 2009-07-28 02:51:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704007010/ | Quick Look | ![]() |
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977 | CENTAURUS_A | 201.3281 | -43.0649 | 200.594745 | -42.804861 | 217.131954 | -31.381221 | 309.48077241 | 19.37569293 | 303.3465 | 55057.3798148148 | 2009-08-14 09:06:56 | 55059.1051388889 | 2009-08-16 02:31:24 | 704018030 | 55.9442 | 50 | 55.9522 | 55.9442 | 0 | 55.9442 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.4915 | 46.4915 | 149.0478 | 3 | PROCESSED | 57548.1889699074 | 2016-06-09 04:32:07 | 55434 | 2010-08-26 00:00:00 | 55068.1674768518 | 2009-08-25 04:01:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704018030/ | Quick Look | ![]() |
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978 | EMS0992 | 230.2572 | -3.8213 | 229.602576 | -3.642087 | 228.859181 | 14.124861 | 358.15856297 | 42.46037658 | 113.2867 | 55593.7858564815 | 2011-02-01 18:51:38 | 55594.1841898148 | 2011-02-02 04:25:14 | 705026010 | 18.979 | 20 | 18.979 | 18.979 | 0 | 18.979 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14.832 | 14.832 | 34.3939 | 0 | PROCESSED | 57600.8001388889 | 2016-07-31 19:12:12 | 55973 | 2012-02-16 00:00:00 | 55607.0454976852 | 2011-02-15 01:05:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705026010/ | Quick Look | ![]() |
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979 | A2104E | 235.1486 | -3.297 | 234.495076 | -3.136609 | 233.617797 | 15.850396 | 2.9252225 | 39.1285511 | 117.6908 | 54118.1261226852 | 2007-01-18 03:01:37 | 54118.6850231482 | 2007-01-18 16:26:26 | 801003010 | 22.7847 | 20 | 22.7847 | 22.7847 | 0 | 22.7847 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.7352 | 17.7352 | 48.2879 | 1 | PROCESSED | 57536.8549189815 | 2016-05-28 20:31:05 | 54735 | 2008-09-26 00:00:00 | 54132.8631365741 | 2007-02-01 20:42:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801003010/ | Quick Look | ![]() |
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980 | A399/401 FILAMENT | 44.7475 | 13.2485 | 44.061375 | 13.049612 | 46.15841 | -3.573964 | 164.45015039 | -39.12843885 | 74.1756 | 53966.1736921296 | 2006-08-19 04:10:07 | 53969.4641666667 | 2006-08-22 11:08:24 | 801020010 | 151.0601 | 150 | 151.0601 | 151.0681 | 151.0681 | 151.0681 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 142.2036 | 142.2036 | 284.2738 | 5 | PROCESSED | 57535.3984837963 | 2016-05-27 09:33:49 | 54526 | 2008-03-01 00:00:00 | 54021.1056944444 | 2006-10-13 02:32:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | THE DETECTION OF WHIM IN THE A399/401 FILAMENT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801020010/ | Quick Look | ![]() |
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981 | EMS1341 | 301.2467 | 70.0571 | 301.259152 | 69.912683 | 31.029252 | 78.090273 | 102.85714193 | 19.4440121 | 233.7732 | 55527.303275463 | 2010-11-27 07:16:43 | 55527.7619675926 | 2010-11-27 18:17:14 | 705027010 | 23.0668 | 20 | 23.0668 | 23.0668 | 0 | 23.0668 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.5055 | 21.5055 | 39.6239 | 0 | PROCESSED | 57554.2240856482 | 2016-06-15 05:22:41 | 55903 | 2011-12-08 00:00:00 | 55537.0214814815 | 2010-12-07 00:30:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705027010/ | Quick Look | ![]() |
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982 | A1060_OFFSET | 159.8425 | -27.5312 | 159.252316 | -27.270314 | 173.386883 | -33.06567 | 270.15539037 | 26.80693828 | 96.4852 | 54425.0245486111 | 2007-11-21 00:35:21 | 54427.7988888889 | 2007-11-23 19:10:24 | 802028010 | 103.7993 | 100 | 103.7993 | 103.7993 | 0 | 103.7993 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.1119 | 89.1119 | 239.6797 | 2 | PROCESSED | 57540.6102662037 | 2016-06-01 14:38:47 | 54804 | 2008-12-04 00:00:00 | 54434.2515509259 | 2007-11-30 06:02:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOSUKE SATO | JAP | 2 | AO2 | TEMPERATURE AND ABUNDANCE PROFILES IN THE OUTER REGION OF THE NON-CD CLUSTER A1060 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802028010/ | Quick Look | ![]() |
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983 | A2142 OFFSET2 | 239.2185 | 27.5666 | 238.702662 | 27.710117 | 228.594218 | 46.67807 | 44.63617571 | 49.06945571 | 260.7114 | 54358.4806597222 | 2007-09-15 11:32:09 | 54360.0627893518 | 2007-09-17 01:30:25 | 802031010 | 57.7187 | 50 | 57.7187 | 57.7187 | 0 | 57.7187 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 52.5976 | 52.5976 | 136.6318 | 1 | PROCESSED | 57539.9791666667 | 2016-05-31 23:30:00 | 54751 | 2008-10-12 00:00:00 | 54371.4005208333 | 2007-09-28 09:36:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYA OHASHI | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802031010/ | Quick Look | ![]() |
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984 | HESS J1745-303B | 266.0577 | -30.545 | 265.253177 | -30.523904 | 266.569275 | -7.150762 | 358.47050833 | -0.58308172 | 102.2921 | 55254.6768634259 | 2010-02-27 16:14:41 | 55255.9515509259 | 2010-02-28 22:50:14 | 504002010 | 53.0609 | 50 | 53.0609 | 53.0609 | 0 | 53.0609 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.585 | 46.585 | 110.1219 | 1 | PROCESSED | 57550.7606481482 | 2016-06-11 18:15:20 | 55636 | 2011-03-16 00:00:00 | 55267.2715856482 | 2010-03-12 06:31:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504002010/ | Quick Look | ![]() |
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985 | AWM7 SOUTH OFFSET | 43.2198 | 40.6314 | 42.417413 | 40.427233 | 53.073147 | 23.000259 | 146.52805812 | -16.61071542 | 257.3937 | 54519.4104861111 | 2008-02-23 09:51:06 | 54521.6112847222 | 2008-02-25 14:40:15 | 802045020 | 91.2272 | 80 | 91.2272 | 91.2272 | 0 | 91.2272 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.0285 | 80.0285 | 190.1139 | 2 | PROCESSED | 57541.7536111111 | 2016-06-02 18:05:12 | 54904 | 2009-03-14 00:00:00 | 54535.283599537 | 2008-03-10 06:48:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA ISHISAKI | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802045020/ | Quick Look | ![]() |
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986 | ASO0218 | 157.1332 | -58.313 | 156.668691 | -58.056852 | 197.346686 | -59.525927 | 285.06973918 | -0.48663651 | 315.2825 | 55020.3423148148 | 2009-07-08 08:12:56 | 55020.9467476852 | 2009-07-08 22:43:19 | 504045010 | 22.8449 | 20 | 22.8449 | 22.8449 | 0 | 22.8449 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1544 | 21.1544 | 52.2179 | 1 | PROCESSED | 57547.7933680556 | 2016-06-08 19:02:27 | 55400 | 2010-07-23 00:00:00 | 55034.2716898148 | 2009-07-22 06:31:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504045010/ | Quick Look | ![]() |
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987 | NGC 3997 | 179.448 | 25.2646 | 178.805338 | 25.542926 | 168.8766 | 22.834867 | 218.72362191 | 77.82883353 | 305.585 | 56439.4793981482 | 2013-05-27 11:30:20 | 56441.452974537 | 2013-05-29 10:52:17 | 708002010 | 87.1383 | 80 | 87.1383 | 87.1383 | 0 | 87.1383 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.0504 | 83.0504 | 170.508 | 2 | PROCESSED | 57611.4399305556 | 2016-08-11 10:33:30 | 56816 | 2014-06-08 00:00:00 | 56450.866724537 | 2013-06-07 20:48:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080015 | 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. 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. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 8 | AO8 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708002010/ | Quick Look | ![]() |
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988 | DEM L 192 | 81.4194 | -67.497 | 81.444182 | -67.538512 | 340.379487 | -86.530508 | 277.77177426 | -33.0775429 | 334.6993 | 54968.6808680556 | 2009-05-17 16:20:27 | 54971.0113310185 | 2009-05-20 00:16:19 | 804009010 | 87.3165 | 80 | 87.3245 | 87.3165 | 0 | 87.3245 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.0589 | 80.0589 | 201.3277 | 2 | PROCESSED | 57546.6405439815 | 2016-06-07 15:22:23 | 55356 | 2010-06-09 00:00:00 | 54987.4577314815 | 2009-06-05 10:59:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040009 | The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYA YAMAGUCHI | JAP | 4 | AO4 | DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804009010/ | Quick Look | ![]() |
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989 | FERMI_0281 | 197.9603 | -34.4918 | 197.262031 | -34.226396 | 210.309678 | -24.734564 | 307.70107754 | 28.19093927 | 309.4896 | 55047.2059606482 | 2009-08-04 04:56:35 | 55048.3043287037 | 2009-08-05 07:18:14 | 804018010 | 39.9038 | 40 | 39.9038 | 39.9038 | 0 | 39.9038 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.5708 | 35.5708 | 94.8819 | 1 | PROCESSED | 57548.0705902778 | 2016-06-09 01:41:39 | 55423 | 2010-08-15 00:00:00 | 55060.7435763889 | 2009-08-17 17:50:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804018010/ | Quick Look | ![]() |
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990 | FORNAX A W-LOBE N | 50.5227 | -36.9675 | 50.043813 | -37.145451 | 32.738272 | -52.85468 | 239.75066849 | -56.83654313 | 27.8129 | 54991.7546875 | 2009-06-09 18:06:45 | 54992.8119675926 | 2009-06-10 19:29:14 | 804037010 | 60.7627 | 50 | 60.7707 | 60.7627 | 0 | 60.7707 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.817 | 54.817 | 91.3258 | 1 | PROCESSED | 57547.5602777778 | 2016-06-08 13:26:48 | 55367 | 2010-06-20 00:00:00 | 55001.1883912037 | 2009-06-19 04:31:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MAKOTO TASHIRO | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804037010/ | Quick Look | ![]() |
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991 | CYGNUS LOOP 6 | 314.1656 | 31.2305 | 313.646001 | 31.037451 | 329.094604 | 46.032553 | 75.19999907 | -9.14964477 | 81.8988 | 55301.8924189815 | 2010-04-15 21:25:05 | 55302.1398148148 | 2010-04-16 03:21:20 | 505014010 | 12.4623 | 10 | 12.4783 | 12.4623 | 0 | 12.4783 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.0683 | 12.0683 | 21.3599 | 0 | PROCESSED | 57551.2257060185 | 2016-06-12 05:25:01 | 55287 | 2010-04-01 00:00:00 | 55362.3410532407 | 2010-06-15 08:11:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505014010/ | Quick Look | ![]() |
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992 | CYGNUS LOOP 12 | 313.6077 | 30.3526 | 313.085044 | 30.161518 | 327.967179 | 45.415269 | 74.20451075 | -9.33661335 | 82.0022 | 55329.1256944444 | 2010-05-13 03:01:00 | 55329.8391666667 | 2010-05-13 20:08:24 | 505020010 | 27.8427 | 28 | 27.8507 | 27.8507 | 0 | 27.8427 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0522 | 21.0522 | 61.64 | 0 | PROCESSED | 57551.5093055556 | 2016-06-12 12:13:24 | 55287 | 2010-04-01 00:00:00 | 55393.4203009259 | 2010-07-16 10:05:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505020010/ | Quick Look | ![]() |
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993 | SPT-CLJ2344-4243 | 356.1816 | -42.7169 | 355.522212 | -42.994645 | 336.755816 | -37.082735 | 339.63806237 | -69.34299043 | 226.1467 | 56605.0105902778 | 2013-11-09 00:15:15 | 56607.4106597222 | 2013-11-11 09:51:21 | 708012010 | 86.2043 | 80 | 86.2043 | 86.2043 | 0 | 86.2043 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.0289 | 80.0289 | 207.3477 | 3 | PROCESSED | 57613.3115625 | 2016-08-13 07:28:39 | 56383 | 2013-04-01 00:00:00 | 56653.7570949074 | 2013-12-27 18:10:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080071 | SPT-CLJ2344-4243 is a distant (z=0.596) extremely luminous (Lx=8x10^45erg/s) cluster with a strong cooling flow rate of 3820 Msun/year. The central galaxy of the cluster shows huge star formation activity and has a luminous (Lx=3x10^45 erg/s) AGN. According to the paper by McDonald et al. (2012) and Fe I detection by our analysis of the archived data of Suzaku, this AGN is likely to be a type 2 QSO, for which we don ft know any other example situated at the center of a cluster. We are observing a special phase of co-evolution of a cluster, its central galaxy, and SMBH at its center. We propose to perform 80ks x 4 times observations with Suzaku to estimate SMBH mass in this system through X-ray variability and to get Fe I line detection with higher confidence. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SHUTARO UEDA | JAP | 8 | AO8 | CO-EVOLUTION IN SMBH, GALAXY AND CLUSTERS; SUZAKU OBSERVATION OF A TYPE 2 QSO AT THE CENTER OF SPT-CLJ2344-4243 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708012010/ | Quick Look | ![]() |
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994 | FVW319.8+0.3_BGD | 225.4141 | -58.3766 | 224.455219 | -58.179449 | 241.611855 | -39.24635 | 319.32044374 | 0.28957352 | 278.3765 | 55413.9313888889 | 2010-08-05 22:21:12 | 55414.6724768518 | 2010-08-06 16:08:22 | 505030010 | 51.6262 | 50 | 51.6262 | 51.6636 | 0 | 51.6476 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.0503 | 40.0503 | 64.0179 | 1 | PROCESSED | 57552.8534837963 | 2016-06-13 20:29:01 | 55793 | 2011-08-20 00:00:00 | 55427.2012152778 | 2010-08-19 04:49:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 5 | AO5 | SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505030010/ | Quick Look | ![]() |
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995 | DEM L 86 | 77.4674 | -68.8946 | 77.532288 | -68.954899 | 328.060855 | -84.723884 | 279.75652902 | -34.25087364 | 194.4731 | 55552.1478703704 | 2010-12-22 03:32:56 | 55552.9495601852 | 2010-12-22 22:47:22 | 505041010 | 51.4681 | 50 | 51.4997 | 51.4997 | 0 | 51.4681 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.2589 | 44.2589 | 69.2579 | 0 | PROCESSED | 57554.4839236111 | 2016-06-15 11:36:51 | 55973 | 2012-02-16 00:00:00 | 55607.0926851852 | 2011-02-15 02:13:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI NAKAJIMA | JAP | 5 | AO5 | UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505041010/ | Quick Look | ![]() |
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996 | A 2218 | 249.0001 | 66.203 | 248.949919 | 66.302836 | 172.76704 | 81.613118 | 97.724401 | 38.11892096 | 242.3617 | 53644.3643402778 | 2005-10-01 08:44:39 | 53645.3446643518 | 2005-10-02 08:16:19 | 100030010 | 43.3629 | 50 | 43.3629 | 44.7173 | 43.4253 | 43.8248 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41.4918 | 41.4918 | 84.678 | 1 | PROCESSED | 57527.4791898148 | 2016-05-19 11:30:02 | 54247 | 2007-05-27 00:00:00 | 54035.7677314815 | 2006-10-27 18:25:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | A2218 and its offset observation | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100030010/ | Quick Look | ![]() |
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997 | 3C78 | 47.1071 | 4.1138 | 46.452233 | 3.923143 | 45.835066 | -12.996467 | 174.85308943 | -44.51284685 | 84.4195 | 55793.5846990741 | 2011-08-20 14:01:58 | 55795.7502430556 | 2011-08-22 18:00:21 | 706013010 | 97.0122 | 100 | 97.0122 | 97.0122 | 0 | 97.0122 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 85.9075 | 85.9075 | 187.0878 | 0 | PROCESSED | 57602.928275463 | 2016-08-02 22:16:43 | 56176 | 2012-09-06 00:00:00 | 55806.3891435185 | 2011-09-02 09:20:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 6 | AO6 | ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706013010/ | Quick Look | ![]() |
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998 | NGC3628 | 170.0699 | 13.5986 | 169.41715 | 13.872528 | 165.514956 | 8.570385 | 240.83294046 | 64.7853987 | 100 | 55890.624212963 | 2011-11-25 14:58:52 | 55892.4070601852 | 2011-11-27 09:46:10 | 806018010 | 81.5115 | 80 | 81.5275 | 81.5115 | 0 | 81.5218 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.5925 | 70.5925 | 153.9938 | 1 | PROCESSED | 57603.996087963 | 2016-08-03 23:54:22 | 56269 | 2012-12-08 00:00:00 | 55901.2586689815 | 2011-12-06 06:12:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060082 | We propose 80 ksec observations of edge-on nearby spiral starburst galaxies, NGC3628 and NGC891. We aim to obtain the temperature and the abundance pattern in both the disk and halo regions of two starburst galaxies and hopefully constrain the model of the interactions between not only disk and halo but also halo and intergalactic medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IKUYUKI MITSUISHI | JAP | 6 | AO6 | OBSERVATIONS OF AN EDGE-ON STARBURST GALAXIES NGC3628 & NGC891 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806018010/ | Quick Look | ![]() |
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999 | SGR1900+14 | 286.803 | 9.3875 | 286.206177 | 9.3084 | 289.573902 | 31.693472 | 43.07594962 | 0.80149907 | 86.5533 | 53826.3631597222 | 2006-04-01 08:42:57 | 53826.9113310185 | 2006-04-01 21:52:19 | 401022010 | 17.0562 | 20 | 17.7046 | 21.7074 | 21.6555 | 17.0562 | 1 | 2 | 1 | 1 | 1 | 0 | 0 | 14.3604 | 14.3604 | 47.336 | 1 | PROCESSED | 57533.34875 | 2016-05-25 08:22:12 | 54394 | 2007-10-21 00:00:00 | 53906.0977893518 | 2006-06-20 02:20:49 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUJIN NAKAGAWA | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401022010/ | Quick Look | ![]() |
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1000 | AWM7 SE2 | 44.7376 | 40.9954 | 43.928492 | 40.796305 | 54.382202 | 22.988972 | 147.39655193 | -15.74105021 | 257.0003 | 56707.1291319444 | 2014-02-19 03:05:57 | 56707.9132407407 | 2014-02-19 21:55:04 | 808026010 | 35.304 | 35 | 35.304 | 35.316 | 0 | 35.308 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.1778 | 31.1778 | 67.742 | 4 | PROCESSED | 57613.8746064815 | 2016-08-13 20:59:26 | 57085 | 2015-03-04 00:00:00 | 56719.7754398148 | 2014-03-03 18:36:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808026010/ | Quick Look | ![]() |
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1001 | NGC6251_LOBE_BGD1 | 247.6537 | 82.9256 | 249.113456 | 83.028127 | 99.179697 | 72.901441 | 116.18672095 | 31.0445068 | 26.9624 | 55667.0269328704 | 2011-04-16 00:38:47 | 55667.4328125 | 2011-04-16 10:23:15 | 706004010 | 18.822 | 20 | 18.8357 | 18.822 | 0 | 18.8356 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9572 | 18.9572 | 35.0659 | 1 | PROCESSED | 57601.5125694445 | 2016-08-01 12:18:06 | 56058 | 2012-05-11 00:00:00 | 55691.0888194444 | 2011-05-10 02:07:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706004010/ | Quick Look | ![]() |
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1002 | JUPITER | 28.7092 | 10.4688 | 28.044402 | 10.223855 | 30.381154 | -1.215152 | 147.29554938 | -49.38035583 | 249.1847 | 55930.8245717593 | 2012-01-04 19:47:23 | 55931.8508564815 | 2012-01-05 20:25:14 | 506006020 | 35.518 | 160 | 35.522 | 35.518 | 0 | 35.526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.367 | 34.367 | 88.6599 | 0 | PROCESSED | 57604.3110185185 | 2016-08-04 07:27:52 | 56316 | 2013-01-24 00:00:00 | 55946.2294097222 | 2012-01-20 05:30:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006020/ | Quick Look | ![]() |
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1003 | HESS J1943+213 | 295.9916 | 21.301 | 295.448325 | 21.18018 | 303.194 | 41.793482 | 57.76229591 | -1.30331963 | 246.7107 | 55875.6293055556 | 2011-11-10 15:06:12 | 55876.6015393518 | 2011-11-11 14:26:13 | 706007010 | 38.8815 | 40 | 38.8815 | 38.8895 | 0 | 38.8895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.313 | 35.313 | 83.972 | 1 | PROCESSED | 57603.7570601852 | 2016-08-03 18:10:10 | 56256 | 2012-11-25 00:00:00 | 55890.6970833333 | 2011-11-25 16:43:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | LUKASZ STAWARZ | JAP | 6 | AO6 | PECULIAR UNIDENTIFIED TEV SOURCE HESS J1943+213 IN THE GALACTIC PLANE: EXTREME BLAZAR OR SOMETHING ELSE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706007010/ | Quick Look | ![]() |
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1004 | SWIFT J1310.9-5553 | 197.6868 | -55.8722 | 196.924529 | -55.606324 | 222.251055 | -43.758692 | 305.6577855 | 6.89731776 | 290.4478 | 55761.4489467593 | 2011-07-19 10:46:29 | 55762.6432523148 | 2011-07-20 15:26:17 | 706009010 | 82.785 | 80 | 82.793 | 82.785 | 0 | 82.785 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.5081 | 67.5081 | 103.1779 | 1 | PROCESSED | 57602.6323263889 | 2016-08-02 15:10:33 | 56213 | 2012-10-13 00:00:00 | 55845.247662037 | 2011-10-11 05:56:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 6 | AO6 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706009010/ | Quick Look | ![]() |
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1005 | 3C 98 | 59.723 | 10.4395 | 59.038566 | 10.297703 | 59.781896 | -9.882185 | 179.82925767 | -31.05249617 | 81.003 | 55812.5811342593 | 2011-09-08 13:56:50 | 55815.280787037 | 2011-09-11 06:44:20 | 706015010 | 101.144 | 100 | 101.144 | 101.144 | 0 | 101.144 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.8389 | 89.8389 | 233.214 | 3 | PROCESSED | 57603.1723611111 | 2016-08-03 04:08:12 | 56218 | 2012-10-18 00:00:00 | 55851.4528356482 | 2011-10-17 10:52:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | POSHAK GANDHI | JAP | 6 | AO6 | HARD X-RAY EMISSION AND REFLECTION IN RADIO GALAXIES: 3C 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706015010/ | Quick Look | ![]() |
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1006 | CTB1_NE | 0.2869 | 62.6043 | 359.6465 | 62.325973 | 37.675416 | 54.459267 | 117.18345572 | 0.29518062 | 253.7193 | 55923.0281134259 | 2011-12-28 00:40:29 | 55924.1251736111 | 2011-12-29 03:00:15 | 506035010 | 52.666 | 50 | 52.666 | 52.666 | 0 | 52.666 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3108 | 48.3108 | 94.7759 | 3 | PROCESSED | 57604.2722569444 | 2016-08-04 06:32:03 | 56313 | 2013-01-21 00:00:00 | 55972.6734490741 | 2012-02-15 16:09:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA NAKASHIMA | JAP | 6 | AO6 | NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506035010/ | Quick Look | ![]() |
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1007 | W28WEST | 269.8372 | -23.6072 | 269.074768 | -23.604556 | 269.841247 | -0.166403 | 6.15250357 | 0.06606197 | 270.1135 | 55844.0583217593 | 2011-10-10 01:23:59 | 55848.1342708333 | 2011-10-14 03:13:21 | 506036010 | 151.0892 | 150 | 151.0972 | 151.0892 | 0 | 151.0923 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 128.9797 | 128.9797 | 352.1259 | 2 | PROCESSED | 57603.4758449074 | 2016-08-03 11:25:13 | 56240 | 2012-11-09 00:00:00 | 55872.5113425926 | 2011-11-07 12:16:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO SAWADA | JAP | 6 | AO6 | THE SNR W28 - SEARCHING FOR THE PHYSICAL CONNECTION BETWEEN HIGH-ENERGY COSMIC RAYS AND OVER-IONIZED PLASMA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506036010/ | Quick Look | ![]() |
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1008 | 1FGL J0103.1+4840 | 15.7305 | 48.657 | 15.006375 | 48.388615 | 36.058904 | 38.14189 | 124.88749892 | -14.17113818 | 69.2705 | 55753.0127430556 | 2011-07-11 00:18:21 | 55755.0002199074 | 2011-07-13 00:00:19 | 706025010 | 84.3622 | 80 | 84.3622 | 84.3622 | 0 | 84.3622 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.727 | 79.727 | 171.6957 | 2 | PROCESSED | 57602.5903935185 | 2016-08-02 14:10:10 | 56148 | 2012-08-09 00:00:00 | 55778.4339814815 | 2011-08-05 10:24:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KOTO MAEDA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706025010/ | Quick Look | ![]() |
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1009 | RX J1633+4718 | 248.3647 | 47.3332 | 248.004849 | 47.436616 | 228.791999 | 67.699433 | 73.56993988 | 42.60070523 | 133.9355 | 55962.6778240741 | 2012-02-05 16:16:04 | 55963.7502430556 | 2012-02-06 18:00:21 | 706027040 | 45.4834 | 40 | 45.4834 | 45.4834 | 0 | 45.4834 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.3113 | 40.3113 | 92.6459 | 0 | PROCESSED | 57604.5712152778 | 2016-08-04 13:42:33 | 56345 | 2013-02-22 00:00:00 | 55978.5479282407 | 2012-02-21 13:09:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KIYOSHI HAYASHIDA | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706027040/ | Quick Look | ![]() |
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1010 | FERMI_BUBBLE_S2 | 330.2693 | -46.4894 | 329.48073 | -46.73026 | 314.804008 | -31.978019 | 351.28666586 | -51.42688059 | 44.0074 | 56035.2081018518 | 2012-04-18 04:59:40 | 56035.6736921296 | 2012-04-18 16:10:07 | 507010010 | 20.3496 | 20 | 20.3576 | 20.3496 | 0 | 20.3648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.278 | 14.278 | 40.2139 | 0 | PROCESSED | 57605.1975231482 | 2016-08-05 04:44:26 | 56420 | 2013-05-08 00:00:00 | 56049.1880555556 | 2012-05-02 04:30:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507010010/ | Quick Look | ![]() |
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1011 | MARS-P2 | 102.9198 | 25.1641 | 102.151384 | 25.224519 | 101.686434 | 2.245784 | 190.26475308 | 11.2294146 | 298.0203 | 54559.4100925926 | 2008-04-03 09:50:32 | 54559.493275463 | 2008-04-03 11:50:19 | 403006020 | 4.8546 | 100 | 4.8546 | 4.8866 | 0 | 4.8706 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.6121 | 3.6121 | 7.1839 | 0 | PROCESSED | 57542.0367939815 | 2016-06-03 00:52:59 | 54953 | 2009-05-02 00:00:00 | 54577.0304976852 | 2008-04-21 00:43:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006020/ | Quick Look | ![]() |
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1012 | MARS-P19 | 103.6272 | 25.0809 | 102.859615 | 25.144671 | 102.332327 | 2.221472 | 190.61541806 | 11.77628093 | 298.2673 | 54560.8266319444 | 2008-04-04 19:50:21 | 54560.9098842593 | 2008-04-04 21:50:14 | 403006190 | 2.8398 | 100 | 2.8398 | 2.8482 | 0 | 2.8438 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1.8441 | 1.8441 | 7.19 | 0 | PROCESSED | 57542.0723958333 | 2016-06-03 01:44:15 | 54953 | 2009-05-02 00:00:00 | 54578.0465625 | 2008-04-22 01:07:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006190/ | Quick Look | ![]() |
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1013 | VELA JR P31 | 133.8003 | -46.8845 | 133.374404 | -46.692518 | 161.076222 | -59.989175 | 267.03483855 | -1.15221367 | 347.0003 | 54655.085 | 2008-07-08 02:02:24 | 54655.3273032407 | 2008-07-08 07:51:19 | 503043010 | 11.2095 | 10 | 11.2175 | 11.2255 | 0 | 11.2095 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.542 | 11.542 | 20.9279 | 0 | PROCESSED | 57542.9998263889 | 2016-06-03 23:59:45 | 55048 | 2009-08-05 00:00:00 | 54679.372974537 | 2008-08-01 08:57:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503043010/ | Quick Look | ![]() |
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1014 | NGC 4593 | 189.9132 | -5.341 | 189.26831 | -5.066485 | 191.201043 | -0.986248 | 297.48043001 | 57.40595243 | 111.8998 | 57021.7640856482 | 2014-12-30 18:20:17 | 57025.333287037 | 2015-01-03 07:59:56 | 709014050 | 145.2819 | 30 | 145.2819 | 145.3032 | 0 | 145.2899 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5760069445 | 2016-08-17 13:49:27 | 57415 | 2016-01-28 00:00:00 | 57049.4542939815 | 2015-01-27 10:54:11 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014050/ | Quick Look | ![]() |
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1015 | NGC 1566 | 65.0038 | -54.9403 | 64.723209 | -55.058612 | 32.065014 | -73.361775 | 264.31301386 | -43.39149342 | 351.3031 | 56066.0671759259 | 2012-05-19 01:36:44 | 56067.2738310185 | 2012-05-20 06:34:19 | 707002010 | 72.791 | 80 | 72.791 | 72.791 | 0 | 72.791 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.9581 | 71.9581 | 104.2239 | 2 | PROCESSED | 57605.4671875 | 2016-08-05 11:12:45 | 56442 | 2013-05-30 00:00:00 | 56076.0434606482 | 2012-05-29 01:02:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 7 | AO7 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707002010/ | Quick Look | ![]() |
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1016 | RX J1713.7-3946 NE | 258.6449 | -39.4419 | 257.780148 | -39.385009 | 260.872484 | -16.359233 | 347.70840856 | -0.44579664 | 85.9991 | 56714.667349537 | 2014-02-26 16:00:59 | 56716.5279513889 | 2014-02-28 12:40:15 | 508017010 | 100.6728 | 100 | 100.7048 | 100.6968 | 0 | 100.6728 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 104.394 | 104.394 | 160.7277 | 1 | PROCESSED | 57613.9490162037 | 2016-08-13 22:46:35 | 57093 | 2015-03-12 00:00:00 | 56727.6718865741 | 2014-03-11 16:07:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080029 | We proposed Suzaku observation of a thermal emission line in the young TeV gamma-ray SNR RX J1713.7-3946. Most recently, we found the candidate of thermal emission line toward North-East of the SNR analyzed with Suzaku archive data. The region is present in the vicinity of the small molecular cloud interacts with the SNR shock wave. Main purpose is significant detection of the Si line about 5 sigma. This observation will be observable only with Suzaku and lead to a large step forward on cosmic-ray acceleration and shock-cloud interaction in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | HIDETOSHI SANO | JAP | 8 | AO8 | SUZAKU OBSERVATION OF A THERMAL EMISSION LINE IN THE SNR RX J1713.7-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508017010/ | Quick Look | ![]() |
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1017 | JUPITER | 103.9685 | 23.1027 | 103.212311 | 23.168111 | 102.830346 | 0.281775 | 192.5818164 | 11.23089407 | 264.4391 | 56763.3891666667 | 2014-04-16 09:20:24 | 56763.722349537 | 2014-04-16 17:20:11 | 508023050 | 14.3106 | 160 | 14.3106 | 14.3207 | 0 | 14.3207 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9511111111 | 2016-08-14 22:49:36 | 57212 | 2015-07-09 00:00:00 | 56782.4912731482 | 2014-05-05 11:47:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023050/ | Quick Look | ![]() |
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1018 | IGR J17195-4100 | 259.8947 | -41.0152 | 259.016072 | -40.964234 | 261.995287 | -17.853831 | 346.97641748 | -2.13400756 | 97.0631 | 54880.4607175926 | 2009-02-18 11:03:26 | 54881.3106481482 | 2009-02-19 07:27:20 | 403028010 | 31.6456 | 30 | 31.6456 | 31.6456 | 0 | 31.6456 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.9178 | 26.9178 | 73.428 | 0 | PROCESSED | 57545.5868981482 | 2016-06-06 14:05:08 | 55330 | 2010-05-14 00:00:00 | 54895.5494328704 | 2009-03-05 13:11:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403028010/ | Quick Look | ![]() |
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1019 | VELA JR WEST2 | 131.7715 | -45.9871 | 131.345884 | -45.80238 | 157.754454 | -59.989666 | 265.452568 | -1.6600557 | 116.213 | 56619.4434490741 | 2013-11-23 10:38:34 | 56620.0800115741 | 2013-11-24 01:55:13 | 508037010 | 29.185 | 30 | 29.193 | 29.201 | 0 | 29.185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0652 | 35.0652 | 54.9859 | 1 | PROCESSED | 57613.3840277778 | 2016-08-13 09:13:00 | 56995 | 2014-12-04 00:00:00 | 56629.6443055556 | 2013-12-03 15:27:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDETOSHI SANO | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508037010/ | Quick Look | ![]() |
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1020 | ARK 120 | 79.0439 | -0.2064 | 78.404432 | -0.260846 | 78.068932 | -23.195412 | 201.74563913 | -21.16237248 | 274.9546 | 54191.755162037 | 2007-04-01 18:07:26 | 54193.905150463 | 2007-04-03 21:43:25 | 702014010 | 100.8635 | 100 | 100.8635 | 100.8635 | 0 | 100.8635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.3121 | 95.3121 | 185.7439 | 1 | PROCESSED | 57538.0955324074 | 2016-05-30 02:17:34 | 54744 | 2008-10-05 00:00:00 | 54200.5657060185 | 2007-04-10 13:34:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 2 | AO2 | THE ORIGIN OF THE BROAD FE LINE IN THE SEYFERT 1 ARK 120 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702014010/ | Quick Look | ![]() |
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1021 | G359.0-0.9 NE | 266.7211 | -30.1578 | 265.918955 | -30.139926 | 267.135952 | -6.749255 | 359.09932581 | -0.86996543 | 100.9984 | 56720.9624537037 | 2014-03-04 23:05:56 | 56722.041875 | 2014-03-06 01:00:18 | 508057010 | 49.8156 | 50 | 49.8156 | 49.8396 | 0 | 49.8236 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 45.0097 | 45.0097 | 93.2479 | 1 | PROCESSED | 57613.9450925926 | 2016-08-13 22:40:56 | 57102 | 2015-03-21 00:00:00 | 56740.6678009259 | 2014-03-24 16:01:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508057010/ | Quick Look | ![]() |
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1022 | NGC 3516 | 166.6912 | 72.5534 | 165.838584 | 72.823761 | 123.385975 | 57.972253 | 133.24889589 | 42.41461595 | 284.0065 | 56441.4603009259 | 2013-05-29 11:02:50 | 56442.6355787037 | 2013-05-30 15:15:14 | 708006040 | 54.218 | 50 | 54.218 | 54.218 | 0 | 54.218 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.1207 | 53.1207 | 101.54 | 1 | PROCESSED | 57615.5831134259 | 2016-08-15 13:59:41 | 56383 | 2013-04-01 00:00:00 | 56503.6575347222 | 2013-07-30 15:46:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006040/ | Quick Look | ![]() |
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1023 | RXJ2056.6+4940 | 314.1926 | 49.6559 | 313.786825 | 49.462572 | 344.783467 | 62.123143 | 89.31769097 | 2.74712249 | 241.0011 | 55887.7886805556 | 2011-11-22 18:55:42 | 55888.5355208333 | 2011-11-23 12:51:09 | 406014010 | 42.3731 | 40 | 42.3811 | 42.3731 | 0 | 42.3731 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.6665 | 44.6665 | 64.524 | 1 | PROCESSED | 57603.9503356482 | 2016-08-03 22:48:29 | 56264 | 2012-12-03 00:00:00 | 55897.0994791667 | 2011-12-02 02:23:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISO | JAP | 6 | AO6 | SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406014010/ | Quick Look | ![]() |
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1024 | PSR J1044-5737 | 161.1338 | -57.616 | 160.63624 | -57.35288 | 199.24967 | -57.525785 | 286.57019106 | 1.16750605 | 109.1973 | 55542.2984259259 | 2010-12-12 07:09:44 | 55542.7292939815 | 2010-12-12 17:30:11 | 405013010 | 22.63 | 30 | 22.63 | 22.63 | 0 | 22.6358 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.9603 | 21.9603 | 37.2 | 0 | PROCESSED | 57554.3753125 | 2016-06-15 09:00:27 | 55917 | 2011-12-22 00:00:00 | 55550.9648148148 | 2010-12-20 23:09:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405013010/ | Quick Look | ![]() |
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1025 | VELA PWN S1 | 128.1818 | -46.8811 | 127.77491 | -46.709753 | 154.389152 | -62.054406 | 264.65396784 | -4.16648977 | 122.1894 | 56988.5541087963 | 2014-11-27 13:17:55 | 56988.8905324074 | 2014-11-27 21:22:22 | 509017010 | 15.4638 | 15 | 15.4638 | 15.4878 | 0 | 15.7838 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8238194444 | 2016-08-16 19:46:18 | 57368 | 2015-12-12 00:00:00 | 57002.4344328704 | 2014-12-11 10:25:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509017010/ | Quick Look | ![]() |
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1026 | G166.0+4.3_NE | 81.7708 | 42.9893 | 80.873891 | 42.947312 | 83.615806 | 19.731256 | 166.12860985 | 4.39756168 | 84.8043 | 56919.0138773148 | 2014-09-19 00:19:59 | 56920.3092824074 | 2014-09-20 07:25:22 | 509022010 | 54.3942 | 60 | 54.3942 | 61.5931 | 0 | 61.5931 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5656134259 | 2016-08-16 13:34:29 | 57296 | 2015-10-01 00:00:00 | 56940.6693981482 | 2014-10-10 16:03:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509022010/ | Quick Look | ![]() |
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1027 | AX J1620.7-4942 | 245.1985 | -49.7112 | 244.261349 | -49.592314 | 252.133944 | -27.795213 | 333.72306976 | 0.21790295 | 274.6004 | 56158.5209027778 | 2012-08-19 12:30:06 | 56159.5245717593 | 2012-08-20 12:35:23 | 407020010 | 42.2062 | 40 | 44.2713 | 44.2744 | 0 | 42.2062 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 44.8052 | 44.8052 | 86.7119 | 0 | PROCESSED | 57606.89875 | 2016-08-06 21:34:12 | 56582 | 2013-10-17 00:00:00 | 56212.7789930556 | 2012-10-12 18:41:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUO MAKISHIMA | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407020010/ | Quick Look | ![]() |
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1028 | NGC 4593 | 189.9148 | -5.3464 | 189.269905 | -5.071886 | 191.204626 | -0.990591 | 297.48422734 | 57.40070716 | 292.7769 | 56830.338275463 | 2014-06-22 08:07:07 | 56831.0988657407 | 2014-06-23 02:22:22 | 709014020 | 30.961 | 30 | 30.977 | 30.961 | 0 | 30.985 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.408 | 30.408 | 65.688 | 0 | PROCESSED | 57615.3154976852 | 2016-08-15 07:34:19 | 57212 | 2015-07-09 00:00:00 | 56846.5106365741 | 2014-07-08 12:15:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014020/ | Quick Look | ![]() |
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1029 | SWIFT J0250.7+4142 | 42.6629 | 41.6747 | 41.856234 | 41.468698 | 53.00104 | 24.122797 | 145.63636615 | -15.88173015 | 76.5152 | 56872.0541898148 | 2014-08-03 01:18:02 | 56873.8814930556 | 2014-08-04 21:09:21 | 709006010 | 82.1549 | 80 | 82.1629 | 82.1629 | 0 | 82.1549 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4596527778 | 2016-08-16 11:01:54 | 57267 | 2015-09-02 00:00:00 | 56902.7258564815 | 2014-09-02 17:25:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090019 | 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 two Compton thick AGN candidates in the 70 month 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 | YOSHIHIRO UEDA | JAP | 9 | AO9 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709006010/ | Quick Look | ![]() |
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1030 | NGC 4593 | 189.9131 | -5.3423 | 189.268209 | -5.067785 | 191.201461 | -0.987483 | 297.48045078 | 57.40464867 | 113.7512 | 57006.6309375 | 2014-12-15 15:08:33 | 57007.3023263889 | 2014-12-16 07:15:21 | 709014030 | 30.5312 | 30 | 30.5312 | 30.5392 | 0 | 30.5392 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5109722222 | 2016-08-17 12:15:48 | 57383 | 2015-12-27 00:00:00 | 57017.413900463 | 2014-12-26 09:56:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709014030/ | Quick Look | ![]() |
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1031 | SDSSJ084234.9+362503 | 130.6534 | 36.3531 | 129.855939 | 36.532969 | 123.380084 | 17.503637 | 186.36195466 | 37.19411123 | 266.2333 | 53868.6856018518 | 2006-05-13 16:27:16 | 53871.41625 | 2006-05-16 09:59:24 | 701004010 | 109.9556 | 120 | 109.9716 | 109.9636 | 109.9556 | 109.9636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 127.2306 | 127.2306 | 235.8948 | 1 | PROCESSED | 57534.3648032407 | 2016-05-26 08:45:19 | 54400 | 2007-10-27 00:00:00 | 53920.287650463 | 2006-07-04 06:54:13 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 1 | AO1 | THE MOST LUMINOUS TYPE 2 QSO IN SDSS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701004010/ | Quick Look | ![]() |
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1032 | PKS1510-089 | 228.2094 | -9.0956 | 227.535962 | -8.908847 | 228.284042 | 8.500549 | 351.2919833 | 40.14272744 | 102.2005 | 54858.1887615741 | 2009-01-27 04:31:49 | 54859.2258564815 | 2009-01-28 05:25:14 | 703005010 | 44.3054 | 40 | 44.3054 | 44.3054 | 0 | 44.3054 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6537 | 16.6537 | 89.5979 | 0 | PROCESSED | 57545.3861342593 | 2016-06-06 09:16:02 | 54557 | 2008-04-01 00:00:00 | 54880.5404282407 | 2009-02-18 12:58:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/703005010/ | Quick Look | ![]() |
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1033 | RXJ1713-3946 | 258.942 | -39.4278 | 258.077115 | -39.372323 | 261.109643 | -16.326699 | 347.8535904 | -0.62405701 | 268.0013 | 53998.4433912037 | 2006-09-20 10:38:29 | 53998.8467476852 | 2006-09-20 20:19:19 | 501071010 | 21.1741 | 20 | 21.1741 | 21.1981 | 21.1901 | 21.1821 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18.3387 | 18.3387 | 34.8399 | 0 | PROCESSED | 57535.634537037 | 2016-05-27 15:13:44 | 54526 | 2008-03-01 00:00:00 | 54020.8878009259 | 2006-10-12 21:18:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501071010/ | Quick Look | ![]() |
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1034 | FORNAX A LOBE BKG | 50.9375 | -37.5569 | 50.463091 | -37.733287 | 32.824918 | -53.528276 | 240.74738045 | -56.44161041 | 91.6954 | 56510.6236458333 | 2013-08-06 14:58:03 | 56511.9333912037 | 2013-08-07 22:24:05 | 808044010 | 54.4545 | 50 | 54.4625 | 54.4545 | 0 | 54.4705 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.8925 | 46.8925 | 113.1478 | 1 | PROCESSED | 57612.1934837963 | 2016-08-12 04:38:37 | 56955 | 2014-10-25 00:00:00 | 56587.7940046296 | 2013-10-22 19:03:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080056 | We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 8 | AO8 | COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808044010/ | Quick Look | ![]() |
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1035 | SGR 1806-20 | 272.1614 | -20.4072 | 271.417079 | -20.415895 | 272.018881 | 3.01842 | 9.99816367 | -0.23801419 | 88.2521 | 57120.8242592593 | 2015-04-08 19:46:56 | 57122.7405324074 | 2015-04-10 17:46:22 | 408014010 | 70.8195 | 70 | 70.8195 | 74.7739 | 0 | 74.8169 | 2 | 2 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0034143518 | 2016-08-18 00:04:55 | 57503 | 2016-04-25 00:00:00 | 57135.3828356482 | 2015-04-23 09:11:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080040 | Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. | GALACTIC POINT SOURCES | 4 | B | TERUAKI ENOTO | JAP | 8 | AO8 | ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408014010/ | Quick Look | ![]() |
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1036 | M81 | 148.8559 | 68.9951 | 147.832512 | 69.232018 | 119.540473 | 51.512284 | 142.17660014 | 40.93097712 | 281.1688 | 53863.0052083333 | 2006-05-08 00:07:30 | 53864.5209953704 | 2006-05-09 12:30:14 | 701022010 | 103.5186 | 100 | 103.5266 | 103.5266 | 103.5266 | 103.5186 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.7369 | 70.7369 | 130.9421 | 0 | PROCESSED | 57534.2973726852 | 2016-05-26 07:08:13 | 54397 | 2007-10-24 00:00:00 | 53913.9816550926 | 2006-06-27 23:33:35 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKESHI ITOH | JAP | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701022010/ | Quick Look | ![]() |
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1037 | SWIFT J0350.1-5019 | 57.5315 | -50.3337 | 57.174394 | -50.483946 | 28.735241 | -67.001155 | 259.74491819 | -49.02538792 | 320.5309 | 53838.5046875 | 2006-04-13 12:06:45 | 53838.6752199074 | 2006-04-13 16:12:19 | 701017010 | 2.6998 | 20 | 2.7158 | 2.7158 | 2.6998 | 2.7078 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1.1771 | 1.1771 | 9.165 | 0 | PROCESSED | 57533.4464930556 | 2016-05-25 10:42:57 | 54750 | 2008-10-11 00:00:00 | 53905.4679398148 | 2006-06-19 11:13:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017010/ | Quick Look | ![]() |
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1038 | V1223 SGR | 283.7562 | -31.163 | 282.951401 | -31.227311 | 281.856338 | -8.287095 | 4.95737746 | -14.35200731 | 75.0006 | 56745.6297453704 | 2014-03-29 15:06:50 | 56746.5002430556 | 2014-03-30 12:00:21 | 408019010 | 29.3493 | 180 | 29.3893 | 29.3493 | 0 | 29.3967 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 26.131 | 26.131 | 75.192 | 1 | PROCESSED | 57614.1428703704 | 2016-08-14 03:25:44 | 57121 | 2015-04-09 00:00:00 | 56756.7522800926 | 2014-04-09 18:03:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080086 | A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS. | GALACTIC POINT SOURCES | 4 | B | TAKAYUKI YUASA | JAP | 8 | AO8 | DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408019010/ | Quick Look | ![]() |
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1039 | N103B | 77.15 | -68.7359 | 77.208253 | -68.79772 | 330.089921 | -84.667648 | 279.60217418 | -34.399508 | 199.4598 | 55194.4728356482 | 2009-12-29 11:20:53 | 55200.6044560185 | 2010-01-04 14:30:25 | 804039010 | 223.8999 | 150 | 224.0108 | 223.8999 | 0 | 224.0028 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.096 | 46.096 | 129.9558 | 0 | PROCESSED | 57550.0511805556 | 2016-06-11 01:13:42 | 55584 | 2011-01-23 00:00:00 | 55218.4707060185 | 2010-01-22 11:17:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040080 | We aim to detect very low abundance lines, Cr and Mn, from SNR N103B in the Large Magellanic Cloud which is a low metaricity galaxy. It is known that a mass ratio of Mn to Cr synthesized in Type Ia supernovae is strongly correrated with the metaricity of the progenitor white dwarf. In the early Suzaku observation, we already detected the Cr line with about 3-sigma confidence level. In this follow-up observation, we detect the Cr and Mn lines with significant confidence, and determine the metaricity of the progenitor of SNR N103B. This will be the first measurement of the white dwarf's metaricity in the extra-galactic object. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TORU TAMAGAWA | JAP | 4 | AO4 | A MANGANESE LINE DETECTION FROM SNR N103B IN A LOW METARICITY GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804039010/ | Quick Look | ![]() |
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1040 | 1RXSJ170856.9-235936 | 257.2347 | -23.9931 | 256.473449 | -23.929773 | 258.342614 | -1.066908 | 359.58527393 | 9.56844908 | 95.2085 | 57099.2765625 | 2015-03-18 06:38:15 | 57099.6030324074 | 2015-03-18 14:28:22 | 409016010 | 15.3768 | 15 | 15.3768 | 15.3848 | 0 | 15.3768 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8053703704 | 2016-08-17 19:19:44 | 57479 | 2016-04-01 00:00:00 | 57112.4072106482 | 2015-03-31 09:46:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 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 | B | HIDEYUKI MORI | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409016010/ | Quick Look | ![]() |
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1041 | A478 OFFSET B | 63.3675 | 10.7352 | 62.68015 | 10.608912 | 63.410539 | -10.281556 | 182.20374123 | -28.1098658 | 260.0004 | 55601.549849537 | 2011-02-09 13:11:47 | 55602.6897685185 | 2011-02-10 16:33:16 | 805002010 | 45.3211 | 45 | 45.3211 | 45.3211 | 0 | 45.3211 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.2117 | 34.2117 | 98.4779 | 1 | PROCESSED | 57600.9178935185 | 2016-07-31 22:01:46 | 55983 | 2012-02-26 00:00:00 | 55617.4110763889 | 2011-02-25 09:51:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | ANDREW FABIAN | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805002010/ | Quick Look | ![]() |
1042 | N49 | 81.5075 | -66.0821 | 81.488489 | -66.123294 | 4.042744 | -86.564563 | 276.09278992 | -33.24378088 | 327.2258 | 56056.8032986111 | 2012-05-09 19:16:45 | 56060.6898148148 | 2012-05-13 16:33:20 | 807007010 | 184.543 | 190 | 184.559 | 184.543 | 0 | 184.559 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 206.5829 | 206.5829 | 335.7558 | 3 | PROCESSED | 57605.4699189815 | 2016-08-05 11:16:41 | 56527 | 2013-08-23 00:00:00 | 56161.1703935185 | 2012-08-22 04:05:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070036 | Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYUKI UCHIDA | JAP | 7 | AO7 | FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807007010/ | Quick Look | ![]() |
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1043 | GALACTIC CENTER GC2 | 265.779 | -29.1853 | 264.9833 | -29.162875 | 266.287161 | -5.798531 | 359.50136289 | 0.33591697 | 108.7998 | 54170.1638773148 | 2007-03-11 03:55:59 | 54170.7946064815 | 2007-03-11 19:04:14 | 501047010 | 25.599 | 25 | 25.607 | 25.599 | 0 | 25.623 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.0886 | 19.0886 | 54.4799 | 0 | PROCESSED | 57537.6398611111 | 2016-05-29 15:21:24 | 54736 | 2008-09-27 00:00:00 | 54182.2693865741 | 2007-03-23 06:27:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501047010/ | Quick Look | ![]() |
1044 | CENTAURUS CLUSTER NW | 191.8913 | -40.8227 | 191.202719 | -40.549873 | 208.557036 | -32.526985 | 302.14149361 | 22.04310508 | 292.0001 | 56850.5075462963 | 2014-07-12 12:10:52 | 56854.4064236111 | 2014-07-16 09:45:15 | 809007010 | 147.8889 | 150 | 147.8889 | 148.5689 | 0 | 148.5689 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6625 | 14.6625 | 46.016 | 1 | PROCESSED | 57615.4267476852 | 2016-08-15 10:14:31 | 57283 | 2015-09-18 00:00:00 | 56917.6316666667 | 2014-09-17 15:09:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090031 | We propose to observe the north-west offset (20'--40' or 0.4--0.8 r500) of the Centaurus cluster with a 150 ks exposure. A previous Suzaku observation with a 10 ks exposure yielded a very low Fe abundance (0.0-0.1 solar) in the ICM. With a 150 ks exposure, we will detect the Fe-K line of He-like Fe and derive Fe abundance with an accuracy of 0.05 solar. Then, we will be able to study the validity of the Fe abundance derived from the Fe L lines from cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 9 | AO9 | COMPARISON OF THE FE ABUNDANCES FROM THE L AND K LINES FROM THE CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809007010/ | Quick Look | ![]() |
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1045 | HIGH LAT. DIFFUSE B | 38.7468 | -52.2774 | 38.331334 | -52.495237 | 4.39034 | -61.411521 | 272.40280946 | -58.27300774 | 280.6379 | 53783.933900463 | 2006-02-17 22:24:49 | 53786.5211111111 | 2006-02-20 12:30:24 | 500027020 | 103.553 | 100 | 103.553 | 103.561 | 103.561 | 103.561 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.6094 | 68.6094 | 223.5238 | 3 | PROCESSED | 57533.0790972222 | 2016-05-25 01:53:54 | 54247 | 2007-05-27 00:00:00 | 54041.5670717593 | 2006-11-02 13:36:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027020/ | Quick Look | ![]() |
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1046 | GC14 | 267.1584 | -29.141 | 266.362704 | -29.125263 | 267.496319 | -5.724596 | 0.16624555 | -0.66947426 | 260.5381 | 54382.6950694444 | 2007-10-09 16:40:54 | 54383.1530555556 | 2007-10-10 03:40:24 | 502002010 | 23.1903 | 20 | 23.2063 | 23.1903 | 0 | 23.2063 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.9329 | 20.9329 | 39.5599 | 0 | PROCESSED | 57540.2209490741 | 2016-06-01 05:18:10 | 54771 | 2008-11-01 00:00:00 | 54402.7240740741 | 2007-10-29 17:22:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502002010/ | Quick Look | ![]() |
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1047 | Z348 | 16.7077 | 1.0407 | 16.065796 | 0.773597 | 15.79467 | -5.606239 | 131.03941429 | -61.58850223 | 247.9196 | 54110.9286689815 | 2007-01-10 22:17:17 | 54111.5259722222 | 2007-01-11 12:37:24 | 801050010 | 22.6477 | 23 | 22.6477 | 22.6477 | 0 | 22.6477 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.3403 | 21.3403 | 51.589 | 1 | PROCESSED | 57536.8362384259 | 2016-05-28 20:04:11 | 54735 | 2008-09-26 00:00:00 | 54133.0321643518 | 2007-02-02 00:46:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHIFUMI FUTAMASE | JAP | 1 | AO1 | THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801050010/ | Quick Look | ![]() |
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1048 | GC_LARGEPROJECT8 | 265.1842 | -30.7499 | 264.378561 | -30.724571 | 265.818402 | -7.37856 | 357.90048261 | -0.05223369 | 268.8911 | 54727.1991782407 | 2008-09-18 04:46:49 | 54728.3141203704 | 2008-09-19 07:32:20 | 503014010 | 55.3651 | 50 | 55.3651 | 55.3891 | 0 | 55.3651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.2069 | 51.2069 | 96.3118 | 1 | PROCESSED | 57543.8756481482 | 2016-06-04 21:00:56 | 54557 | 2008-04-01 00:00:00 | 54783.7018055556 | 2008-11-13 16:50:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503014010/ | Quick Look | ![]() |
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1049 | A2256BKG | 259.0594 | 79.1323 | 259.847378 | 79.183226 | 99.226233 | 77.073038 | 111.31764948 | 31.03227987 | 219.8044 | 56236.1893865741 | 2012-11-05 04:32:43 | 56237.0696875 | 2012-11-06 01:40:21 | 807025010 | 39.6865 | 40 | 39.6865 | 39.6865 | 0 | 39.6865 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9304 | 48.9304 | 76.0479 | 0 | PROCESSED | 57607.9668634259 | 2016-08-07 23:12:17 | 56630 | 2013-12-04 00:00:00 | 56264.5702199074 | 2012-12-03 13:41:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070058 | We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 7 | AO7 | THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807025010/ | Quick Look | ![]() |
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1050 | CYGNUS LOOP (P22) | 312.8353 | 32.4047 | 312.324184 | 32.216345 | 328.267069 | 47.560901 | 75.39493092 | -7.53123997 | 61.4354 | 54620.2981134259 | 2008-06-03 07:09:17 | 54620.7522453704 | 2008-06-03 18:03:14 | 503058010 | 19.2873 | 15 | 19.2873 | 19.2873 | 0 | 19.2873 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.2203 | 17.2203 | 39.212 | 0 | PROCESSED | 57542.7062037037 | 2016-06-03 16:56:56 | 55003 | 2009-06-21 00:00:00 | 54636.2807638889 | 2008-06-19 06:44:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503058010/ | Quick Look | ![]() |
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1051 | PKS0625-354 | 96.7724 | -35.4904 | 96.328951 | -35.45865 | 100.652009 | -58.681247 | 243.45420005 | -19.97253333 | 121.4596 | 55868.6502199074 | 2011-11-03 15:36:19 | 55871.6231597222 | 2011-11-06 14:57:21 | 706014010 | 100.7198 | 100 | 100.7278 | 100.7278 | 0 | 100.7198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.4342 | 86.4342 | 256.8138 | 4 | PROCESSED | 57603.7550231482 | 2016-08-03 18:07:14 | 56250 | 2012-11-19 00:00:00 | 55881.2887731482 | 2011-11-16 06:55:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 6 | AO6 | ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706014010/ | Quick Look | ![]() |
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1052 | A1631_E | 193.4806 | -15.4427 | 192.82259 | -15.171579 | 198.410093 | -8.910855 | 303.81684947 | 47.4247798 | 113.0006 | 56305.0111226852 | 2013-01-13 00:16:01 | 56305.7231944445 | 2013-01-13 17:21:24 | 807005010 | 20.5236 | 20 | 20.5236 | 20.5236 | 0 | 20.5476 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.1111 | 20.1111 | 61.5119 | 1 | PROCESSED | 57608.4784143518 | 2016-08-08 11:28:55 | 56703 | 2014-02-15 00:00:00 | 56337.4913425926 | 2013-02-14 11:47:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807005010/ | Quick Look | ![]() |
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1053 | BLOWOUT5 | 312.2204 | 31.3402 | 311.705242 | 31.154062 | 326.94204 | 46.789679 | 74.2273165 | -7.78955911 | 225.5762 | 55176.0660532407 | 2009-12-11 01:35:07 | 55176.7307175926 | 2009-12-11 17:32:14 | 504015010 | 30.4064 | 25 | 30.4064 | 30.4064 | 0 | 30.4064 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.6921 | 28.6921 | 57.4239 | 0 | PROCESSED | 57549.7666898148 | 2016-06-10 18:24:02 | 55555 | 2010-12-25 00:00:00 | 55189.2693981482 | 2009-12-24 06:27:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504015010/ | Quick Look | ![]() |
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1054 | NGC6946 | 308.6989 | 60.1968 | 308.436769 | 60.023263 | 358.020745 | 71.889708 | 95.74917907 | 11.70533663 | 79.9968 | 56060.7040393518 | 2012-05-13 16:53:49 | 56063.8903935185 | 2012-05-16 21:22:10 | 807035010 | 198.879 | 200 | 198.879 | 198.8958 | 0 | 198.8948 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 182.1955 | 182.1955 | 275.2756 | 3 | PROCESSED | 57605.4921296296 | 2016-08-05 11:48:40 | 56442 | 2013-05-30 00:00:00 | 56075.3809027778 | 2012-05-28 09:08:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070098 | Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. However, the origin of hot ISM is still unclear. We investigate the property of hot ISM according to luminosity of infrared emission, which is good tracer of star formation rate. If the hot ISM depend on the present activity of star formation, there are correlation between hot ISM and infrared emission. We propose the observation of the spiral galaxy NGC 6946. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SAORI KONAMI | JAP | 7 | AO7 | CLARIFICATION OF THE ORIGIN OF HOT ISM IN SPIRAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807035010/ | Quick Look | ![]() |
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1055 | IC 342 X2 | 56.548 | 68.1243 | 55.335293 | 67.96844 | 72.578132 | 46.699378 | 138.10903546 | 10.56584534 | 237.0509 | 55640.3693981482 | 2011-03-20 08:51:56 | 55641.8058101852 | 2011-03-21 19:20:22 | 705009020 | 75.4467 | 80 | 75.4707 | 75.4467 | 0 | 75.4787 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.2577 | 74.2577 | 124.0898 | 1 | PROCESSED | 57601.2497800926 | 2016-08-01 05:59:41 | 56019 | 2012-04-02 00:00:00 | 55652.0183680556 | 2011-04-01 00:26:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOKI ISOBE | JAP | 5 | AO5 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705009020/ | Quick Look | ![]() |
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1056 | EMS1274 | 285.5178 | -51.1684 | 284.542504 | -51.240609 | 280.974965 | -28.317711 | 345.57919311 | -22.40122796 | 103.8598 | 55299.2761921296 | 2010-04-13 06:37:43 | 55300.0056944445 | 2010-04-14 00:08:12 | 705014010 | 43.9253 | 40 | 43.9253 | 43.9333 | 0 | 43.9333 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.9581 | 34.9581 | 63.0159 | 0 | PROCESSED | 57551.1958333333 | 2016-06-12 04:42:00 | 55675 | 2011-04-24 00:00:00 | 55309.2111458333 | 2010-04-23 05:04:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705014010/ | Quick Look | ![]() |
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1057 | FILAMENT JUNCTION A | 165.6591 | 29.2454 | 164.978754 | 29.514668 | 155.086724 | 21.237285 | 201.46002358 | 65.98539565 | 289.5 | 56086.3001041667 | 2012-06-08 07:12:09 | 56088.1238425926 | 2012-06-10 02:58:20 | 807038010 | 69.1428 | 70 | 69.1588 | 69.1428 | 0 | 69.1588 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62.2992 | 62.2992 | 157.5558 | 1 | PROCESSED | 57605.6780787037 | 2016-08-05 16:16:26 | 56543 | 2013-09-08 00:00:00 | 56176.2765046296 | 2012-09-06 06:38:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070105 | We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NORIO SEKIYA | JAP | 7 | AO7 | EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807038010/ | Quick Look | ![]() |
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1058 | FILAMENT JUNCTION B | 173.7402 | 21.0892 | 173.087159 | 21.365728 | 165.694635 | 16.835806 | 227.90630551 | 71.55824615 | 299.4979 | 56088.1275115741 | 2012-06-10 03:03:37 | 56089.3439814815 | 2012-06-11 08:15:20 | 807039010 | 50.1063 | 50 | 50.1189 | 50.1063 | 0 | 50.1269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.9818 | 40.9818 | 105.0959 | 0 | PROCESSED | 57605.6509375 | 2016-08-05 15:37:21 | 56543 | 2013-09-08 00:00:00 | 56176.2814236111 | 2012-09-06 06:45:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070105 | We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NORIO SEKIYA | JAP | 7 | AO7 | EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807039010/ | Quick Look | ![]() |
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1059 | CYGNUS LOOP 9 | 312.876 | 30.2229 | 312.354142 | 30.034417 | 327.064975 | 45.541284 | 73.70000859 | -8.9268412 | 80.5836 | 55307.2796064815 | 2010-04-21 06:42:38 | 55308.0106597222 | 2010-04-22 00:15:21 | 505017010 | 29.9968 | 29 | 29.9968 | 29.9968 | 0 | 29.9968 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.6281 | 27.6281 | 63.1499 | 1 | PROCESSED | 57551.2933217593 | 2016-06-12 07:02:23 | 55287 | 2010-04-01 00:00:00 | 55364.2675347222 | 2010-06-17 06:25:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505017010/ | Quick Look | ![]() |
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1060 | 3C 59 VICINITY 1 | 32.0992 | 30.0806 | 31.374147 | 29.84386 | 40.280714 | 16.078754 | 142.1363254 | -29.90513458 | 254.1341 | 55940.8410763889 | 2012-01-14 20:11:09 | 55942.215474537 | 2012-01-16 05:10:17 | 506024010 | 55.8581 | 50 | 55.8581 | 55.8581 | 0 | 55.8581 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0404 | 46.0404 | 118.7379 | 1 | PROCESSED | 57604.3853356482 | 2016-08-04 09:14:53 | 56331 | 2013-02-08 00:00:00 | 55960.1998032407 | 2012-02-03 04:47:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUHIRO SAKAI | JAP | 6 | AO6 | STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506024010/ | Quick Look | ![]() |
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1061 | SWIFT J0544.4-4328 | 86.0099 | -43.419 | 85.632201 | -43.439311 | 82.65148 | -66.759602 | 249.50201979 | -30.05213281 | 308.9989 | 57140.9252083333 | 2015-04-28 22:12:18 | 57143.359212963 | 2015-05-01 08:37:16 | 709005010 | 84.362 | 100 | 84.362 | 92.7251 | 0 | 92.7171 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0749537037 | 2016-08-18 01:47:56 | 57527 | 2016-05-19 00:00:00 | 57160.6331597222 | 2015-05-18 15:11:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090018 | We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance 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 fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI TERASHIMA | JAP | 9 | AO9 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/709005010/ | Quick Look | ![]() |
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1062 | A2163BGD2 | 243.9063 | -6.5323 | 243.237281 | -6.40839 | 243.158854 | 14.509957 | 6.38161233 | 30.26602519 | 93.9997 | 57078.975787037 | 2015-02-25 23:25:08 | 57079.8335763889 | 2015-02-26 20:00:21 | 809011010 | 28.8166 | 30 | 28.8326 | 28.8166 | 0 | 28.8406 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6710763889 | 2016-08-17 16:06:21 | 57458 | 2016-03-11 00:00:00 | 57091.463587963 | 2015-03-10 11:07:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809011010/ | Quick Look | ![]() |
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1063 | HESSJ1507-622_CENTER | 226.7316 | -62.3464 | 225.708755 | -62.153708 | 244.337801 | -42.703137 | 317.95199358 | -3.49348671 | 301.8082 | 56181.4881712963 | 2012-09-11 11:42:58 | 56183.9549189815 | 2012-09-13 22:55:05 | 507025010 | 79.8869 | 80 | 79.8949 | 79.9029 | 0 | 79.8869 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.1958 | 74.1958 | 213.1037 | 1 | PROCESSED | 57607.0557986111 | 2016-08-07 01:20:21 | 56582 | 2013-10-17 00:00:00 | 56212.7347337963 | 2012-10-12 17:38:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | HIRONORI MATSUMOTO | JAP | 7 | AO7 | SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507025010/ | Quick Look | ![]() |
1064 | CAS A | 350.8607 | 58.8031 | 350.294827 | 58.528522 | 27.373119 | 54.842451 | 111.73599633 | -2.14263527 | 251.3043 | 56281.1375115741 | 2012-12-20 03:18:01 | 56283.3466666667 | 2012-12-22 08:19:12 | 507038010 | 102.411 | 100 | 102.419 | 102.411 | 0 | 102.426 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 126.7103 | 126.7103 | 190.8458 | 0 | PROCESSED | 57608.4566435185 | 2016-08-08 10:57:34 | 56683 | 2014-01-26 00:00:00 | 56316.9831365741 | 2013-01-24 23:35:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITOMO MAEDA | JAP | 7 | AO7 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507038010/ | Quick Look | ![]() |
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1065 | RXJ0134-4258 | 23.5686 | -42.9671 | 23.03099 | -43.222871 | 359.764354 | -47.882347 | 276.92816891 | -71.93227434 | 245.0998 | 56290.2726851852 | 2012-12-29 06:32:40 | 56292.2506481482 | 2012-12-31 06:00:56 | 707014010 | 81.429 | 50 | 81.4485 | 81.445 | 0 | 81.429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.1219 | 16.1219 | 37.6859 | 0 | PROCESSED | 57608.396087963 | 2016-08-08 09:30:22 | 56702 | 2014-02-14 00:00:00 | 56336.5473263889 | 2013-02-13 13:08:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROAKI TAKAHASHI | JAP | 7 | AO7 | X-RAY EMISSION FROM THE BRIGHTEST RADIO LOUD NARROW LINE SEYFERT 1 RXJ0134.2-4258 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707014010/ | Quick Look | ![]() |
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1066 | W28_SOUTH | 270.2522 | -23.558 | 269.490042 | -23.557374 | 270.221597 | -0.117322 | 6.38418356 | -0.23955939 | 89.9033 | 56738.9940393518 | 2014-03-22 23:51:25 | 56740.1793518518 | 2014-03-24 04:18:16 | 508006010 | 40.8518 | 100 | 40.8838 | 40.8518 | 0 | 40.8942 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 35.4568 | 35.4568 | 102.4078 | 1 | PROCESSED | 57614.1110648148 | 2016-08-14 02:39:56 | 57359 | 2015-12-03 00:00:00 | 56754.6877083333 | 2014-04-07 16:30:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080017 | A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP. | GALACTIC DIFFUSE EMISSION | 5 | A | MAKOTO SAWADA | JAP | 8 | AO8 | INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508006010/ | Quick Look | ![]() |
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1067 | CYG_COCOON2 | 306.1992 | 40.9463 | 305.753337 | 40.782769 | 326.198572 | 57.540222 | 78.99355785 | 1.86268914 | 253.1744 | 56603.8842939815 | 2013-11-07 21:13:23 | 56605.000162037 | 2013-11-09 00:00:14 | 508020010 | 46.4489 | 50 | 46.4489 | 46.4489 | 0 | 46.4489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.6569 | 44.6569 | 96.3739 | 3 | PROCESSED | 57613.2763194444 | 2016-08-13 06:37:54 | 57018 | 2014-12-27 00:00:00 | 56652.6462152778 | 2013-12-26 15:30:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080048 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density and spatial distribution in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 8 | AO8 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508020010/ | Quick Look | ![]() |
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1068 | VELA PWN W4 | 126.476 | -45.2086 | 126.060911 | -45.04388 | 150.453491 | -61.215385 | 262.5995548 | -4.15230559 | 95.0003 | 56591.4348726852 | 2013-10-26 10:26:13 | 56591.8813888889 | 2013-10-26 21:09:12 | 508045010 | 16.8588 | 15 | 16.8843 | 16.8588 | 0 | 16.8748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.0055 | 16.0055 | 38.578 | 0 | PROCESSED | 57613.1152893518 | 2016-08-13 02:46:01 | 57009 | 2014-12-18 00:00:00 | 56643.6542708333 | 2013-12-17 15:42:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, 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 western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508045010/ | Quick Look | ![]() |
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1069 | VELA PWN GEV6 | 128.0698 | -45.8067 | 127.654656 | -45.635799 | 153.081718 | -61.174639 | 263.73946045 | -3.59392918 | 121.6832 | 56987.9020717593 | 2014-11-26 21:38:59 | 56988.5530324074 | 2014-11-27 13:16:22 | 509016010 | 18.0926 | 15 | 18.1086 | 18.0926 | 0 | 18.1086 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8287037037 | 2016-08-16 19:53:20 | 57450 | 2016-03-03 00:00:00 | 57083.4111574074 | 2015-03-02 09:52:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509016010/ | Quick Look | ![]() |
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1070 | A399EAST | 44.8284 | 12.9677 | 44.143216 | 12.769088 | 46.15453 | -3.865608 | 164.75111172 | -39.30361408 | 72.1818 | 56529.3727777778 | 2013-08-25 08:56:48 | 56530.5036921296 | 2013-08-26 12:05:19 | 808007010 | 50.2768 | 50 | 50.2928 | 50.2768 | 0 | 50.3008 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3039 | 46.3039 | 97.684 | 0 | PROCESSED | 57612.4010069444 | 2016-08-12 09:37:27 | 56956 | 2014-10-26 00:00:00 | 56587.522349537 | 2013-10-22 12:32:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHITAKA ISHISAKI | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808007010/ | Quick Look | ![]() |
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1071 | A2744_NE | 3.7189 | -30.3078 | 3.087931 | -30.585769 | 350.157324 | -29.032997 | 9.14048559 | -81.37985976 | 233.5002 | 56616.3325694445 | 2013-11-20 07:58:54 | 56618.5994791667 | 2013-11-22 14:23:15 | 808008010 | 82.773 | 80 | 82.781 | 82.781 | 0 | 82.773 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.7365 | 71.7365 | 195.8377 | 2 | PROCESSED | 57613.443900463 | 2016-08-13 10:39:13 | 56995 | 2014-12-04 00:00:00 | 56629.7456481482 | 2013-12-03 17:53:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080005 | We propose an additional 80ks pointing to complete our mapping of A2744 out to large radii and constrain the thermodynamical history of the cluster growth. A2744 is a multiple merger, nicknamed Pandora's cluster. Our analysis of existing Suzaku data suggest that this cluster has an anisotropic temperature structure near the virial radius and there is not a simple correlation between temperature and surface mass density of member galaxies. With proposed observations, we can determine, for the first time, the temperature and entropy profiles near the radio relic in the northeast and further test a scenario of gas heating and shock propagation in the cluster outskirts. Suzaku is most suited for this study because of the lowest background and excellent sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 8 | AO8 | REVEALING THE THERMODYNAMICAL EVOLUTION IN THE PANDORA'S CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808008010/ | Quick Look | ![]() |
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1072 | COMA SUBHALO1 | 195.4003 | 29.028 | 194.800096 | 29.29674 | 181.356993 | 32.514724 | 73.80298118 | 87.06170231 | 296.7987 | 56451.3782638889 | 2013-06-08 09:04:42 | 56452.0681712963 | 2013-06-09 01:38:10 | 808018010 | 31.1826 | 30 | 31.1906 | 31.1826 | 0 | 31.1906 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.8197 | 28.8197 | 59.604 | 1 | PROCESSED | 57611.5003935185 | 2016-08-11 12:00:34 | 56869 | 2014-07-31 00:00:00 | 56503.6225462963 | 2013-07-30 14:56:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808018010/ | Quick Look | ![]() |
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1073 | A3627_NORTH | 243.656 | -60.6115 | 242.575411 | -60.485559 | 253.80029 | -38.641261 | 325.45745985 | -6.96421785 | 306.0001 | 56545.808912037 | 2013-09-10 19:24:50 | 56546.5556828704 | 2013-09-11 13:20:11 | 808058010 | 51.8996 | 50 | 51.9316 | 51.9236 | 0 | 51.8996 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43.0284 | 43.0284 | 64.5119 | 1 | PROCESSED | 57612.6119097222 | 2016-08-12 14:41:09 | 56956 | 2014-10-26 00:00:00 | 56588.8328935185 | 2013-10-23 19:59:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080097 | We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATSUHIRO HAYASHI | JAP | 8 | AO8 | OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808058010/ | Quick Look | ![]() |
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1074 | A2104S | 235.0317 | -3.4139 | 234.377731 | -3.253044 | 233.528717 | 15.709214 | 2.71321412 | 39.14413145 | 117.9978 | 54120.3324884259 | 2007-01-20 07:58:47 | 54120.8266087963 | 2007-01-20 19:50:19 | 801004010 | 17.3234 | 20 | 17.3234 | 17.3234 | 0 | 17.3234 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.8291 | 13.8291 | 42.6819 | 1 | PROCESSED | 57536.8854166667 | 2016-05-28 21:15:00 | 54750 | 2008-10-11 00:00:00 | 54137.3891898148 | 2007-02-06 09:20:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801004010/ | Quick Look | ![]() |
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1075 | A3627SE | 243.9338 | -61.0124 | 242.844844 | -60.887647 | 254.085676 | -39.001294 | 325.27404641 | -7.34625911 | 86.273 | 54869.3739236111 | 2009-02-07 08:58:27 | 54870.87875 | 2009-02-08 21:05:24 | 803033010 | 52.6995 | 50 | 52.7395 | 52.6995 | 0 | 52.7235 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.1839 | 48.1839 | 129.9878 | 3 | PROCESSED | 57545.4958912037 | 2016-06-06 11:54:05 | 55330 | 2010-05-14 00:00:00 | 54881.3769212963 | 2009-02-19 09:02:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030117 | We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SHO NISHINO | JAP | 3 | AO3 | OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803033010/ | Quick Look | ![]() |
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1076 | A1631_C | 193.2396 | -15.343 | 192.582019 | -15.071616 | 198.154189 | -8.910152 | 303.4747971 | 47.52714603 | 112.9996 | 56304.4910069444 | 2013-01-12 11:47:03 | 56305.0106944444 | 2013-01-13 00:15:24 | 807004010 | 23.8057 | 20 | 23.8137 | 23.8057 | 0 | 23.8057 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.9369 | 19.9369 | 44.8719 | 0 | PROCESSED | 57608.4757986111 | 2016-08-08 11:25:09 | 56704 | 2014-02-16 00:00:00 | 56337.5260300926 | 2013-02-14 12:37:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807004010/ | Quick Look | ![]() |
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1077 | A548W | 86.2487 | -25.8437 | 85.742711 | -25.86316 | 84.832695 | -49.218426 | 230.35478522 | -25.32458233 | 240.9996 | 56337.0028819444 | 2013-02-14 00:04:09 | 56339.3300462963 | 2013-02-16 07:55:16 | 807033010 | 99.3707 | 100 | 99.3707 | 99.3707 | 0 | 99.3707 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 85.3446 | 85.3446 | 201.0437 | 2 | PROCESSED | 57610.6626041667 | 2016-08-10 15:54:09 | 56738 | 2014-03-22 00:00:00 | 56372.6069444445 | 2013-03-21 14:34:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070085 | Abell 548 west is a near-by (z=0.0424) poor cluster with an X-ray temperature of 3.4 keV. It has two bright radio relic emission located to the north (Feretti et al. 2006), and a candidate shock-front located near the relics (Solovyeva et al. 2008). The cluster X-ray luminosity is more than an order of magnitude dimmer when plotted in the kT-Lx relation. Combined with its too high galaxy velocity dispersion, we consider this target as a critical merger of two group-sized systems, which is a very rare case in our vicinity. Using Suzaku, we will parametrize the low surface brightness candidate shock region, to identify the temperature jump, which cannot be detected with XMM. We will also investigate the IC emission from the relics to measure the lower limit of its magnetic field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO NAKAZAWA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A MERGING GROUP CANDIDATE ABELL 548 WEST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807033010/ | Quick Look | ![]() |
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1078 | 3EGJ1234 1318_3 | 188.2697 | -13.5708 | 187.619846 | -13.295052 | 192.969415 | -9.186347 | 296.11455637 | 49.05777767 | 113.9119 | 54445.0609375 | 2007-12-11 01:27:45 | 54445.8543171296 | 2007-12-11 20:30:13 | 802004010 | 1.602 | 30 | 1.602 | 29.7794 | 0 | 29.7794 | 1 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3048 | 26.3048 | 68.5198 | 0 | PROCESSED | 57637.5213888889 | 2016-09-06 12:30:48 | 54999 | 2009-06-17 00:00:00 | 54633.6933217593 | 2008-06-16 16:38:23 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOMONORI TOTANI | JAP | 2 | AO2 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802004010/ | Quick Look | ![]() |
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1079 | 3EGJ1234 1318_4 | 188.5214 | -13.4715 | 187.871329 | -13.195924 | 193.15662 | -8.997759 | 296.47032219 | 49.18242085 | 113.9125 | 54445.8547453704 | 2007-12-11 20:30:50 | 54446.4655555556 | 2007-12-12 11:10:24 | 802005010 | 20.1392 | 20 | 0 | 20.1392 | 0 | 20.1552 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 20.0064 | 20.0064 | 52.7719 | 0 | PROCESSED | 57540.846875 | 2016-06-01 20:19:30 | 55000 | 2009-06-18 00:00:00 | 54633.6925347222 | 2008-06-16 16:37:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOMONORI TOTANI | JAP | 2 | AO2 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802005010/ | Quick Look | ![]() |
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1080 | A3627CENTER | 243.5672 | -60.8499 | 242.482666 | -60.723566 | 253.815365 | -38.883288 | 325.25917104 | -7.10560665 | 129.9148 | 54905.9231597222 | 2009-03-15 22:09:21 | 54906.6072222222 | 2009-03-16 14:34:24 | 803032010 | 46.0339 | 50 | 46.0388 | 46.0419 | 0 | 46.0339 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43.3969 | 43.3969 | 59.0959 | 0 | PROCESSED | 57545.823900463 | 2016-06-06 19:46:25 | 55330 | 2010-05-14 00:00:00 | 54917.2613657407 | 2009-03-27 06:16:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030117 | We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SHO NISHINO | JAP | 3 | AO3 | OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803032010/ | Quick Look | ![]() |
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1081 | A3112SE | 49.8254 | -44.4068 | 49.393169 | -44.587264 | 25.763903 | -59.224971 | 253.09009544 | -55.79916534 | 40.0009 | 56832.6869791667 | 2014-06-24 16:29:15 | 56834.034849537 | 2014-06-26 00:50:11 | 809026010 | 49.8443 | 45 | 49.8523 | 49.8443 | 0 | 49.8603 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.2246 | 44.2246 | 116.4418 | 0 | PROCESSED | 57615.347662037 | 2016-08-15 08:20:38 | 57212 | 2015-07-09 00:00:00 | 56846.5576273148 | 2014-07-08 13:22:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809026010/ | Quick Look | ![]() |
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1082 | ZWCL 2341.1+0000 | 355.9117 | 0.3303 | 355.271077 | 0.05271 | 356.374003 | 1.928516 | 89.48591025 | -58.06988626 | 66.2761 | 54644.6873148148 | 2008-06-27 16:29:44 | 54645.9258912037 | 2008-06-28 22:13:17 | 803001010 | 50.7413 | 40 | 50.7493 | 50.7413 | 0 | 50.7573 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.4767 | 39.4767 | 107.0018 | 0 | PROCESSED | 57542.9355671296 | 2016-06-03 22:27:13 | 55021 | 2009-07-09 00:00:00 | 54655.1925578704 | 2008-07-08 04:37:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030002 | Recent advances in observational cosmology have revealed that the large-scale distribution of galaxies in the universe has a honeycomb-like structure. However it is still a mystery how such diverse structures emerge out of primeval density fluctuations that grew over time due to the effects of gravity. An important role in the structure-formation process is played by the large-scale shocks that form as the primordial density fluctuations become non-linear and the accretion flows on collapsing structures become supersonic. In order to understand cosmic-rays acceleration greater than 1000 TeV and the structure formation in the early universe, we propose a 40 ksec observation of the proto-cluster filament ZwCl 2341.1+0000 (z = 0.27) with Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JUN KATAOKA | JAP | 3 | AO3 | COSMIC-RAY ACCELERATION AND STRUCTURE FORMATION IN A MPC-SCALE FILAMENTARY NETWORK OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803001010/ | Quick Look | ![]() |
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1083 | A3112N | 49.535 | -43.9764 | 49.09877 | -44.157944 | 25.831039 | -58.74808 | 252.47008016 | -56.12805661 | 40.0008 | 56831.1105439815 | 2014-06-23 02:39:11 | 56832.6863194444 | 2014-06-24 16:28:18 | 809027010 | 49.5323 | 45 | 49.5323 | 49.8923 | 0 | 49.8923 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.2405 | 44.2405 | 136.1356 | 2 | PROCESSED | 57615.3567476852 | 2016-08-15 08:33:43 | 57212 | 2015-07-09 00:00:00 | 56846.5678703704 | 2014-07-08 13:37:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809027010/ | Quick Look | ![]() |
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1084 | PKS 0558-504 VIC 2 | 88.9376 | -50.5474 | 88.635341 | -50.553317 | 87.569877 | -73.980493 | 257.96524127 | -29.21937587 | 349.9999 | 56822.2473148148 | 2014-06-14 05:56:08 | 56824.093900463 | 2014-06-16 02:15:13 | 809035010 | 60.1523 | 60 | 60.1523 | 62.1728 | 0 | 62.1888 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.7476 | 56.7476 | 159.5318 | 2 | PROCESSED | 57615.2572800926 | 2016-08-15 06:10:29 | 57204 | 2015-07-01 00:00:00 | 56835.7714236111 | 2014-06-27 18:30:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090086 | We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAZUHIRO SAKAI | JAP | 9 | AO9 | IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809035010/ | Quick Look | ![]() |
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1085 | RXCJ0234.5-5830 | 38.6494 | -58.5096 | 38.292773 | -58.727647 | 354.405777 | -65.806692 | 280.27566127 | -53.84414378 | 249.7915 | 55212.1975115741 | 2010-01-16 04:44:25 | 55212.4794328704 | 2010-01-16 11:30:23 | 804003010 | 13.5665 | 10 | 13.5745 | 13.5665 | 0 | 13.5825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7771 | 10.7771 | 24.3559 | 0 | PROCESSED | 57550.1603125 | 2016-06-11 03:50:51 | 55594 | 2011-02-02 00:00:00 | 55228.0359722222 | 2010-02-01 00:51:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804003010/ | Quick Look | ![]() |
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1086 | NGC 6251 | 247.2266 | 82.6554 | 248.601394 | 82.760043 | 99.818913 | 73.103839 | 115.95247359 | 31.23340212 | 185.0319 | 55885.7751736111 | 2011-11-20 18:36:15 | 55887.7821875 | 2011-11-22 18:46:21 | 806015010 | 100.1571 | 100 | 100.1651 | 100.1571 | 0 | 100.1651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.5943 | 98.5943 | 173.3759 | 1 | PROCESSED | 57603.983599537 | 2016-08-03 23:36:23 | 56264 | 2012-12-03 00:00:00 | 55897.1810300926 | 2011-12-02 04:20:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060045 | Suzaku observations of lobes of Fanaroff-Riley Type-1 Radio Galaxies NGC 6251 and IC 4296 are proposed. Utilizing the high sensitivity for the diffuse sources of Suzaku, we propose precise measurement of the inverse-Compton X-rays form Fanaroff-Riley Type-1 Radio lobes to determine the electron energy density. Comparing the electron energy density with those of Fanaroff-Riley Type-2 Radio lobes, we examine an evolution model of the radio galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROMI SETA | JAP | 6 | AO6 | OBSERVATIONS OF LOBES OF FANAROFF-RILEY TYPE-1 RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806015010/ | Quick Look | ![]() |
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1087 | A1674_NE | 196.3328 | 67.5805 | 195.880568 | 67.847887 | 143.656053 | 62.969177 | 120.89335151 | 49.49272287 | 327.6637 | 56799.3349189815 | 2014-05-22 08:02:17 | 56800.5487962963 | 2014-05-23 13:10:16 | 809042010 | 60.5303 | 40 | 0 | 60.5303 | 0 | 0 | 0 | 3 | 0 | 0 | 1 | 0 | 0 | 61.6512 | 61.6512 | 104.8597 | 2 | PROCESSED | 57615.1320023148 | 2016-08-15 03:10:05 | 57626 | 2016-08-26 00:00:00 | 56818.712650463 | 2014-06-10 17:06:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042010/ | Quick Look | ![]() |
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1088 | NGC 5044 SOUTH 30' | 198.7482 | -16.8629 | 198.081082 | -16.598731 | 203.683963 | -8.265963 | 311.00467544 | 45.63931299 | 110.0008 | 55222.2581365741 | 2010-01-26 06:11:43 | 55224.0190277778 | 2010-01-28 00:27:24 | 804014010 | 65.1766 | 60 | 65.1846 | 65.1766 | 0 | 65.1846 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1628 | 44.1628 | 152.1218 | 1 | PROCESSED | 57550.4424768518 | 2016-06-11 10:37:10 | 55602 | 2011-02-10 00:00:00 | 55236.2169675926 | 2010-02-09 05:12:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040013 | Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804014010/ | Quick Look | ![]() |
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1089 | A1674_Center | 195.9709 | 67.5098 | 195.513873 | 67.777673 | 143.620899 | 62.81475 | 121.09709791 | 49.57408901 | 327.6687 | 56800.5493171296 | 2014-05-23 13:11:01 | 56801.6251736111 | 2014-05-24 15:00:15 | 809042020 | 56.0395 | 40 | 0 | 56.0395 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 56.0296 | 56.0296 | 92.9376 | 0 | PROCESSED | 57615.1546180556 | 2016-08-15 03:42:39 | 57626 | 2016-08-26 00:00:00 | 56862.7934837963 | 2014-07-24 19:02:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042020/ | Quick Look | ![]() |
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1090 | A1674_Offset | 196.9691 | 67.2995 | 196.521421 | 67.56601 | 144.467706 | 63.021341 | 120.47867852 | 49.75037622 | 328.362 | 56801.6258333333 | 2014-05-24 15:01:12 | 56802.7363541667 | 2014-05-25 17:40:21 | 809042030 | 67.4756 | 40 | 0 | 67.4756 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 63.4535 | 63.4535 | 95.9418 | 0 | PROCESSED | 57615.1567013889 | 2016-08-15 03:45:39 | 57626 | 2016-08-26 00:00:00 | 56818.7013541667 | 2014-06-10 16:49:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042030/ | Quick Look | ![]() |
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1091 | A1674_SW | 195.6324 | 67.4673 | 195.171121 | 67.735617 | 143.543166 | 62.683089 | 121.29194244 | 49.62561755 | 325.0183 | 56802.7378472222 | 2014-05-25 17:42:30 | 56804.2224537037 | 2014-05-27 05:20:20 | 809042040 | 6.3772 | 40 | 6.3772 | 90.8498 | 0 | 6.3772 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 71.0768 | 71.0768 | 103.0788 | 1 | PROCESSED | 57615.185787037 | 2016-08-15 04:27:32 | 57626 | 2016-08-26 00:00:00 | 56818.7191203704 | 2014-06-10 17:15:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042040/ | Quick Look | ![]() |
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1092 | THE MOON | 135.7323 | 11.3866 | 135.051985 | 11.584787 | 134.824104 | -5.224923 | 217.57839096 | 34.30376044 | 284.6998 | 56783.949849537 | 2014-05-06 22:47:47 | 56784.073125 | 2014-05-07 01:45:18 | 809001040 | 5.5556 | 45 | 5.5556 | 5.5714 | 0 | 5.5636 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.574 | 4.574 | 10.6479 | 0 | PROCESSED | 57615.0559606482 | 2016-08-15 01:20:35 | 57162 | 2015-05-20 00:00:00 | 56796.5928240741 | 2014-05-19 14:13:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001040/ | Quick Look | ![]() |
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1093 | THE MOON | 137.1548 | 11.8786 | 136.473781 | 12.081578 | 136.019585 | -4.350943 | 217.75615417 | 35.77416951 | 105.7184 | 56975.0809490741 | 2014-11-14 01:56:34 | 56975.1987615741 | 2014-11-14 04:46:13 | 809001190 | 6.413 | 45 | 6.413 | 6.413 | 0 | 6.413 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.77 | 2016-08-16 18:28:48 | 57358 | 2015-12-02 00:00:00 | 56992.4097916667 | 2014-12-01 09:50:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001190/ | Quick Look | ![]() |
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1094 | RXCJ2157.4-0747 NE | 329.3742 | -7.8003 | 328.713545 | -8.039068 | 328.756448 | 4.373785 | 49.81973283 | -44.55901105 | 250.0004 | 56972.5422453704 | 2014-11-11 13:00:50 | 56973.0835069445 | 2014-11-12 02:00:15 | 809021010 | 18.63 | 20 | 18.646 | 18.63 | 0 | 18.646 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.764375 | 2016-08-16 18:20:42 | 57352 | 2015-11-26 00:00:00 | 56986.4078240741 | 2014-11-25 09:47:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809021010/ | Quick Look | ![]() |
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1095 | A2029_2 | 227.8527 | 6.0108 | 227.233944 | 6.198717 | 223.562452 | 22.914786 | 6.92100367 | 50.6092725 | 112.9534 | 55224.3333912037 | 2010-01-28 08:00:05 | 55224.9794444444 | 2010-01-28 23:30:24 | 804024020 | 26.0185 | 22 | 26.0225 | 26.0185 | 0 | 26.0262 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.9033 | 15.9033 | 55.814 | 0 | PROCESSED | 57550.4048726852 | 2016-06-11 09:43:01 | 55637 | 2011-03-17 00:00:00 | 55271.0156365741 | 2010-03-16 00:22:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024020/ | Quick Look | ![]() |
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1096 | A1246_CENTER | 170.9992 | 21.4865 | 170.340675 | 21.761183 | 163.096496 | 16.147963 | 224.00399917 | 69.32667171 | 120.0006 | 55151.2043981482 | 2009-11-16 04:54:20 | 55152.274525463 | 2009-11-17 06:35:19 | 804028010 | 48.4564 | 40 | 48.4724 | 48.4564 | 0 | 48.4724 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.2156 | 37.2156 | 92.4339 | 0 | PROCESSED | 57549.4081018518 | 2016-06-10 09:47:40 | 55531 | 2010-12-01 00:00:00 | 55162.1616319445 | 2009-11-27 03:52:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040053 | We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 4 | AO4 | MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804028010/ | Quick Look | ![]() |
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1097 | A1246_OFF | 171.128 | 21.4191 | 170.469781 | 21.693883 | 163.239064 | 16.135503 | 224.30142226 | 69.41574013 | 120.0005 | 55163.0212152778 | 2009-11-28 00:30:33 | 55164.9606365741 | 2009-11-29 23:03:19 | 804029010 | 80.3804 | 80 | 80.3964 | 80.3804 | 0 | 80.391 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.158 | 55.158 | 167.5558 | 1 | PROCESSED | 57549.6578472222 | 2016-06-10 15:47:18 | 55549 | 2010-12-19 00:00:00 | 55181.239849537 | 2009-12-16 05:45:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040053 | We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 4 | AO4 | MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804029010/ | Quick Look | ![]() |
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1098 | AWM7 45' EAST | 44.4244 | 41.5971 | 43.612656 | 41.396941 | 54.340636 | 23.633961 | 146.87973673 | -15.32937684 | 74.1373 | 55780.4446527778 | 2011-08-07 10:40:18 | 55781.3155208333 | 2011-08-08 07:34:21 | 806008010 | 36.8794 | 35 | 36.8794 | 36.8794 | 0 | 36.8794 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.7039 | 35.7039 | 75.2399 | 0 | PROCESSED | 57602.7523726852 | 2016-08-02 18:03:25 | 56169 | 2012-08-30 00:00:00 | 55802.4637384259 | 2011-08-29 11:07:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806008010/ | Quick Look | ![]() |
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1099 | A3376 EAST | 90.8243 | -39.9606 | 90.417011 | -39.957602 | 91.41993 | -63.398251 | 246.56739968 | -25.79165375 | 80.8001 | 56549.3239699074 | 2013-09-14 07:46:31 | 56551.6953472222 | 2013-09-16 16:41:18 | 808028010 | 81.5734 | 81 | 81.5734 | 81.5734 | 0 | 81.5734 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.1814 | 75.1814 | 204.8578 | 2 | PROCESSED | 57612.6739467593 | 2016-08-12 16:10:29 | 56956 | 2014-10-26 00:00:00 | 56588.6883449074 | 2013-10-23 16:31:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808028010/ | Quick Look | ![]() |
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1100 | A2199_NE | 247.516 | 39.7841 | 247.089512 | 39.891486 | 233.470249 | 60.402163 | 63.26645529 | 43.42583068 | 143.5992 | 56661.6024074074 | 2014-01-04 14:27:28 | 56662.5572222222 | 2014-01-05 13:22:24 | 808050010 | 44.1631 | 40 | 44.1711 | 44.1631 | 0 | 44.1711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.3531 | 42.3531 | 82.4919 | 1 | PROCESSED | 57613.7484953704 | 2016-08-13 17:57:50 | 57079 | 2015-02-26 00:00:00 | 56713.7287037037 | 2014-02-25 17:29:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080067 | We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 8 | AO8 | COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808050010/ | Quick Look | ![]() |
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1101 | A3627_WEST | 243.1701 | -60.6984 | 242.089882 | -60.570358 | 253.528582 | -38.78018 | 325.22376786 | -6.86207305 | 306.0002 | 56546.5563425926 | 2013-09-11 13:21:08 | 56547.2535185185 | 2013-09-12 06:05:04 | 808059010 | 52.7998 | 50 | 52.7998 | 52.8237 | 0 | 52.8078 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8968 | 42.8968 | 60.2319 | 0 | PROCESSED | 57612.5956481482 | 2016-08-12 14:17:44 | 56956 | 2014-10-26 00:00:00 | 56588.7134837963 | 2013-10-23 17:07:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080097 | We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATSUHIRO HAYASHI | JAP | 8 | AO8 | OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808059010/ | Quick Look | ![]() |
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1102 | FJ1336+3553_OFFSET | 203.9396 | 35.8517 | 203.380018 | 36.106643 | 185.299819 | 41.923502 | 78.4395295 | 77.15761363 | 299.9998 | 56836.6568171296 | 2014-06-28 15:45:49 | 56837.6530092593 | 2014-06-29 15:40:20 | 809041010 | 43.307 | 45 | 43.307 | 45.5019 | 0 | 45.5179 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3386458333 | 2016-08-15 08:07:39 | 57212 | 2015-07-09 00:00:00 | 56846.5938425926 | 2014-07-08 14:15:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809041010/ | Quick Look | ![]() |
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1103 | CEN_A_LOBE_N5 | 198.8206 | -42.0777 | 198.100689 | -41.813564 | 214.682372 | -31.301214 | 307.6547721 | 20.57528449 | 295.9847 | 56865.6873032407 | 2014-07-27 16:29:43 | 56867.2502430556 | 2014-07-29 06:00:21 | 809006010 | 51.9392 | 50 | 51.9392 | 52.5746 | 0 | 52.5746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6586 | 10.6586 | 20.936 | 0 | PROCESSED | 57615.4722916667 | 2016-08-15 11:20:06 | 57267 | 2015-09-02 00:00:00 | 56898.3358449074 | 2014-08-29 08:03:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809006010/ | Quick Look | ![]() |
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1104 | THE MOON | 134.2483 | 11.6812 | 133.56589 | 11.874254 | 133.339832 | -5.352995 | 216.51758385 | 33.11115118 | 281.9606 | 56783.8139699074 | 2014-05-06 19:32:07 | 56783.948125 | 2014-05-06 22:45:18 | 809001030 | 6.4899 | 45 | 6.4979 | 6.4899 | 0 | 6.4979 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.02 | 7.02 | 11.5839 | 0 | PROCESSED | 57615.0497222222 | 2016-08-15 01:11:36 | 57162 | 2015-05-20 00:00:00 | 56793.5289930556 | 2014-05-16 12:41:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001030/ | Quick Look | ![]() |
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1105 | THE MOON | 140.1926 | 10.5514 | 139.518228 | 10.7642 | 139.270066 | -4.724239 | 220.86178985 | 37.88683751 | 291.2213 | 56784.325775463 | 2014-05-07 07:49:07 | 56784.4480555556 | 2014-05-07 10:45:12 | 809001070 | 6.405 | 45 | 6.405 | 6.405 | 0 | 6.405 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.677 | 6.677 | 10.5539 | 0 | PROCESSED | 57615.0674074074 | 2016-08-15 01:37:04 | 57218 | 2015-07-15 00:00:00 | 56852.581875 | 2014-07-14 13:57:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001070/ | Quick Look | ![]() |
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1106 | RXCJ2157.4-0747 SE | 329.2877 | -7.568 | 328.627588 | -7.806552 | 328.755658 | 4.621414 | 50.03773919 | -44.36639016 | 250.0002 | 56973.0839351852 | 2014-11-12 02:00:52 | 56973.6668055556 | 2014-11-12 16:00:12 | 809022010 | 25.9584 | 20 | 25.9744 | 25.9584 | 0 | 25.9824 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7636111111 | 2016-08-16 18:19:36 | 57352 | 2015-11-26 00:00:00 | 56986.4089351852 | 2014-11-25 09:48:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809022010/ | Quick Look | ![]() |
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1107 | RXCJ2157.4-0747 SW | 329.5619 | -7.7328 | 328.901524 | -7.972036 | 328.954889 | 4.373264 | 50.03497203 | -44.68420804 | 250.0004 | 56976.2027893518 | 2014-11-15 04:52:01 | 56976.7307175926 | 2014-11-15 17:32:14 | 809023010 | 20.9188 | 20 | 20.9188 | 20.9188 | 0 | 20.9188 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.786099537 | 2016-08-16 18:51:59 | 57361 | 2015-12-05 00:00:00 | 56993.4286921296 | 2014-12-02 10:17:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809023010/ | Quick Look | ![]() |
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1108 | A3112E | 49.9177 | -44.1055 | 49.483567 | -44.285626 | 26.168536 | -58.996914 | 252.54334877 | -55.82694751 | 25.0007 | 56829.3656134259 | 2014-06-21 08:46:29 | 56830.3266435185 | 2014-06-22 07:50:22 | 809024010 | 33.435 | 45 | 33.435 | 34.195 | 0 | 34.219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.293 | 30.293 | 82.9918 | 1 | PROCESSED | 57615.3104398148 | 2016-08-15 07:27:02 | 57239 | 2015-08-05 00:00:00 | 56873.1925 | 2014-08-04 04:37:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809024010/ | Quick Look | ![]() |
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1109 | NGC 3516 | 166.6817 | 72.5579 | 165.82888 | 72.82825 | 123.376111 | 57.97325 | 133.24892211 | 42.40929053 | 306.0068 | 57154.3345023148 | 2015-05-12 08:01:41 | 57157.0348611111 | 2015-05-15 00:50:12 | 710009010 | 117.7012 | 120 | 117.7012 | 123.0032 | 0 | 124.7632 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6915277778 | 2016-08-18 16:35:48 | 57593 | 2016-07-24 00:00:00 | 57224.4439467593 | 2015-07-21 10:39:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100040 | In the AO-8 cycle, we have proposed several X-ray and optical simultaneous observations of a type I Seyfert galaxy NGC 3516, and obtained a good correlation between those wavelengths in its faint phase. The result suggests that a hard primary X-ray continua found in NGC 3516 by Noda et al. (2013) is generated in a corona formed closely to an accretion disk, which is possibly a radiatively inefficient accretion flow. As a next step, we examine whether or not an X-ray variation is also correlated with that in optical, when NGC 3516 is in the bright phase, and the other primary X-ray continuum, also reported by Noda et al. (2013), is dominant. For it, we propose an X-ray and optical simultaneous observation of NGC 3516 with an exposure of 120 ksec, which is triggered by a Swift monitoring. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 10 | AO10-TOO | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF NGC 3516 IN ITS BRIGHT PHASE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/710009010/ | Quick Look | ![]() |
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1110 | RX J1347.5-1145 | 206.856 | -11.8093 | 206.189594 | -11.560184 | 209.147124 | -0.679556 | 323.97916756 | 48.76108187 | 292.056 | 53916.7756597222 | 2006-06-30 18:36:57 | 53918.7600115741 | 2006-07-02 18:14:25 | 801013010 | 69.6611 | 75 | 69.6611 | 69.6611 | 69.6611 | 69.6611 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.982 | 60.982 | 171.3759 | 0 | PROCESSED | 57534.8555671296 | 2016-05-26 20:32:01 | 54394 | 2007-10-21 00:00:00 | 53926.4810300926 | 2006-07-10 11:32:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NAOMI OTA | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013010/ | Quick Look | ![]() |
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1111 | OPHIUCHUS CLUSTER 5 | 258.0184 | -23.1077 | 257.261763 | -23.048099 | 258.982957 | -0.123527 | 0.73892155 | 9.49336651 | 88.7652 | 54181.8276736111 | 2007-03-22 19:51:51 | 54182.4890277778 | 2007-03-23 11:44:12 | 801026010 | 24.2557 | 15 | 24.2557 | 24.2557 | 0 | 24.2557 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2271 | 19.2271 | 57.1359 | 0 | PROCESSED | 57537.9767013889 | 2016-05-29 23:26:27 | 54736 | 2008-09-27 00:00:00 | 54186.2070949074 | 2007-03-27 04:58:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801026010/ | Quick Look | ![]() |
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1112 | M87 CENTER | 187.7366 | 12.4456 | 187.103964 | 12.721646 | 182.061198 | 14.477269 | 283.82387862 | 74.55209055 | 120.529 | 54068.9187037037 | 2006-11-29 22:02:56 | 54071.1266666667 | 2006-12-02 03:02:24 | 801038010 | 98.1831 | 100 | 98.1831 | 98.1831 | 0 | 98.1831 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 88.2503 | 88.2503 | 190.7308 | 2 | PROCESSED | 57536.2829050926 | 2016-05-28 06:47:23 | 54735 | 2008-09-26 00:00:00 | 54090.4156134259 | 2006-12-21 09:58:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801038010/ | Quick Look | ![]() |
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1113 | PERSEUS CL OFFSET | 49.6445 | 42.068 | 48.814215 | 41.886236 | 58.537476 | 22.936041 | 150.06631202 | -12.92163855 | 65.996 | 53980.0800925926 | 2006-09-02 01:55:20 | 53980.7668287037 | 2006-09-02 18:24:14 | 801049010 | 29.2438 | 30 | 29.2559 | 29.2479 | 29.2518 | 29.2438 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.6729 | 25.6729 | 59.3299 | 1 | PROCESSED | 57535.4121296296 | 2016-05-27 09:53:28 | 54526 | 2008-03-01 00:00:00 | 54021.3135416667 | 2006-10-13 07:31:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049010/ | Quick Look | ![]() |
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1114 | MARS-P18 | 103.5869 | 25.0943 | 102.819218 | 25.15788 | 102.294706 | 2.231395 | 190.58743765 | 11.74868918 | 298.2592 | 54560.7434837963 | 2008-04-04 17:50:37 | 54560.8264351852 | 2008-04-04 19:50:04 | 403006180 | 1.8618 | 100 | 1.8618 | 1.8618 | 0 | 1.8618 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.9396 | 1.9396 | 7.1539 | 0 | PROCESSED | 57542.0705555556 | 2016-06-03 01:41:36 | 54953 | 2009-05-02 00:00:00 | 54578.0530555556 | 2008-04-22 01:16:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006180/ | Quick Look | ![]() |
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1115 | PERSEUS CL OFFSET | 50.2242 | 41.1004 | 49.398659 | 40.920786 | 58.698225 | 21.886134 | 150.98569591 | -13.49005998 | 65.9967 | 53981.4552662037 | 2006-09-03 10:55:35 | 53982.1418287037 | 2006-09-04 03:24:14 | 801049030 | 32.8396 | 30 | 32.8556 | 32.8476 | 32.8396 | 32.8636 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 31.0313 | 31.0313 | 59.288 | 0 | PROCESSED | 57535.4291087963 | 2016-05-27 10:17:55 | 54526 | 2008-03-01 00:00:00 | 54020.8372106482 | 2006-10-12 20:05:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049030/ | Quick Look | ![]() |
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1116 | IGR J00234+6141 | 5.7092 | 61.7549 | 5.020335 | 61.477793 | 39.893501 | 52.142885 | 119.55446517 | -0.92914674 | 80.286 | 55372.004375 | 2010-06-25 00:06:18 | 55373.2397569445 | 2010-06-26 05:45:15 | 405022010 | 81.88 | 80 | 81.88 | 81.88 | 0 | 81.88 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.0364 | 70.0364 | 106.6979 | 1 | PROCESSED | 57552.4371759259 | 2016-06-13 10:29:32 | 55780 | 2011-08-07 00:00:00 | 55414.1791666667 | 2010-08-06 04:18:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUKIKATSU TERADA | JAP | 5 | AO5 | SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405022010/ | Quick Look | ![]() |
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1117 | ABELL 2199 OFFSET 2 | 247.3619 | 39.6495 | 246.934152 | 39.757579 | 233.32636 | 60.237575 | 63.07626508 | 43.54039287 | 251.2564 | 54011.5284722222 | 2006-10-03 12:41:00 | 54012.1578587963 | 2006-10-04 03:47:19 | 801058010 | 22.7072 | 25 | 22.7232 | 22.7072 | 22.7232 | 22.7232 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.704 | 20.704 | 54.36 | 0 | PROCESSED | 57535.7442476852 | 2016-05-27 17:51:43 | 54735 | 2008-09-26 00:00:00 | 54024.6719907407 | 2006-10-16 16:07:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801058010/ | Quick Look | ![]() |
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1118 | XSS J12270-4859 | 187.002 | -48.8936 | 186.3245 | -48.617009 | 209.763835 | -41.252243 | 298.97017898 | 13.79783482 | 315.9792 | 54686.9674421296 | 2008-08-08 23:13:07 | 54687.6480787037 | 2008-08-09 15:33:14 | 403029010 | 29.6232 | 30 | 29.6232 | 29.6232 | 0 | 29.6232 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.58 | 34.58 | 58.7919 | 0 | PROCESSED | 57543.2069907407 | 2016-06-04 04:58:04 | 55073 | 2009-08-30 00:00:00 | 54707.1730208333 | 2008-08-29 04:09:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403029010/ | Quick Look | ![]() |
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1119 | L106_B3 | 337.3111 | 61.2453 | 336.866796 | 60.988922 | 21.907924 | 61.425064 | 106.66847152 | 2.94694679 | 86.3781 | 55332.0617013889 | 2010-05-16 01:28:51 | 55333.5078587963 | 2010-05-17 12:11:19 | 505054010 | 59.3804 | 60 | 59.3804 | 59.3804 | 0 | 59.3804 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 54.0551 | 54.0551 | 124.908 | 3 | PROCESSED | 57551.5609259259 | 2016-06-12 13:27:44 | 55765 | 2011-07-23 00:00:00 | 55393.2646759259 | 2010-07-16 06:21:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 5 | AO5 | ORIGIN OF SOFT X-RAY EMISSION IN THE MILKY-WAY DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505054010/ | Quick Look | ![]() |
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1120 | EMS01095 | 252.3381 | -45.0256 | 251.43287 | -44.939011 | 256.578669 | -22.402784 | 340.43907916 | -0.17827348 | 87.5534 | 55603.1544328704 | 2011-02-11 03:42:23 | 55603.7613310185 | 2011-02-11 18:16:19 | 405027010 | 20.9332 | 20 | 20.9344 | 20.9344 | 0 | 20.9332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.9762 | 16.9762 | 52.4319 | 0 | PROCESSED | 57600.9093055556 | 2016-07-31 21:49:24 | 55983 | 2012-02-26 00:00:00 | 55617.4127430556 | 2011-02-25 09:54:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405027010/ | Quick Look | ![]() |
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1121 | HD125599 | 215.4515 | -48.0762 | 214.633471 | -47.848202 | 230.117069 | -31.899698 | 318.15137849 | 12.10713587 | 289.1653 | 55414.6760069444 | 2010-08-06 16:13:27 | 55415.1571990741 | 2010-08-07 03:46:22 | 405030010 | 31.048 | 30 | 31.056 | 31.056 | 0 | 31.048 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.8599 | 24.8599 | 41.5679 | 0 | PROCESSED | 57552.8615277778 | 2016-06-13 20:40:36 | 55793 | 2011-08-20 00:00:00 | 55427.1753819444 | 2010-08-19 04:12:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405030010/ | Quick Look | ![]() |
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1122 | A2142 OFFSET3 | 239.0356 | 27.7434 | 238.520462 | 27.887676 | 228.29172 | 46.798568 | 44.85726257 | 49.26078026 | 283.7312 | 54341.8454166667 | 2007-08-29 20:17:24 | 54342.3960532407 | 2007-08-30 09:30:19 | 802032010 | 23.7899 | 20 | 23.7899 | 23.7899 | 0 | 23.7899 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.2425 | 14.2425 | 47.5699 | 0 | PROCESSED | 57539.8930671296 | 2016-05-31 21:26:01 | 54724 | 2008-09-15 00:00:00 | 54356.294849537 | 2007-09-13 07:04:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYA OHASHI | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802032010/ | Quick Look | ![]() |
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1123 | VICINITY_4U1957+11 | 300.5977 | 12.1307 | 300.008296 | 11.990222 | 305.849194 | 31.842544 | 52.0534723 | -9.74567764 | 252.1551 | 55499.6275578704 | 2010-10-30 15:03:41 | 55501.8265625 | 2010-11-01 19:50:15 | 505057010 | 80.5839 | 80 | 80.5839 | 80.5839 | 0 | 80.5839 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.2042 | 59.2042 | 189.9759 | 2 | PROCESSED | 57553.9949305556 | 2016-06-14 23:52:42 | 55882 | 2011-11-17 00:00:00 | 55515.3752083333 | 2010-11-15 09:00:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOH TAKEI | JAP | 5 | AO5 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC LOW-LATITUDE HOT GAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505057010/ | Quick Look | ![]() |
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1124 | 1RXSJ171405.2-202747 | 258.5195 | -20.4586 | 257.777244 | -20.401416 | 259.232449 | 2.554431 | 3.21945841 | 10.61986264 | 93.18 | 57079.8384027778 | 2015-02-26 20:07:18 | 57080.0974652778 | 2015-02-27 02:20:21 | 409012010 | 10.9777 | 10 | 10.9777 | 11.0017 | 0 | 10.9937 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6641319444 | 2016-08-17 15:56:21 | 57458 | 2016-03-11 00:00:00 | 57091.4587847222 | 2015-03-10 11:00:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 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 | B | HIDEYUKI MORI | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409012010/ | Quick Look | ![]() |
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1125 | 1RXSJ165739.1-294946 | 254.4116 | -29.828 | 253.617619 | -29.751315 | 256.402928 | -7.119224 | 353.32761408 | 8.10480043 | 98.1097 | 57103.7733333333 | 2015-03-22 18:33:36 | 57104.2294328704 | 2015-03-23 05:30:23 | 409014010 | 17.2255 | 12 | 17.2255 | 17.2575 | 0 | 17.2335 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8394212963 | 2016-08-17 20:08:46 | 57486 | 2016-04-08 00:00:00 | 57119.4211458333 | 2015-04-07 10:06:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 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 | B | HIDEYUKI MORI | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409014010/ | Quick Look | ![]() |
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1126 | NGC3556 | 167.883 | 55.6841 | 167.153795 | 55.95585 | 141.585681 | 45.289435 | 148.29932367 | 56.24590288 | 111.9355 | 54795.9750694444 | 2008-11-25 23:24:06 | 54797.8890162037 | 2008-11-27 21:20:11 | 803013010 | 84.1642 | 100 | 84.1702 | 84.1659 | 0 | 84.1642 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.3537 | 60.3537 | 165.2879 | 2 | PROCESSED | 57544.6094212963 | 2016-06-05 14:37:34 | 55175 | 2009-12-10 00:00:00 | 54811.7645717593 | 2008-12-11 18:20:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030058 | We propose to observe NGC 3556, a nearby edge-on spiral galaxy, with 100 ks exposure. Galactic coronal X-ray emission in and around several spiral galaxies have been spatially resolved using Chandra and XMM instruments. The target is one of these galaxies showing relatively luminous X-ray emission. Due to limited spectral capability of these instruments, X-ray spectral properties of these diffuse emission have not yet been investigated. We use good spectral capability of the SUZAKU/XIS to investigate the temperature structure and constrain the metal abundance pattern for the first time in galactic corona. We study origin, heating mechanism, and chemical properties of these galactic corona. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 3 | AO3 | GALACTIC CORONA IN AND AROUND THE EDGE-ON GALAXY NGC 3556 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803013010/ | Quick Look | ![]() |
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1127 | JUPITER | 29.0829 | 10.6504 | 28.417372 | 10.406323 | 30.788902 | -1.172897 | 147.71201597 | -49.07381266 | 249.1851 | 55939.2483912037 | 2012-01-13 05:57:41 | 55939.8634722222 | 2012-01-13 20:43:24 | 506006050 | 23.2827 | 160 | 23.2907 | 23.2827 | 0 | 23.2954 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2679 | 19.2679 | 53.136 | 0 | PROCESSED | 57604.3330902778 | 2016-08-04 07:59:39 | 56331 | 2013-02-08 00:00:00 | 55960.1390740741 | 2012-02-03 03:20:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006050/ | Quick Look | ![]() |
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1128 | A2163_NE | 244.026 | -6.0591 | 243.359036 | -5.935716 | 243.191505 | 14.996833 | 6.90407558 | 30.45267126 | 113.8304 | 54870.8869560185 | 2009-02-08 21:17:13 | 54872.1724421296 | 2009-02-10 04:08:19 | 803022010 | 51.7974 | 40 | 51.8054 | 51.8134 | 0 | 51.7974 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.861 | 43.861 | 111.0518 | 1 | PROCESSED | 57545.4990162037 | 2016-06-06 11:58:35 | 55330 | 2010-05-14 00:00:00 | 54895.5963888889 | 2009-03-05 14:18:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030094 | We propose 2 pointing observations of a hot cluster A2163 (z=0.2). A2163 is an X-ray brightest object among the violent merger candidates, which possess a huge radio halo and a complex temperature structure. Thus it is a unique target to discover extremely hot (>20keV) gas produced via merger shock. Thanks to the unprecedent high-quality broad-band spectra of Suzaku we can accurately determine the temperature of the hot gas. Which, at the same time, leads to the detection of the buried non-thermal hard X-ray emission. Combining this observation with the high-resolution images of our thermal SZ effect and the XMM observation, we can obtain a spatial distribution of the extremely hot thermal gas in the merging cluster for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 3 | AO3 | BROAD-BAND SPECTROSCOPY OF THE HOTTEST ABELL GALAXY CLUSTER A2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803022010/ | Quick Look | ![]() |
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1129 | WESTERLUND1_2 | 252.808 | -46.1402 | 251.891543 | -46.055758 | 257.089266 | -23.465452 | 339.79276992 | -1.14410237 | 285.6981 | 55451.2033912037 | 2010-09-12 04:52:53 | 55452.6077777778 | 2010-09-13 14:35:12 | 505050010 | 52.6541 | 50 | 52.6541 | 52.6541 | 0 | 52.6541 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7536 | 42.7536 | 121.3099 | 0 | PROCESSED | 57553.3934375 | 2016-06-14 09:26:33 | 55829 | 2011-09-25 00:00:00 | 55463.2091435185 | 2010-09-24 05:01:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505050010/ | Quick Look | ![]() |
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1130 | CYGNUS LOOP BLOWOUT5 | 312.5999 | 28.7931 | 312.071808 | 28.605616 | 325.981178 | 44.311018 | 72.41540255 | -9.63024021 | 60.972 | 55708.6627546296 | 2011-05-27 15:54:22 | 55709.5335185185 | 2011-05-28 12:48:16 | 506015010 | 36.7552 | 35 | 36.7632 | 36.7552 | 0 | 36.7695 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 31.6317 | 31.6317 | 75.216 | 1 | PROCESSED | 57602.1728935185 | 2016-08-02 04:08:58 | 56093 | 2012-06-15 00:00:00 | 55725.2447569444 | 2011-06-13 05:52:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506015010/ | Quick Look | ![]() |
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1131 | VELA JR SE2 | 133.8563 | -47.0644 | 133.431556 | -46.872219 | 161.338969 | -60.118086 | 267.19687484 | -1.23927515 | 109.9991 | 56620.734375 | 2013-11-24 17:37:30 | 56621.062650463 | 2013-11-25 01:30:13 | 508061010 | 14.4492 | 15 | 14.4492 | 14.4711 | 0 | 14.4572 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.7997 | 18.7997 | 28.3599 | 0 | PROCESSED | 57613.398912037 | 2016-08-13 09:34:26 | 56998 | 2014-12-07 00:00:00 | 56632.5722685185 | 2013-12-06 13:44:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 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) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | TARO FUKUYAMA | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508061010/ | Quick Look | ![]() |
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1132 | FERMI_0265 | 187.7993 | -14.1672 | 187.149588 | -13.891145 | 192.78645 | -9.915447 | 295.5292019 | 48.41340382 | 292.6305 | 55040.2233449074 | 2009-07-28 05:21:37 | 55041.5002777778 | 2009-07-29 12:00:24 | 804017020 | 52.6378 | 54 | 52.6378 | 52.9098 | 0 | 52.9018 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 48.06 | 48.06 | 110.3041 | 0 | PROCESSED | 57547.9908333333 | 2016-06-08 23:46:48 | 55422 | 2010-08-14 00:00:00 | 55050.4462384259 | 2009-08-07 10:42:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804017020/ | Quick Look | ![]() |
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1133 | FERMI_0291 | 203.2955 | 51.017 | 202.790071 | 51.273115 | 172.022229 | 54.301955 | 107.38909593 | 64.83295576 | 302.8355 | 54983.4258680556 | 2009-06-01 10:13:15 | 54984.4725 | 2009-06-02 11:20:24 | 804019010 | 46.3536 | 40 | 46.3616 | 46.3536 | 0 | 46.3696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7073 | 42.7073 | 90.3858 | 1 | PROCESSED | 57547.4428703704 | 2016-06-08 10:37:44 | 55363 | 2010-06-16 00:00:00 | 54994.2756018518 | 2009-06-12 06:36:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804019010/ | Quick Look | ![]() |
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1134 | CAS A | 350.8704 | 58.8069 | 350.304462 | 58.532314 | 27.384002 | 54.841803 | 111.74200441 | -2.14072863 | 228.5251 | 56672.9492708333 | 2014-01-15 22:46:57 | 56673.8064699074 | 2014-01-16 19:21:19 | 508011010 | 0 | 120 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.771412037 | 2016-08-13 18:30:50 | 56717 | 2014-03-01 00:00:00 | 56712.601400463 | 2014-02-24 14:26:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080021 | 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 | B | YOSHITOMO MAEDA | JAP | 8 | AO8 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508011010/ | Quick Look | ![]() |
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1135 | N132D | 81.1356 | -69.5861 | 81.235257 | -69.628797 | 313.439432 | -85.525223 | 280.24807804 | -32.83670135 | 53.4639 | 53597.5317361111 | 2005-08-15 12:45:42 | 53597.6932291667 | 2005-08-15 16:38:15 | 100002020 | 0 | 7 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6768865741 | 2016-05-12 16:14:43 | 54247 | 2007-05-27 00:00:00 | 54230.4131828704 | 2007-05-10 09:54:59 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD HV ON WITH N132D | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002020/ | Quick Look | ![]() |
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1136 | N132D | 81.0865 | -69.7023 | 81.190689 | -69.745221 | 312.425808 | -85.439083 | 280.38777612 | -32.83268249 | 53.5118 | 53597.8375 | 2005-08-15 20:06:00 | 53597.9865625 | 2005-08-15 23:40:39 | 100002040 | 0 | 7 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6840277778 | 2016-05-12 16:25:00 | 54247 | 2007-05-27 00:00:00 | 54230.4148726852 | 2007-05-10 09:57:25 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | JAP | 0 | SWG | HXD HV ON WITH N132D | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002040/ | Quick Look | ![]() |
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1137 | W44_SOUTH | 284.0546 | 1.2208 | 283.419443 | 1.15468 | 285.391807 | 23.913502 | 34.56340933 | -0.50670684 | 73.0006 | 56756.507025463 | 2014-04-09 12:10:07 | 56757.3474074074 | 2014-04-10 08:20:16 | 508003020 | 32.3696 | 33 | 32.3776 | 32.3776 | 0 | 32.3696 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5034 | 29.5034 | 72.5959 | 1 | PROCESSED | 57614.2259837963 | 2016-08-14 05:25:25 | 57193 | 2015-06-20 00:00:00 | 56825.6834027778 | 2014-06-17 16:24:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508003020/ | Quick Look | ![]() |
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1138 | ABELL 2199 OFFSET 1 | 247.0269 | 39.6504 | 246.598636 | 39.759978 | 232.832467 | 60.158374 | 63.06766091 | 43.79825488 | 251.7923 | 54009.8973958333 | 2006-10-01 21:32:15 | 54010.4467476852 | 2006-10-02 10:43:19 | 801057010 | 24.6315 | 25 | 24.6315 | 24.6315 | 24.6315 | 24.6315 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.5343 | 25.5343 | 47.454 | 0 | PROCESSED | 57535.7339814815 | 2016-05-27 17:36:56 | 54735 | 2008-09-26 00:00:00 | 54021.2449189815 | 2006-10-13 05:52:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801057010/ | Quick Look | ![]() |
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1139 | ABELL 2199 OFFSET 3 | 247.3596 | 39.3165 | 246.92934 | 39.424595 | 233.528009 | 59.920137 | 62.61707687 | 43.53145251 | 252.4737 | 54012.1589351852 | 2006-10-04 03:48:52 | 54012.6786921296 | 2006-10-04 16:17:19 | 801059010 | 25.2467 | 25 | 25.2467 | 25.2467 | 25.2467 | 25.2467 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.505 | 20.505 | 44.8879 | 1 | PROCESSED | 57535.7507291667 | 2016-05-27 18:01:03 | 54735 | 2008-09-26 00:00:00 | 54025.4730092593 | 2006-10-17 11:21:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801059010/ | Quick Look | ![]() |
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1140 | COMA OUTSKIRTS3 | 196.1692 | 28.7094 | 195.570451 | 28.977142 | 182.240031 | 32.536562 | 62.09765822 | 86.67565791 | 116.0002 | 55901.9229513889 | 2011-12-06 22:09:03 | 55902.7161342593 | 2011-12-07 17:11:14 | 806022010 | 31.22 | 30 | 31.244 | 31.22 | 0 | 31.22 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.7241 | 28.7241 | 68.5199 | 0 | PROCESSED | 57604.0669212963 | 2016-08-04 01:36:22 | 56284 | 2012-12-23 00:00:00 | 55915.1959837963 | 2011-12-20 04:42:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806022010/ | Quick Look | ![]() |
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1141 | A2744_SW | 3.5132 | -30.5508 | 2.881732 | -30.828827 | 349.850108 | -29.168885 | 8.03425743 | -81.13040471 | 233.4967 | 55540.2569791667 | 2010-12-10 06:10:03 | 55542.2883217593 | 2010-12-12 06:55:11 | 805015010 | 69.7763 | 65 | 69.7763 | 69.7763 | 0 | 69.7763 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.2396 | 59.2396 | 175.4817 | 0 | PROCESSED | 57554.4226851852 | 2016-06-15 10:08:40 | 55917 | 2011-12-22 00:00:00 | 55551.0433101852 | 2010-12-21 01:02:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050013 | We propose Suzaku observations of two merging clusters of galaxies, A2744 and the Bullet Cluster, to map the entropy variation out to the virial radius. Recent numerical simulations indicate that the entropy generation occurs through two-shock propagations, which is to be markedly seen in the cluster outskirts. On the other hand, little observational testing has been done for this regime of merging systems. We thus request three additional pointings to cover regions of large-scale filaments discovered in the optical. This study can only be achieved by Suzaku because of the lowest background level and excellent sensitivity, and will bring us new constraints on the thermodynamical history of the clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 5 | AO5 | MAPPING THE GAS ENTROPY GENERATION IN A SEQUENCE OF MERGING CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805015010/ | Quick Look | ![]() |
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1142 | RXCJ0411.2-4819 | 62.816 | -48.3247 | 62.453818 | -48.452722 | 38.950898 | -67.014001 | 255.63059498 | -46.16240445 | 110.1457 | 55461.4637384259 | 2010-09-22 11:07:47 | 55461.7793865741 | 2010-09-22 18:42:19 | 805024010 | 11.3649 | 10 | 11.3649 | 11.3649 | 0 | 11.3649 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10.396 | 10.396 | 27.264 | 0 | PROCESSED | 57553.4942361111 | 2016-06-14 11:51:42 | 55836 | 2011-10-02 00:00:00 | 55470.1084606482 | 2010-10-01 02:36:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050021 | We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 5 | AO5 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805024010/ | Quick Look | ![]() |
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1143 | NGC 4697 | 192.1513 | -5.7906 | 191.50498 | -5.518104 | 193.427288 | -0.530434 | 301.63561999 | 57.07401872 | 112.9816 | 55575.4840277778 | 2011-01-14 11:37:00 | 55578.1905324074 | 2011-01-17 04:34:22 | 805041010 | 102.3091 | 100 | 102.3091 | 102.3091 | 0 | 102.3091 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.0471 | 76.0471 | 233.8161 | 1 | PROCESSED | 57600.7175462963 | 2016-07-31 17:13:16 | 55962 | 2012-02-05 00:00:00 | 55595.5109027778 | 2011-02-03 12:15:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050080 | We propose the observation of the elliptical galaxy NGC 4697, whose temperature of interstellar medium is low, 0.3 keV. Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. The different abundance pattern between S0 and elliptical galaxies was reported in recent study. To understand the formation process of early-type galaxies in more detail, it is very important to appreciate whether the different abundance pattern is due to morphology or temperature of system. The purpose of this proposal is to reveal the relation between abundance pattern, morphology, and temperature of system by investigating the abundance pattern of the elliptical galaxy, which has lower temperature. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SAORI KONAMI | JAP | 5 | AO5 | MEASUREMENT OF ABUNDANCE PATTERN IN LOW TEMPARTURE ISM OF ELLIPTICAL GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805041010/ | Quick Look | ![]() |
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1144 | CENTAURUS B | 206.7067 | -60.4086 | 205.850027 | -60.15889 | 231.235341 | -45.192759 | 309.7224369 | 1.73083578 | 275.5009 | 55758.843912037 | 2011-07-16 20:15:14 | 55760.4932060185 | 2011-07-18 11:50:13 | 806017010 | 93.6172 | 120 | 93.645 | 93.6172 | 0 | 93.637 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 27.6959 | 0 | PROCESSED | 57602.5915625 | 2016-08-02 14:11:51 | 56152 | 2012-08-13 00:00:00 | 55830.7256134259 | 2011-09-26 17:24:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060070 | X-ray observation of radio lobe is essential to reveal the particle acceleration mechanism in the lobe, because we can obtain magnetic field and electron energy density without assumption of equipartition. The radio lobe of FR I radio galaxy Centaurus B was previously detected by ASCA. For revealing the mechanism of particle acceleration in radio lobes, detailed multi-wavelength observations are very important. We propose a deep observation of the radio lobe by Suzaku, which has the advantage of low background and high sensitivity for diffuse X-ray. Good quality Suzaku data combined with a detailed modeling reveals particle acceleration mechanism working in the radio lobe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YASUYUKI TANAKA | JAP | 6 | AO6 | X-RAY OBSERVATION OF RADIO LOBE OF FR I RADIO GALAXY CENTAURUS B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806017010/ | Quick Look | ![]() |
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1145 | 1RXSJ174459.5-172640 | 266.2467 | -17.4406 | 265.51875 | -17.420611 | 266.390507 | 5.953243 | 9.76958181 | 6.08973572 | 101.0461 | 54555.6304050926 | 2008-03-30 15:07:47 | 54556.5834953704 | 2008-03-31 14:00:14 | 402003010 | 43.5793 | 40 | 43.5953 | 43.5793 | 0 | 43.6033 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.5916 | 29.5916 | 82.3439 | 1 | PROCESSED | 57541.9975462963 | 2016-06-02 23:56:28 | 54937 | 2009-04-16 00:00:00 | 54570.1529282407 | 2008-04-14 03:40:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIDEYUKI MORI | JAP | 2 | AO2 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402003010/ | Quick Look | ![]() |
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1146 | U SCO | 245.629 | -17.8143 | 244.907277 | -17.697813 | 246.808051 | 3.686286 | 357.72199881 | 21.90970563 | 93.274 | 55236.514375 | 2010-02-09 12:20:42 | 55237.1668865741 | 2010-02-10 04:00:19 | 404018020 | 28.9369 | 20 | 28.9369 | 28.9369 | 0 | 28.9369 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.3288 | 18.3288 | 56.3699 | 0 | PROCESSED | 57550.5565393518 | 2016-06-11 13:21:25 | 55619 | 2011-02-27 00:00:00 | 55251.1498611111 | 2010-02-24 03:35:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | DAI TAKEI | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404018020/ | Quick Look | ![]() |
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1147 | PSR B1259-63 | 195.6821 | -63.8856 | 194.892558 | -63.616964 | 227.728655 | -50.936167 | 304.1741357 | -1.04108664 | 280.935 | 54288.622025463 | 2007-07-07 14:55:43 | 54289.062662037 | 2007-07-08 01:30:14 | 402014010 | 21.8634 | 20 | 21.8714 | 21.8634 | 0 | 21.8714 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.86 | 26.86 | 38.0639 | 1 | PROCESSED | 57539.1256481482 | 2016-05-31 03:00:56 | 54696 | 2008-08-18 00:00:00 | 54328.4884722222 | 2007-08-16 11:43:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014010/ | Quick Look | ![]() |
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1148 | MARS-P6 | 103.0844 | 25.143 | 102.316186 | 25.2042 | 101.836831 | 2.238113 | 190.34808199 | 11.3557719 | 298.0743 | 54559.7434375 | 2008-04-03 17:50:33 | 54559.8265972222 | 2008-04-03 19:50:18 | 403006060 | 1.939 | 100 | 1.939 | 1.939 | 0 | 1.939 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.8046 | 1.8046 | 7.1819 | 0 | PROCESSED | 57542.0435416667 | 2016-06-03 01:02:42 | 54953 | 2009-05-02 00:00:00 | 54577.1376388889 | 2008-04-21 03:18:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006060/ | Quick Look | ![]() |
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1149 | MARS-P7 | 103.127 | 25.1401 | 102.358824 | 25.201502 | 101.875529 | 2.238706 | 190.36726484 | 11.38956433 | 298.0907 | 54559.8267476852 | 2008-04-03 19:50:31 | 54559.9029861111 | 2008-04-03 21:40:18 | 403006070 | 2.5028 | 100 | 2.5139 | 2.5108 | 0 | 2.5028 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.6506 | 1.6506 | 6.584 | 0 | PROCESSED | 57542.0488310185 | 2016-06-03 01:10:19 | 54953 | 2009-05-02 00:00:00 | 54577.1486342593 | 2008-04-21 03:34:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006070/ | Quick Look | ![]() |
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1150 | MARS-P12 | 103.3358 | 25.1148 | 102.567873 | 25.177192 | 102.066233 | 2.230736 | 190.47148034 | 11.55063865 | 298.1645 | 54560.2434837963 | 2008-04-04 05:50:37 | 54560.3266666667 | 2008-04-04 07:50:24 | 403006120 | 3.455 | 100 | 3.455 | 3.455 | 0 | 3.455 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.678 | 2.678 | 7.1759 | 0 | PROCESSED | 57542.0566782407 | 2016-06-03 01:21:37 | 54953 | 2009-05-02 00:00:00 | 54577.1789467593 | 2008-04-21 04:17:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006120/ | Quick Look | ![]() |
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1151 | YY DRA | 175.8686 | 71.6187 | 175.161968 | 71.896164 | 128.299312 | 59.497013 | 130.35712902 | 44.51671754 | 282.0676 | 54632.7758217593 | 2008-06-15 18:37:11 | 54633.4098842593 | 2008-06-16 09:50:14 | 403022010 | 29.1851 | 30 | 29.1851 | 29.1851 | 0 | 29.1851 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.4743 | 27.4743 | 54.7779 | 1 | PROCESSED | 57542.8240509259 | 2016-06-03 19:46:38 | 55013 | 2009-07-01 00:00:00 | 54644.1517592593 | 2008-06-27 03:38:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403022010/ | Quick Look | ![]() |
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1152 | TV COL | 82.3326 | -32.8641 | 81.870324 | -32.902382 | 78.445337 | -55.999473 | 236.83580562 | -30.63495041 | 295.9146 | 54573.7555555556 | 2008-04-17 18:08:00 | 54574.6668634259 | 2008-04-18 16:00:17 | 403023010 | 35.8367 | 40 | 35.8367 | 35.8367 | 0 | 35.8367 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.1023 | 30.1023 | 78.7299 | 0 | PROCESSED | 57542.3393055556 | 2016-06-03 08:08:36 | 54953 | 2009-05-02 00:00:00 | 54587.0666550926 | 2008-05-01 01:35:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403023010/ | Quick Look | ![]() |
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1153 | WR140 | 305.2159 | 43.8446 | 304.793528 | 43.684914 | 327.480092 | 60.454485 | 80.96257668 | 4.11237193 | 190.1825 | 54844.5415162037 | 2009-01-13 12:59:47 | 54846.500162037 | 2009-01-15 12:00:14 | 403030010 | 89.4068 | 80 | 89.4068 | 89.4068 | 0 | 89.4068 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.0557 | 78.0557 | 169.1969 | 1 | PROCESSED | 57545.2609606482 | 2016-06-06 06:15:47 | 55328 | 2010-05-12 00:00:00 | 54861.8550115741 | 2009-01-30 20:31:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITOMO MAEDA | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403030010/ | Quick Look | ![]() |
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1154 | WR140 | 305.211 | 43.8318 | 304.788544 | 43.672134 | 327.46168 | 60.444795 | 80.94998516 | 4.10805919 | 199.7371 | 54835.3583449074 | 2009-01-04 08:36:01 | 54836.4252199074 | 2009-01-05 10:12:19 | 403031010 | 47.2664 | 40 | 47.2664 | 47.2664 | 0 | 47.2824 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.303 | 45.303 | 92.1618 | 0 | PROCESSED | 57545.1036921296 | 2016-06-06 02:29:19 | 55328 | 2010-05-12 00:00:00 | 54850.2164583333 | 2009-01-19 05:11:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITOMO MAEDA | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403031010/ | Quick Look | ![]() |
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1155 | V603 AQL | 282.2246 | 0.5976 | 281.586541 | 0.540157 | 283.33615 | 23.473967 | 33.17431822 | 0.83751501 | 93.9529 | 55267.0156597222 | 2010-03-12 00:22:33 | 55267.9773032407 | 2010-03-12 23:27:19 | 404020010 | 34.9173 | 30 | 34.9309 | 34.9173 | 0 | 34.9309 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.2045 | 30.2045 | 83.0778 | 1 | PROCESSED | 57550.8656018518 | 2016-06-11 20:46:28 | 55645 | 2011-03-25 00:00:00 | 55279.4471296296 | 2010-03-24 10:43:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEI SAITOU | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404020010/ | Quick Look | ![]() |
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1156 | PQ GEM | 117.7967 | 14.685 | 117.09108 | 14.813297 | 116.98609 | -6.189538 | 206.10344887 | 19.72488518 | 295.2889 | 54933.5737037037 | 2009-04-12 13:46:08 | 54934.6329166667 | 2009-04-13 15:11:24 | 404030010 | 46.7387 | 40 | 46.7387 | 46.7387 | 0 | 46.7387 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.2479 | 43.2479 | 91.5079 | 0 | PROCESSED | 57546.1405787037 | 2016-06-07 03:22:26 | 55324 | 2010-05-08 00:00:00 | 54949.5317939815 | 2009-04-28 12:45:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI YUASA | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404030010/ | Quick Look | ![]() |
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1157 | U GEM IN OUTBURST | 118.7732 | 21.9928 | 118.033393 | 22.125213 | 116.515178 | 1.161478 | 199.23241259 | 23.39259554 | 281.117 | 56029.4105324074 | 2012-04-12 09:51:10 | 56030.750162037 | 2012-04-13 18:00:14 | 407035010 | 50.2547 | 50 | 50.2547 | 50.2547 | 0 | 50.2547 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.2967 | 47.2967 | 115.7079 | 1 | PROCESSED | 57605.2002199074 | 2016-08-05 04:48:19 | 56415 | 2013-05-03 00:00:00 | 56044.3887731482 | 2012-04-27 09:19:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAYUKI HAYASHI | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407035010/ | Quick Look | ![]() |
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1158 | SAGITTARIUS A* | 266.4172 | -29.0091 | 265.622479 | -28.989771 | 266.842554 | -5.607236 | 359.94331347 | -0.04710749 | 285.0015 | 56554.8566087963 | 2013-09-19 20:33:31 | 56555.4439930556 | 2013-09-20 10:39:21 | 408017030 | 20.2613 | 20 | 20.268 | 20.2613 | 0 | 20.268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.549 | 20.549 | 50.7419 | 1 | PROCESSED | 57612.6558217593 | 2016-08-12 15:44:23 | 56956 | 2014-10-26 00:00:00 | 56588.6928935185 | 2013-10-23 16:37:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | YOSHITOMO MAEDA | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408017030/ | Quick Look | ![]() |
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1159 | CYGNUS_LOOP_P3 | 313.0409 | 31.565 | 312.525205 | 31.375918 | 328.010479 | 46.721185 | 74.84662265 | -8.19493741 | 240.0003 | 54418.4174074074 | 2007-11-14 10:01:04 | 54418.9377083333 | 2007-11-14 22:30:18 | 501014010 | 16.7648 | 12 | 16.7812 | 16.7808 | 0 | 16.7648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6962 | 14.6962 | 44.9439 | 0 | PROCESSED | 57540.5210069445 | 2016-06-01 12:30:15 | 54798 | 2008-11-28 00:00:00 | 54430.2624884259 | 2007-11-26 06:17:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501014010/ | Quick Look | ![]() |
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1160 | DRACO HVC REGION A | 243.9602 | 60.0594 | 243.754378 | 60.182015 | 196.928393 | 76.754112 | 91.20688798 | 42.38144862 | 79.8192 | 53814.6161111111 | 2006-03-20 14:47:12 | 53816.0050578704 | 2006-03-22 00:07:17 | 501004010 | 61.1798 | 60 | 61.1798 | 61.1798 | 61.1798 | 61.1798 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61.2301 | 61.2301 | 119.9879 | 2 | PROCESSED | 57533.2956481482 | 2016-05-25 07:05:44 | 54394 | 2007-10-21 00:00:00 | 53906.0459722222 | 2006-06-20 01:06:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKESHI TSURU | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501004010/ | Quick Look | ![]() |
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1161 | GC_LARGEPROJECT13 | 264.4001 | -31.8052 | 263.587715 | -31.776061 | 265.18111 | -8.457548 | 356.65040302 | -0.04773216 | 95.4712 | 54881.6929282407 | 2009-02-19 16:37:49 | 54883.0522453704 | 2009-02-21 01:15:14 | 503019010 | 52.7764 | 50 | 52.7764 | 52.7972 | 0 | 52.7844 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4395 | 42.4395 | 117.4338 | 0 | PROCESSED | 57545.6322106482 | 2016-06-06 15:10:23 | 54557 | 2008-04-01 00:00:00 | 54902.1118171296 | 2009-03-12 02:41:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503019010/ | Quick Look | ![]() |
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1162 | HESS J1800-240B | 270.1124 | -24.0578 | 269.347343 | -24.056487 | 270.09306 | -0.616951 | 5.8867537 | -0.376417 | 87.1402 | 54562.3157523148 | 2008-04-06 07:34:41 | 54563.0141666667 | 2008-04-07 00:20:24 | 503026010 | 31.6728 | 30 | 31.6728 | 31.6728 | 0 | 31.6728 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.7698 | 26.7698 | 60.32 | 1 | PROCESSED | 57542.2491319444 | 2016-06-03 05:58:45 | 54953 | 2009-05-02 00:00:00 | 54580.1793402778 | 2008-04-24 04:18:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKAAKI TANAKA | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503026010/ | Quick Look | ![]() |
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1163 | VELA JR P25 | 132.5224 | -46.8921 | 132.101077 | -46.704657 | 159.613489 | -60.474295 | 266.48184745 | -1.82836861 | 347.0024 | 54653.1675462963 | 2008-07-06 04:01:16 | 54653.4335532407 | 2008-07-06 10:24:19 | 503037010 | 13.16 | 10 | 13.16 | 13.16 | 0 | 13.16 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.4325 | 12.4325 | 22.9759 | 0 | PROCESSED | 57542.9817476852 | 2016-06-03 23:33:43 | 55048 | 2009-08-05 00:00:00 | 54679.3166203704 | 2008-08-01 07:35:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503037010/ | Quick Look | ![]() |
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1164 | CYGNUS LOOP (P27) | 313.8328 | 30.0104 | 313.308096 | 29.818528 | 328.031945 | 45.024246 | 74.06049539 | -9.7037521 | 49.6211 | 54599.5480092593 | 2008-05-13 13:09:08 | 54600.0494675926 | 2008-05-14 01:11:14 | 503063010 | 22.7843 | 20 | 22.7923 | 22.7843 | 0 | 22.8003 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.0688 | 20.0688 | 43.3239 | 0 | PROCESSED | 57542.5253587963 | 2016-06-03 12:36:31 | 54975 | 2009-05-24 00:00:00 | 54609.1396990741 | 2008-05-23 03:21:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503063010/ | Quick Look | ![]() |
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1165 | VICINITY_OF_PKS_2155-2 | 330.1861 | -29.9649 | 329.464287 | -30.205624 | 321.680429 | -16.673826 | 18.22929909 | -52.62033555 | 55.8323 | 54588.3553356482 | 2008-05-02 08:31:41 | 54590.7293865741 | 2008-05-04 17:30:19 | 503083010 | 87.3274 | 80 | 87.3274 | 87.3274 | 0 | 87.3274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.8451 | 75.8451 | 205.1059 | 3 | PROCESSED | 57542.4726736111 | 2016-06-03 11:20:39 | 54975 | 2009-05-24 00:00:00 | 54608.2608912037 | 2008-05-22 06:15:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TOSHISHIGE HAGIHARA | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503083010/ | Quick Look | ![]() |
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1166 | RIM2 | 311.426 | 31.5946 | 310.913676 | 31.411344 | 326.171395 | 47.287726 | 74.00572356 | -7.09996284 | 246.8661 | 55153.9497337963 | 2009-11-18 22:47:37 | 55154.4843055556 | 2009-11-19 11:37:24 | 504006010 | 26.3059 | 24 | 26.3059 | 26.3059 | 0 | 26.3059 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.237 | 22.237 | 46.1839 | 0 | PROCESSED | 57549.4609490741 | 2016-06-10 11:03:46 | 55534 | 2010-12-04 00:00:00 | 55166.4447916667 | 2009-12-01 10:40:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504006010/ | Quick Look | ![]() |
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1167 | HD161103 | 266.1888 | -27.2272 | 265.405227 | -27.206791 | 266.594492 | -3.831151 | 1.35850162 | 1.05434609 | 105.2351 | 54884.7946643518 | 2009-02-22 19:04:19 | 54886.7057175926 | 2009-02-24 16:56:14 | 403001010 | 71.5249 | 60 | 71.5329 | 71.5249 | 0 | 71.5409 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.6647 | 59.6647 | 165.0858 | 1 | PROCESSED | 57545.6533217593 | 2016-06-06 15:40:47 | 55330 | 2010-05-14 00:00:00 | 54903.6732523148 | 2009-03-13 16:09:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUNICHIRO MIURA | JAP | 3 | AO3 | SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403001010/ | Quick Look | ![]() |
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1168 | RIM3 | 311.3232 | 31.2993 | 310.809596 | 31.116423 | 325.884456 | 47.049295 | 73.71675058 | -7.21258663 | 246.4181 | 55154.4849189815 | 2009-11-19 11:38:17 | 55155.1204166667 | 2009-11-20 02:53:24 | 504007010 | 21.5566 | 19 | 21.5566 | 21.5566 | 0 | 21.5566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.481 | 17.481 | 54.9039 | 0 | PROCESSED | 57549.4865277778 | 2016-06-10 11:40:36 | 55534 | 2010-12-04 00:00:00 | 55166.4304166667 | 2009-12-01 10:19:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504007010/ | Quick Look | ![]() |
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1169 | RIM6 | 314.3771 | 31.4503 | 313.858117 | 31.256512 | 329.460239 | 46.161653 | 75.4881661 | -9.14820234 | 247.047 | 55155.7987615741 | 2009-11-20 19:10:13 | 55156.1745833333 | 2009-11-21 04:11:24 | 504010010 | 14.3275 | 11 | 14.3475 | 14.3435 | 0 | 14.3275 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7152 | 10.7152 | 32.468 | 0 | PROCESSED | 57549.4929513889 | 2016-06-10 11:49:51 | 55534 | 2010-12-04 00:00:00 | 55166.4272916667 | 2009-12-01 10:15:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504010010/ | Quick Look | ![]() |
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1170 | W28_EASTSHELL | 270.3727 | -23.2858 | 269.612111 | -23.285763 | 270.332756 | 0.154633 | 6.67541903 | -0.20080463 | 88.0003 | 55617.4542939815 | 2011-02-25 10:54:11 | 55620.1723032407 | 2011-02-28 04:08:07 | 505006010 | 99.9816 | 100 | 99.9816 | 99.9816 | 0 | 99.9816 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.6772 | 83.6772 | 234.8157 | 3 | PROCESSED | 57601.1152430556 | 2016-08-01 02:45:57 | 55287 | 2010-04-01 00:00:00 | 55642.1946643518 | 2011-03-22 04:40:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505006010/ | Quick Look | ![]() |
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1171 | CYGNUS LOOP 4 | 312.482 | 31.9468 | 311.969326 | 31.759715 | 327.592245 | 47.259949 | 74.84594636 | -7.58533627 | 81.0154 | 55301.6216087963 | 2010-04-15 14:55:07 | 55301.8912037037 | 2010-04-15 21:23:20 | 505012010 | 12.4535 | 12 | 12.4535 | 12.4535 | 0 | 12.4535 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.182 | 12.182 | 23.2801 | 1 | PROCESSED | 57551.2226736111 | 2016-06-12 05:20:39 | 55287 | 2010-04-01 00:00:00 | 55362.3160763889 | 2010-06-15 07:35:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505012010/ | Quick Look | ![]() |
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1172 | JUPITER | 104.585 | 23.053 | 103.829387 | 23.12132 | 103.399653 | 0.287954 | 192.87049462 | 11.72496816 | 267.157 | 56768.1148958333 | 2014-04-21 02:45:27 | 56768.2245138889 | 2014-04-21 05:23:18 | 508023140 | 5.2482 | 160 | 5.2642 | 5.2482 | 0 | 5.2708 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9659259259 | 2016-08-14 23:10:56 | 57212 | 2015-07-09 00:00:00 | 56846.5934143518 | 2014-07-08 14:14:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | 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 simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023140/ | Quick Look | ![]() |
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1173 | CYGNUS LOOP 13 | 313.3172 | 30.1574 | 312.794183 | 29.967347 | 327.529928 | 45.333203 | 73.89066537 | -9.26489611 | 82.0018 | 55329.8397337963 | 2010-05-13 20:09:13 | 55330.4925694444 | 2010-05-14 11:49:18 | 505021010 | 21.565 | 21 | 21.565 | 21.597 | 0 | 21.565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.12 | 18.12 | 56.3999 | 1 | PROCESSED | 57551.5081597222 | 2016-06-12 12:11:45 | 55287 | 2010-04-01 00:00:00 | 55393.3656712963 | 2010-07-16 08:46:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505021010/ | Quick Look | ![]() |
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1174 | CYGNUS LOOP 15 | 313.2124 | 29.6854 | 312.687356 | 29.495723 | 327.15263 | 44.932937 | 73.46064198 | -9.49078141 | 50.2914 | 55343.3019791667 | 2010-05-27 07:14:51 | 55343.6994675926 | 2010-05-27 16:47:14 | 505023010 | 19.2953 | 19 | 19.2953 | 19.2953 | 0 | 19.2953 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.514 | 16.514 | 34.32 | 1 | PROCESSED | 57551.5915972222 | 2016-06-12 14:11:54 | 55287 | 2010-04-01 00:00:00 | 55355.1545833333 | 2010-06-08 03:42:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505023010/ | Quick Look | ![]() |
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1175 | WESTERLUND1_1 | 251.8398 | -46.6023 | 250.920426 | -46.513379 | 256.432477 | -24.011612 | 339.00946678 | -0.92860911 | 283.3468 | 55449.7733217593 | 2010-09-10 18:33:35 | 55451.2015740741 | 2010-09-12 04:50:16 | 505049010 | 51.932 | 50 | 51.932 | 51.932 | 0 | 51.932 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.8437 | 44.8437 | 123.3861 | 1 | PROCESSED | 57553.3910532407 | 2016-06-14 09:23:07 | 55829 | 2011-09-25 00:00:00 | 55461.3235069444 | 2010-09-22 07:45:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505049010/ | Quick Look | ![]() |
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1176 | CYGNUS LOOP W-B-N | 311.1498 | 30.6623 | 310.633359 | 30.480063 | 325.327706 | 46.517719 | 73.11766027 | -7.48614398 | 71.1125 | 55692.7736574074 | 2011-05-11 18:34:04 | 55693.7709606482 | 2011-05-12 18:30:11 | 506007010 | 45.9006 | 44 | 45.9006 | 45.9006 | 0 | 45.9006 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8337 | 40.8337 | 86.1339 | 0 | PROCESSED | 57602.0331597222 | 2016-08-02 00:47:45 | 56072 | 2012-05-25 00:00:00 | 55705.1432523148 | 2011-05-24 03:26:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 6 | AO6 | HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506007010/ | Quick Look | ![]() |
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1177 | CYGNUS LOOP BLOWOUT4 | 312.6611 | 29.185 | 312.13473 | 28.997294 | 326.258052 | 44.653722 | 72.76042835 | -9.42856877 | 61.4261 | 55707.9937268518 | 2011-05-26 23:50:58 | 55708.6620486111 | 2011-05-27 15:53:21 | 506014010 | 26.0551 | 25 | 26.0551 | 26.0631 | 0 | 26.0711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2713 | 20.2713 | 57.7379 | 0 | PROCESSED | 57602.1387037037 | 2016-08-02 03:19:44 | 56092 | 2012-06-14 00:00:00 | 55725.2494097222 | 2011-06-13 05:59:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506014010/ | Quick Look | ![]() |
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1178 | S147_NE | 85.8826 | 28.3008 | 85.092656 | 28.278902 | 86.363834 | 4.912026 | 180.30181638 | -0.72311498 | 273.9004 | 55996.1741666667 | 2012-03-10 04:10:48 | 55997.2919097222 | 2012-03-11 07:00:21 | 506030010 | 48.0142 | 45 | 48.0302 | 48.0142 | 0 | 48.0382 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.608 | 42.608 | 96.5559 | 0 | PROCESSED | 57604.8622685185 | 2016-08-04 20:41:40 | 56385 | 2013-04-03 00:00:00 | 56016.6658912037 | 2012-03-30 15:58:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHITAKA HANABATA | JAP | 6 | AO6 | STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506030010/ | Quick Look | ![]() |
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1179 | FERMI_BUBBLE_N1 | 234.2494 | 5.0833 | 233.629011 | 5.247167 | 230.509588 | 23.755664 | 11.24626366 | 44.86747445 | 287.5001 | 56144.9615277778 | 2012-08-05 23:04:36 | 56145.3981365741 | 2012-08-06 09:33:19 | 507001010 | 21.0485 | 20 | 21.0485 | 21.0485 | 0 | 21.0485 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.5275 | 17.5275 | 37.7199 | 1 | PROCESSED | 57606.7753703704 | 2016-08-06 18:36:32 | 56533 | 2013-08-29 00:00:00 | 56167.2004166667 | 2012-08-28 04:48:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507001010/ | Quick Look | ![]() |
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1180 | FERMI_BUBBLE_N8 | 234.713 | 2.1937 | 234.081258 | 2.355767 | 231.775859 | 21.073749 | 8.32709248 | 42.83416107 | 287.4999 | 56148.4316782407 | 2012-08-09 10:21:37 | 56148.9953240741 | 2012-08-09 23:53:16 | 507008010 | 22.115 | 20 | 22.119 | 22.115 | 0 | 22.123 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22.3246 | 22.3246 | 48.694 | 0 | PROCESSED | 57606.8152546296 | 2016-08-06 19:33:58 | 56536 | 2013-09-01 00:00:00 | 56169.1379976852 | 2012-08-30 03:18:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507008010/ | Quick Look | ![]() |
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1181 | FERMI_BUBBLE_S5 | 332.6607 | -46.1905 | 331.884331 | -46.436996 | 316.726495 | -32.387556 | 351.01438321 | -53.09632639 | 44.0062 | 56036.5915625 | 2012-04-19 14:11:51 | 56037.1140972222 | 2012-04-20 02:44:18 | 507013010 | 21.0044 | 20 | 21.0124 | 21.0204 | 0 | 21.0044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.8854 | 20.8854 | 45.1099 | 0 | PROCESSED | 57605.2184259259 | 2016-08-05 05:14:32 | 56420 | 2013-05-08 00:00:00 | 56049.260787037 | 2012-05-02 06:15:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507013010/ | Quick Look | ![]() |
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1182 | GC_SOUTH_4 | 268.4148 | -29.4524 | 267.616941 | -29.442757 | 268.602472 | -6.019039 | 0.45858363 | -1.77042753 | 273.9837 | 56206.6347106482 | 2012-10-06 15:13:59 | 56207.6987731482 | 2012-10-07 16:46:14 | 507031010 | 52.8743 | 50 | 52.8903 | 52.8903 | 0 | 52.8743 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 54.1402 | 54.1402 | 91.9199 | 0 | PROCESSED | 57607.3059837963 | 2016-08-07 07:20:37 | 56595 | 2013-10-30 00:00:00 | 56226.5383449074 | 2012-10-26 12:55:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507031010/ | Quick Look | ![]() |
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1183 | G32.8-0.1 NORTH | 282.8355 | -0.0511 | 282.194351 | -0.111437 | 283.93132 | 22.770824 | 32.87550481 | -0.00195799 | 74.4992 | 56037.6100347222 | 2012-04-20 14:38:27 | 56038.7897685185 | 2012-04-21 18:57:16 | 507035010 | 55.1475 | 50 | 55.1475 | 55.1475 | 0 | 55.1475 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 53.4834 | 53.4834 | 101.9259 | 0 | PROCESSED | 57605.250162037 | 2016-08-05 06:00:14 | 56421 | 2013-05-09 00:00:00 | 56054.2396990741 | 2012-05-07 05:45:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507035010/ | Quick Look | ![]() |
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1184 | W44_SOUTH | 284.0612 | 1.21 | 283.425992 | 1.143849 | 285.397736 | 23.902065 | 34.55680978 | -0.51750637 | 254.9998 | 56587.9436921296 | 2013-10-22 22:38:55 | 56589.5105671296 | 2013-10-24 12:15:13 | 508003010 | 66.7193 | 100 | 66.7333 | 66.7284 | 0 | 66.7193 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 59.54 | 59.54 | 135.3439 | 0 | PROCESSED | 57613.1119675926 | 2016-08-13 02:41:14 | 57193 | 2015-06-20 00:00:00 | 56603.6796180556 | 2013-11-07 16:18:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508003010/ | Quick Look | ![]() |
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1185 | W28_SOUTH | 270.2594 | -23.5602 | 269.497229 | -23.559609 | 270.228192 | -0.119534 | 6.38554367 | -0.24638203 | 269.9307 | 56938.465162037 | 2014-10-08 11:09:50 | 56939.7308101852 | 2014-10-09 17:32:22 | 508006020 | 61.7346 | 60 | 61.7346 | 61.7385 | 0 | 61.7465 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6318402778 | 2016-08-16 15:09:51 | 57359 | 2015-12-03 00:00:00 | 56993.4258333333 | 2014-12-02 10:13:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080017 | A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP. | GALACTIC DIFFUSE EMISSION | 5 | A | MAKOTO SAWADA | JAP | 8 | AO8 | INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508006020/ | Quick Look | ![]() |
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1186 | NW_BGD | 233.685 | -9.8963 | 233.005634 | -9.73009 | 233.775325 | 9.095249 | 355.50550051 | 35.80785483 | 289.7923 | 56499.8451041667 | 2013-07-26 20:16:57 | 56500.4266319445 | 2013-07-27 10:14:21 | 508008010 | 24.1275 | 20 | 24.1275 | 24.1275 | 0 | 24.1275 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.0402 | 22.0402 | 50.216 | 1 | PROCESSED | 57612.0809953704 | 2016-08-12 01:56:38 | 56955 | 2014-10-25 00:00:00 | 56587.4600578704 | 2013-10-22 11:02:29 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508008010/ | Quick Look | ![]() |
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1187 | CAS A | 350.8384 | 58.8278 | 350.272774 | 58.553239 | 27.387727 | 54.868389 | 111.73335389 | -2.11549771 | 73.3126 | 56828.040162037 | 2014-06-20 00:57:50 | 56828.7711111111 | 2014-06-20 18:30:24 | 508011020 | 28.0732 | 30 | 28.0812 | 28.0732 | 0 | 29.7402 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 30.9971 | 30.9971 | 63.1439 | 2 | PROCESSED | 57615.2981712963 | 2016-08-15 07:09:22 | 57206 | 2015-07-03 00:00:00 | 56839.7807986111 | 2014-07-01 18:44:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080021 | 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 | B | YOSHITOMO MAEDA | JAP | 8 | AO8 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508011020/ | Quick Look | ![]() |
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1188 | HESS J1641-463 | 250.6069 | -46.2544 | 249.692976 | -46.159834 | 255.458921 | -23.78613 | 338.71856162 | -0.05766971 | 282.1914 | 56898.1501736111 | 2014-08-29 03:36:15 | 56898.2719907407 | 2014-08-29 06:31:40 | 509010010 | 0 | 40 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5288773148 | 2016-08-16 12:41:35 | 56748 | 2014-04-01 00:00:00 | 56979.4106944445 | 2014-11-18 09:51:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090045 | The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 9 | AO9 | IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509010010/ | Quick Look | ![]() |
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1189 | G166.0+4.3_SE | 81.6669 | 42.6537 | 80.773056 | 42.61122 | 83.513405 | 19.400906 | 166.36639381 | 4.14814693 | 85.0186 | 56921.2402777778 | 2014-09-21 05:46:00 | 56922.0209606482 | 2014-09-22 00:30:11 | 509024010 | 31.2731 | 60 | 31.2731 | 34.2171 | 0 | 34.2731 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5684722222 | 2016-08-16 13:38:36 | 57626 | 2016-08-26 00:00:00 | 56945.4935532407 | 2014-10-15 11:50:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024010/ | Quick Look | ![]() |
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1190 | N4438 TAIL | 186.7653 | 12.9509 | 186.13191 | 13.227515 | 180.954769 | 14.552434 | 279.81897455 | 74.71807646 | 119.2941 | 56636.4959259259 | 2013-12-10 11:54:08 | 56639.0884259259 | 2013-12-13 02:07:20 | 808045010 | 102.7738 | 100 | 102.7738 | 102.7738 | 0 | 102.7738 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.8342 | 92.8342 | 223.962 | 2 | PROCESSED | 57613.6203587963 | 2016-08-13 14:53:19 | 57016 | 2014-12-25 00:00:00 | 56650.8089583333 | 2013-12-24 19:24:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080059 | We propose a 100 ks XIS observation to the Halpha/X-ray filament connecting N4438 and M86 in the Virgo cluster. Our main objective is to probe conclusively the OVII line which is marginally detected with the XMM-Newton. If established, by employing line diagnostic and non-equilibrium ionization analysis, we will be able to determine the ionization temperature and elapsed timescale of the multi-phase ISM stripped from N4438, and give constraint on the thermal conductivity and metal enrichment of the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LIYI GU | JAP | 8 | AO8 | A SUZAKU OBSERVATION OF ONGOING IONIZATION OF ISM IN THE VIRGO CLUSTER ICM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808045010/ | Quick Look | ![]() |
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1191 | A399&A401 FILAMENT | 44.5739 | 13.3044 | 43.887717 | 13.104923 | 46.011939 | -3.472452 | 164.23302583 | -39.1861165 | 71.9992 | 56522.5065972222 | 2013-08-18 12:09:30 | 56523.421724537 | 2013-08-19 10:07:17 | 808005010 | 42.1655 | 40 | 42.1655 | 42.1655 | 0 | 42.1655 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.981 | 40.981 | 79.0638 | 2 | PROCESSED | 57612.3602083333 | 2016-08-12 08:38:42 | 56956 | 2014-10-26 00:00:00 | 56587.6829398148 | 2013-10-22 16:23:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHITAKA ISHISAKI | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808005010/ | Quick Look | ![]() |
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1192 | A2255_SE | 258.2963 | 63.8192 | 258.210545 | 63.875842 | 203.735886 | 84.382935 | 93.63129587 | 34.92006939 | 200.0025 | 56613.9474537037 | 2013-11-17 22:44:20 | 56615.3084953704 | 2013-11-19 07:24:14 | 808040010 | 64.733 | 60 | 64.741 | 64.741 | 0 | 64.733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8865 | 64.8865 | 117.5879 | 1 | PROCESSED | 57613.3519097222 | 2016-08-13 08:26:45 | 57029 | 2015-01-07 00:00:00 | 56653.6890046296 | 2013-12-27 16:32:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080047 | We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROKO YOSHIDA | JAP | 8 | AO8 | MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808040010/ | Quick Look | ![]() |
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1193 | 3C390.3_VICINITY_2 | 284.1264 | 79.7065 | 284.963939 | 79.636578 | 79.391227 | 76.323687 | 111.42410994 | 26.43157038 | 239.9994 | 56608.493900463 | 2013-11-12 11:51:13 | 56609.4897222222 | 2013-11-13 11:45:12 | 808047010 | 52.8856 | 50 | 52.9066 | 52.8936 | 0 | 52.8856 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.4013 | 48.4013 | 86.0319 | 0 | PROCESSED | 57613.3036111111 | 2016-08-13 07:17:12 | 56991 | 2014-11-30 00:00:00 | 56625.7010648148 | 2013-11-29 16:49:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080060 | We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO SAKAI | JAP | 8 | AO8 | DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808047010/ | Quick Look | ![]() |
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1194 | NGC1550_45OFFSET_E | 65.5544 | 2.4106 | 64.903424 | 2.293944 | 64.093741 | -18.859585 | 191.40103429 | -31.31407553 | 260.0002 | 56696.1115393518 | 2014-02-08 02:40:37 | 56697.3543634259 | 2014-02-09 08:30:17 | 808060010 | 53.0496 | 50 | 53.0496 | 53.0496 | 0 | 53.0496 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8049421296 | 2016-08-13 19:19:07 | 57075 | 2015-02-22 00:00:00 | 56709.7114351852 | 2014-02-21 17:04:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080110 | We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TORU SASAKI | JAP | 8 | AO8 | STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808060010/ | Quick Look | ![]() |
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1195 | THE MOON | 141.5744 | 9.879 | 140.90311 | 10.096072 | 140.776608 | -4.942339 | 222.40545014 | 38.80103529 | 285.4041 | 56784.4506712963 | 2014-05-07 10:48:58 | 56784.5827662037 | 2014-05-07 13:59:11 | 809001080 | 5.6107 | 45 | 5.6107 | 5.6107 | 0 | 5.6107 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.507 | 5.507 | 11.3919 | 0 | PROCESSED | 57615.0708217593 | 2016-08-15 01:41:59 | 57220 | 2015-07-17 00:00:00 | 56854.5770717593 | 2014-07-16 13:50:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001080/ | Quick Look | ![]() |
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1196 | THE MOON | 22.6503 | 9.5807 | 21.992046 | 9.323163 | 24.491955 | 0.094055 | 138.76659478 | -52.08288303 | 73.7999 | 56856.8890277778 | 2014-07-18 21:20:12 | 56857.0196412037 | 2014-07-19 00:28:17 | 809001130 | 5.3017 | 45 | 5.3017 | 5.3017 | 0 | 5.3017 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4036574074 | 2016-08-15 09:41:16 | 57267 | 2015-09-02 00:00:00 | 56902.5802314815 | 2014-09-02 13:55:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001130/ | Quick Look | ![]() |
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1197 | THE MOON | 26.0744 | 9.9879 | 25.412732 | 9.737134 | 27.784882 | -0.749126 | 143.76867514 | -50.73288629 | 73.7996 | 56857.1528472222 | 2014-07-19 03:40:06 | 56857.2765856482 | 2014-07-19 06:38:17 | 809001150 | 3.9169 | 45 | 3.9169 | 3.9169 | 0 | 3.9169 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4069097222 | 2016-08-15 09:45:57 | 57235 | 2015-08-01 00:00:00 | 56869.6125925926 | 2014-07-31 14:42:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001150/ | Quick Look | ![]() |
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1198 | THE MOON | 147.1957 | 8.7504 | 146.531357 | 8.983511 | 146.407447 | -4.210959 | 227.18440299 | 43.16589995 | 105.6994 | 56975.9388541667 | 2014-11-14 22:31:57 | 56976.0626388889 | 2014-11-15 01:30:12 | 809001260 | 6.33 | 45 | 6.33 | 6.442 | 0 | 6.442 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7804513889 | 2016-08-16 18:43:51 | 57359 | 2015-12-03 00:00:00 | 56992.418587963 | 2014-12-01 10:02:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001260/ | Quick Look | ![]() |
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1199 | THE MOON | 333.6436 | -6.6185 | 332.98809 | -6.867271 | 333.149604 | 3.9961 | 54.50784287 | -47.51853169 | 249.2061 | 56990.1023958333 | 2014-11-29 02:27:27 | 56990.2084837963 | 2014-11-29 05:00:13 | 809001300 | 3.8788 | 45 | 3.8828 | 3.8788 | 0 | 3.8868 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4075115741 | 2016-08-17 09:46:49 | 57415 | 2016-01-28 00:00:00 | 57049.4536805556 | 2015-01-27 10:53:18 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001300/ | Quick Look | ![]() |
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1200 | THE MOON | 339.1671 | -5.6557 | 338.516198 | -5.915354 | 338.624224 | 2.887463 | 60.63287277 | -51.42821416 | 248.2317 | 56990.4856828704 | 2014-11-29 11:39:23 | 56990.608587963 | 2014-11-29 14:36:22 | 809001330 | 6.3646 | 45 | 6.3646 | 6.3646 | 0 | 6.3646 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4115856482 | 2016-08-17 09:52:41 | 57415 | 2016-01-28 00:00:00 | 57006.4031018518 | 2014-12-15 09:40:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001330/ | Quick Look | ![]() |
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1201 | RCW86_NORTH | 220.4956 | -62.2074 | 219.51679 | -61.994077 | 240.607034 | -43.72111 | 315.43082177 | -2.04872285 | 96.1584 | 54860.901099537 | 2009-01-29 21:37:35 | 54862.1175231482 | 2009-01-31 02:49:14 | 503002010 | 55.376 | 50 | 55.384 | 55.384 | 0 | 55.376 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2731 | 50.2731 | 105.0818 | 2 | PROCESSED | 57545.4267939815 | 2016-06-06 10:14:35 | 55329 | 2010-05-13 00:00:00 | 54880.5551041667 | 2009-02-18 13:19:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503002010/ | Quick Look | ![]() |
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1202 | CYGNUS_LOOP_P15 | 312.9857 | 30.6621 | 312.465734 | 30.473222 | 327.433989 | 45.909388 | 74.106397 | -8.72540127 | 61.9987 | 53880.177974537 | 2006-05-25 04:16:17 | 53880.6716898148 | 2006-05-25 16:07:14 | 501032010 | 20.7289 | 21 | 20.7289 | 20.7289 | 20.7289 | 20.7289 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.476 | 17.476 | 42.6349 | 0 | PROCESSED | 57534.4101041667 | 2016-05-26 09:50:33 | 54394 | 2007-10-21 00:00:00 | 53926.2440046296 | 2006-07-10 05:51:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501032010/ | Quick Look | ![]() |
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1203 | GC19 | 265.8593 | -28.4466 | 265.068242 | -28.424576 | 266.336192 | -5.058113 | 0.1669402 | 0.66404713 | 262.6738 | 54384.9647569444 | 2007-10-11 23:09:15 | 54385.4112731482 | 2007-10-12 09:52:14 | 502007010 | 22.0174 | 20 | 22.0174 | 22.0414 | 0 | 22.0254 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.5248 | 19.5248 | 38.572 | 0 | PROCESSED | 57540.2498842593 | 2016-06-01 05:59:50 | 54771 | 2008-11-01 00:00:00 | 54402.4381365741 | 2007-10-29 10:30:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502007010/ | Quick Look | ![]() |
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1204 | VELA JR P16 | 132.6844 | -46.1051 | 132.256587 | -45.917087 | 158.947915 | -59.751955 | 265.94403391 | -1.24290223 | 347.0001 | 54291.4605671296 | 2007-07-10 11:03:13 | 54291.7363773148 | 2007-07-10 17:40:23 | 502038010 | 16.442 | 10 | 16.45 | 16.45 | 0 | 16.442 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.277 | 16.277 | 23.8239 | 1 | PROCESSED | 57539.143900463 | 2016-05-31 03:27:13 | 54696 | 2008-08-18 00:00:00 | 54328.4979398148 | 2007-08-16 11:57:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502038010/ | Quick Look | ![]() |
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1205 | GC_LARGEPROJECT12 | 264.5561 | -31.5945 | 263.745071 | -31.566119 | 265.306919 | -8.241878 | 356.89942182 | -0.04701536 | 96.416 | 54881.313900463 | 2009-02-19 07:32:01 | 54881.6919444445 | 2009-02-19 16:36:24 | 503018030 | 11.914 | 10 | 11.922 | 11.922 | 0 | 11.914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.0909 | 10.0909 | 32.6579 | 1 | PROCESSED | 57545.5776041667 | 2016-06-06 13:51:45 | 54557 | 2008-04-01 00:00:00 | 54895.5872106482 | 2009-03-05 14:05:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018030/ | Quick Look | ![]() |
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1206 | HESSJ1614-B | 243.5783 | -51.8962 | 242.621623 | -51.770198 | 251.47747 | -30.138638 | 331.46625372 | -0.63583262 | 283.7142 | 54730.5632291667 | 2008-09-21 13:31:03 | 54731.2779166667 | 2008-09-22 06:40:12 | 503074010 | 52.6342 | 50 | 52.6422 | 52.6342 | 0 | 52.6342 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.953 | 42.953 | 61.7359 | 0 | PROCESSED | 57543.9760763889 | 2016-06-04 23:25:33 | 55148 | 2009-11-13 00:00:00 | 54780.4609490741 | 2008-11-10 11:03:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIRONORI MATSUMOTO | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503074010/ | Quick Look | ![]() |
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1207 | 2MASX J02485937+2630 | 42.225 | 26.5707 | 41.491892 | 26.363374 | 47.759882 | 9.863115 | 153.13364356 | -29.32417791 | 74.088 | 55030.159224537 | 2009-07-18 03:49:17 | 55031.3766782407 | 2009-07-19 09:02:25 | 704013010 | 42.9501 | 40 | 42.9501 | 43.2153 | 0 | 43.2247 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5403 | 29.5403 | 105.1719 | 0 | PROCESSED | 57547.8817013889 | 2016-06-08 21:09:39 | 55415 | 2010-08-07 00:00:00 | 55048.2541435185 | 2009-08-05 06:05:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704013010/ | Quick Look | ![]() |
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1208 | 2FGL J0923.5+1508 | 140.9887 | 15.0811 | 140.300178 | 15.296347 | 138.613889 | -0.175811 | 215.96780071 | 40.48329137 | 287.9737 | 56046.2642939815 | 2012-04-29 06:20:35 | 56048.4933449074 | 2012-05-01 11:50:25 | 707007010 | 95.2554 | 90 | 95.2794 | 95.2554 | 0 | 95.2794 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.5878 | 89.5878 | 192.568 | 1 | PROCESSED | 57605.3423611111 | 2016-08-05 08:13:00 | 56434 | 2013-05-22 00:00:00 | 56068.6261921296 | 2012-05-21 15:01:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSUKE TAKAHASHI | JAP | 7 | AO7 | SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707007010/ | Quick Look | ![]() |
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1209 | VELA JR P19 | 133.9797 | -46.1476 | 133.547729 | -45.954999 | 160.484775 | -59.304415 | 266.55257885 | -0.58147519 | 346.9993 | 54650.629849537 | 2008-07-03 15:06:59 | 54651.2362731482 | 2008-07-04 05:40:14 | 503031010 | 19.8174 | 10 | 19.8174 | 19.8174 | 0 | 19.8174 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.1564 | 17.1564 | 52.3839 | 1 | PROCESSED | 57542.9517824074 | 2016-06-03 22:50:34 | 55036 | 2009-07-24 00:00:00 | 54665.3240393518 | 2008-07-18 07:46:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503031010/ | Quick Look | ![]() |
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1210 | EMS1160 | 264.608 | 87.3047 | 269.889788 | 87.318057 | 90.726547 | 69.241949 | 120.03425165 | 27.94259409 | 59.9344 | 55312.9874537037 | 2010-04-26 23:41:56 | 55313.4279513889 | 2010-04-27 10:16:15 | 705012010 | 20.2796 | 20 | 20.2796 | 20.2796 | 0 | 20.2796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.8004 | 19.8004 | 38.0539 | 1 | PROCESSED | 57551.2894097222 | 2016-06-12 06:56:45 | 55693 | 2011-05-12 00:00:00 | 55327.1544791667 | 2010-05-11 03:42:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705012010/ | Quick Look | ![]() |
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1211 | EMS1388 | 309.878 | -56.3562 | 308.912808 | -56.532938 | 296.209629 | -36.489343 | 341.17879119 | -37.12820094 | 256.6037 | 55497.456400463 | 2010-10-28 10:57:13 | 55498.1383912037 | 2010-10-29 03:19:17 | 705028010 | 21.5336 | 20 | 21.5416 | 21.5416 | 0 | 21.5336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.3735 | 18.3735 | 58.9099 | 0 | PROCESSED | 57553.876724537 | 2016-06-14 21:02:29 | 55875 | 2011-11-10 00:00:00 | 55508.9886342593 | 2010-11-08 23:43:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUYUKI TANAKA | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705028010/ | Quick Look | ![]() |
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1212 | NGC2273 | 102.5972 | 60.7838 | 101.469265 | 60.841838 | 97.733599 | 37.680709 | 155.04232679 | 23.32753471 | 246.2514 | 54211.2737384259 | 2007-04-21 06:34:11 | 54212.5071643518 | 2007-04-22 12:10:19 | 702003010 | 90.0126 | 50 | 90.0286 | 90.0206 | 0 | 90.0126 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.5887 | 69.5887 | 106.5579 | 1 | PROCESSED | 57538.4439583333 | 2016-05-30 10:39:18 | 54744 | 2008-10-05 00:00:00 | 54216.1628703704 | 2007-04-26 03:54:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HISAMITSU AWAKI | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/702003010/ | Quick Look | ![]() |
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1213 | NGC 4941 | 196.0528 | -5.5595 | 195.404956 | -5.291518 | 196.919842 | 1.18027 | 308.80102111 | 57.16661738 | 292.811 | 56100.4695833333 | 2012-06-22 11:16:12 | 56102.2446643518 | 2012-06-24 05:52:19 | 707001010 | 80.8593 | 80 | 80.8593 | 80.8593 | 0 | 80.8593 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.7486 | 76.7486 | 153.32 | 1 | PROCESSED | 57605.7725115741 | 2016-08-05 18:32:25 | 56480 | 2013-07-07 00:00:00 | 56113.2872800926 | 2012-07-05 06:53:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YOSHIHIRO UEDA | JAP | 7 | AO7 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707001010/ | Quick Look | ![]() |
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1214 | 2FGL J0022.2-1853 | 5.5431 | -18.8956 | 4.911171 | -19.172887 | 357.260083 | -19.481593 | 82.15155077 | -79.37005347 | 62.0041 | 56077.5533564815 | 2012-05-30 13:16:50 | 56078.2856944445 | 2012-05-31 06:51:24 | 707009010 | 34.8678 | 30 | 34.8678 | 34.8678 | 0 | 34.8678 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.1964 | 35.1964 | 63.2639 | 1 | PROCESSED | 57605.5769444444 | 2016-08-05 13:50:48 | 56456 | 2013-06-13 00:00:00 | 56090.1516435185 | 2012-06-12 03:38:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707009010/ | Quick Look | ![]() |
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1215 | NGC1365 | 53.4048 | -36.1458 | 52.927471 | -36.312752 | 36.803781 | -53.045581 | 237.96516908 | -54.5951856 | 59.0002 | 56116.8446064815 | 2012-07-08 20:16:14 | 56117.6910763889 | 2012-07-09 16:35:09 | 707017020 | 33.5858 | 30 | 33.5938 | 33.6018 | 0 | 33.5858 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.579 | 32.579 | 73.1059 | 2 | PROCESSED | 57606.5919791667 | 2016-08-06 14:12:27 | 56508 | 2013-08-04 00:00:00 | 56142.1709606482 | 2012-08-03 04:06:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUSHI FUKAZAWA | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/707017020/ | Quick Look | ![]() |
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1216 | NGC 3516 | 166.74 | 72.5773 | 165.887815 | 72.847717 | 123.371896 | 57.999258 | 133.21492543 | 42.40213112 | 153.6201 | 56572.1874537037 | 2013-10-07 04:29:56 | 56573.9780092593 | 2013-10-08 23:28:20 | 708006050 | 0 | 50 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 37.2053 | 37.2053 | 154.6998 | 0 | PROCESSED | 57612.8632291667 | 2016-08-12 20:43:03 | 56383 | 2013-04-01 00:00:00 | 56631.766712963 | 2013-12-05 18:24:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HIROFUMI NODA | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/708006050/ | Quick Look | ![]() |
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1217 | WKK 4438 | 223.8214 | -51.5512 | 222.94068 | -51.348796 | 237.577105 | -33.176773 | 321.7239088 | 6.74451921 | 87.8973 | 55948.1066319445 | 2012-01-22 02:33:33 | 55950.0610069444 | 2012-01-24 01:27:51 | 706011010 | 70.3088 | 100 | 70.3168 | 70.3088 | 0 | 70.3248 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.486 | 61.486 | 168.8259 | 3 | PROCESSED | 57604.5330324074 | 2016-08-04 12:47:34 | 56469 | 2013-06-26 00:00:00 | 56103.2331597222 | 2012-06-25 05:35:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHI TERASHIMA | JAP | 6 | AO6 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706011010/ | Quick Look | ![]() |
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1218 | COMA SUBHALO4 | 193.8668 | 27.5167 | 193.260337 | 27.78729 | 180.744108 | 30.556584 | 56.62578598 | 89.02439779 | 314.9971 | 56453.5916666667 | 2013-06-10 14:12:00 | 56454.1370717593 | 2013-06-11 03:17:23 | 808022010 | 23.8091 | 20 | 23.8091 | 23.8331 | 0 | 23.8171 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.6195 | 19.6195 | 47.1139 | 0 | PROCESSED | 57611.5223958333 | 2016-08-11 12:32:15 | 56830 | 2014-06-22 00:00:00 | 56464.6326041667 | 2013-06-21 15:10:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808022010/ | Quick Look | ![]() |
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1219 | A85 | 10.4739 | -9.4292 | 9.841504 | -9.703266 | 5.843917 | -12.80705 | 115.23010576 | -72.15810594 | 248.2856 | 54105.4020023148 | 2007-01-05 09:38:53 | 54108.0557175926 | 2007-01-08 01:20:14 | 801041010 | 99.2012 | 100 | 99.2012 | 99.2012 | 0 | 99.2012 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.8139 | 84.8139 | 229.2421 | 2 | PROCESSED | 57536.5180671296 | 2016-05-28 12:26:01 | 54735 | 2008-09-26 00:00:00 | 54132.9388773148 | 2007-02-01 22:31:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYO SHIBATA | JAP | 1 | AO1 | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801041010/ | Quick Look | ![]() |
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1220 | PERSEUS OFFSET-G | 50.3247 | 41.3807 | 49.497049 | 41.201455 | 58.859538 | 22.134977 | 150.89015689 | -13.2150361 | 270.0001 | 55596.3541550926 | 2011-02-04 08:29:59 | 55596.8335648148 | 2011-02-04 20:00:20 | 805047010 | 19.6768 | 25 | 19.7008 | 19.6928 | 0 | 19.6768 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.192 | 13.192 | 41.4119 | 1 | PROCESSED | 57600.8412731482 | 2016-07-31 20:11:26 | 55979 | 2012-02-22 00:00:00 | 55613.0840856482 | 2011-02-21 02:01:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805047010/ | Quick Look | ![]() |
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1221 | FORNAX A EAST LOBE | 51.0149 | -37.2799 | 50.539015 | -37.455999 | 33.113805 | -53.302729 | 240.23704173 | -56.41225665 | 91.5022 | 56506.6358564815 | 2013-08-02 15:15:38 | 56510.623125 | 2013-08-06 14:57:18 | 808043010 | 151.4626 | 150 | 151.4866 | 151.4626 | 0 | 151.4946 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134.0942 | 134.0942 | 344.4353 | 3 | PROCESSED | 57612.2277777778 | 2016-08-12 05:28:00 | 56955 | 2014-10-25 00:00:00 | 56587.7734259259 | 2013-10-22 18:33:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080056 | We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 8 | AO8 | COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808043010/ | Quick Look | ![]() |
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1222 | THE MOON | 148.554 | 8.0651 | 147.892313 | 8.301757 | 147.907786 | -4.401986 | 228.92553687 | 43.99318882 | 105.699 | 56976.0638541667 | 2014-11-15 01:31:57 | 56976.1876388889 | 2014-11-15 04:30:12 | 809001270 | 5.9536 | 45 | 5.9536 | 5.9616 | 0 | 5.9616 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7826967593 | 2016-08-16 18:47:05 | 57359 | 2015-12-03 00:00:00 | 56992.4196527778 | 2014-12-01 10:04:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001270/ | Quick Look | ![]() |
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1223 | CEN_A_LOBE_N3 | 200.614 | -42.0794 | 199.886702 | -41.818146 | 216.080144 | -30.721221 | 309.06646515 | 20.4225822 | 293.3211 | 56862.6955439815 | 2014-07-24 16:41:35 | 56864.2709722222 | 2014-07-26 06:30:12 | 809004010 | 51.4894 | 50 | 51.4894 | 51.4894 | 0 | 51.4894 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6384 | 10.6384 | 21.48 | 0 | PROCESSED | 57615.4562384259 | 2016-08-15 10:56:59 | 57242 | 2015-08-08 00:00:00 | 56875.2082175926 | 2014-08-06 04:59:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809004010/ | Quick Look | ![]() |
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1224 | AX J1846.8-0240 | 281.7182 | -2.6613 | 281.064619 | -2.716297 | 282.480418 | 20.272966 | 30.04319345 | -0.19850989 | 89.4057 | 56018.0125115741 | 2012-04-01 00:18:01 | 56019.1146990741 | 2012-04-02 02:45:10 | 407019010 | 37.6209 | 40 | 37.6209 | 41.6127 | 0 | 39.2207 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.25 | 37.25 | 95.2199 | 0 | PROCESSED | 57605.0756944445 | 2016-08-05 01:49:00 | 56400 | 2013-04-18 00:00:00 | 56033.2323032407 | 2012-04-16 05:34:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUO MAKISHIMA | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/407019010/ | Quick Look | ![]() |
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1225 | N1550_CENTER | 64.9488 | 2.4105 | 64.297881 | 2.291179 | 63.464463 | -18.753248 | 191.00239213 | -31.81480775 | 89.9981 | 54694.185474537 | 2008-08-16 04:27:05 | 54696.3009143518 | 2008-08-18 07:13:19 | 803017010 | 83.2702 | 80 | 83.7102 | 83.2702 | 0 | 83.7102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8874 | 64.8874 | 182.756 | 4 | PROCESSED | 57543.367974537 | 2016-06-04 08:49:53 | 55080 | 2009-09-06 00:00:00 | 54713.2652546296 | 2008-09-04 06:21:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030070 | We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 3 | AO3 | OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803017010/ | Quick Look | ![]() |
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1226 | VELA PWN S2 | 128.0787 | -47.1859 | 127.674645 | -47.014943 | 154.605433 | -62.350481 | 264.85904608 | -4.40317226 | 122.1879 | 56989.4162847222 | 2014-11-28 09:59:27 | 56989.8404976852 | 2014-11-28 20:10:19 | 509018010 | 17.4774 | 15 | 17.4774 | 17.4774 | 0 | 17.4774 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4063773148 | 2016-08-17 09:45:11 | 57368 | 2015-12-12 00:00:00 | 57002.436087963 | 2014-12-11 10:27:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, 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. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509018010/ | Quick Look | ![]() |
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1227 | UGC5101 | 143.841 | 61.3185 | 142.895417 | 61.541858 | 122.479903 | 43.806931 | 152.55229096 | 42.85621781 | 331.581 | 53825.1798148148 | 2006-03-31 04:18:56 | 53826.3509722222 | 2006-04-01 08:25:24 | 701002010 | 48.9902 | 70 | 48.9902 | 48.9902 | 48.9902 | 48.9902 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.9748 | 43.9748 | 101.1779 | 0 | PROCESSED | 57533.3610763889 | 2016-05-25 08:39:57 | 54735 | 2008-09-26 00:00:00 | 53905.890625 | 2006-06-19 21:22:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002010/ | Quick Look | ![]() |
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1228 | IRAS13224-3809 | 201.327 | -38.416 | 200.607672 | -38.155977 | 214.865009 | -27.173801 | 310.18598264 | 23.97820794 | 118.5234 | 54126.2420601852 | 2007-01-26 05:48:34 | 54131.0849421296 | 2007-01-31 02:02:19 | 701003010 | 197.9376 | 200 | 197.9536 | 197.9376 | 0 | 197.9516 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 169.6526 | 169.6526 | 418.3978 | 4 | PROCESSED | 57537.0458912037 | 2016-05-29 01:06:05 | 54777 | 2008-11-07 00:00:00 | 54139.7293287037 | 2007-02-08 17:30:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YASUO TANAKA | JAP | 1 | AO1 | THE REMARKABLE NARROW LINE SEYFERT 1 GALAXY IRAS13224-3809 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701003010/ | Quick Look | ![]() |
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1229 | A963E | 154.4148 | 39.0556 | 153.674896 | 39.305871 | 141.440839 | 26.400688 | 182.51717965 | 55.95361494 | 109.3314 | 54427.8082060185 | 2007-11-23 19:23:49 | 54428.4745833333 | 2007-11-24 11:23:24 | 802011010 | 29.0825 | 25 | 29.0825 | 29.0825 | 0 | 29.0825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4699 | 24.4699 | 57.5679 | 0 | PROCESSED | 57540.5746412037 | 2016-06-01 13:47:29 | 54804 | 2008-12-04 00:00:00 | 54434.1859837963 | 2007-11-30 04:27:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MAKOTO HATTORI | JAP | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802011010/ | Quick Look | ![]() |
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1230 | NGC 253 OFFSET | 12.0926 | -25.0475 | 11.478671 | -25.320084 | 0.364314 | -27.643554 | 104.44696227 | -87.8082396 | 247.2843 | 54829.0152430556 | 2008-12-29 00:21:57 | 54830.2502430556 | 2008-12-30 06:00:21 | 803004010 | 56.7104 | 50 | 56.7104 | 56.7104 | 0 | 56.7104 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.3026 | 51.3026 | 106.6718 | 1 | PROCESSED | 57545.0814351852 | 2016-06-06 01:57:16 | 55213 | 2010-01-17 00:00:00 | 54847.4571296296 | 2009-01-16 10:58:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030027 | Suzaku observations of a hot halo of nearby, edge-on starburst galaxy NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by an offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and the dynamics of the galaxy outflow to the intergalactic space. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORIKO YAMASAKI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803004010/ | Quick Look | ![]() |
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1231 | HD130693 | 222.5749 | -24.4173 | 221.849663 | -24.21107 | 227.410153 | -7.711774 | 334.71293898 | 31.01917553 | 104.6337 | 55580.6525925926 | 2011-01-19 15:39:44 | 55581.2384375 | 2011-01-20 05:43:21 | 405031010 | 21.3145 | 20 | 21.3145 | 21.3145 | 0 | 21.3145 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.4625 | 17.4625 | 50.6059 | 2 | PROCESSED | 57600.6648842593 | 2016-07-31 15:57:26 | 55965 | 2012-02-08 00:00:00 | 55598.9831597222 | 2011-02-06 23:35:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KEN EBISAWA | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405031010/ | Quick Look | ![]() |
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1232 | AQL X-1 | 287.8271 | 0.5745 | 287.188805 | 0.490736 | 289.388235 | 22.823139 | 35.71381986 | -4.15705073 | 244.5264 | 55852.1545486111 | 2011-10-18 03:42:33 | 55853.110625 | 2011-10-19 02:39:18 | 406010010 | 9.4948 | 40 | 9.5968 | 9.4948 | 0 | 9.5968 | 2 | 1 | 0 | 1 | 1 | 0 | 0 | 35.325 | 35.325 | 82.5878 | 1 | PROCESSED | 57603.4610763889 | 2016-08-03 11:03:57 | 56240 | 2012-11-09 00:00:00 | 55873.1222337963 | 2011-11-08 02:56:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KAZUTAKA YAMAOKA | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406010010/ | Quick Look | ![]() |
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1233 | 1E1724-3045 | 261.8859 | -30.8016 | 261.081118 | -30.76036 | 262.965781 | -7.558159 | 356.31902476 | 2.29998715 | 95.7568 | 57113.6866087963 | 2015-04-01 16:28:43 | 57115.0028935185 | 2015-04-03 00:04:10 | 409024010 | 60.2315 | 60 | 60.2315 | 60.2515 | 0 | 60.2337 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9445833333 | 2016-08-17 22:40:12 | 57493 | 2016-04-15 00:00:00 | 57126.4247106482 | 2015-04-14 10:11:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090106 | Low Mass X-ray Binaries(LMXBs) have soft and hard state. After breakthrough of hard state accretion geometry in LMXBs Sakurai et al.2012,2013), we found a clue to connect hard/soft states. first, we found that the geometry of GS1826-238 is similar to that of soft state, and is understood in the framework of Sakurai et al. (2012,2013). Second, we found a surprising relation between two physical quantities of corona, which roughly shows a continuous change of relation between soft/hard states in contrast with a dramatic change of their spectra. In order to confirm such a continuous relation between two distinct states, we propose a LMXB, which usually shows hard state with high luminosity. | GALACTIC POINT SOURCES | 4 | B | KO ONO | JAP | 9 | AO9 | TOWARD COMPREHENSIVE UNDERSTANDING OF LMXBS ~OBSERVATION OF HARD STATE WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/409024010/ | Quick Look | ![]() |
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1234 | HESS J1745-303 2 | 266.4705 | -30.0867 | 265.668866 | -30.067612 | 266.916061 | -6.683329 | 359.0474588 | -0.64781783 | 70.5003 | 54531.5601388889 | 2008-03-06 13:26:36 | 54533.6669444444 | 2008-03-08 16:00:24 | 502017010 | 72.5443 | 67 | 72.5523 | 72.5523 | 0 | 72.5443 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.9723 | 63.9723 | 182.0149 | 2 | PROCESSED | 57541.8457291667 | 2016-06-02 20:17:51 | 54919 | 2009-03-29 00:00:00 | 54550.4057986111 | 2008-03-25 09:44:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502017010/ | Quick Look | ![]() |
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1235 | ASO0382 | 265.491 | -20.8915 | 264.744419 | -20.867803 | 265.774532 | 2.483348 | 6.43327069 | 4.9108593 | 101.5727 | 55276.7369328704 | 2010-03-21 17:41:11 | 55277.3869675926 | 2010-03-22 09:17:14 | 504040010 | 21.2223 | 20 | 21.2223 | 21.2223 | 0 | 21.2223 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3.974 | 3.974 | 56.1089 | 2 | PROCESSED | 57550.9335069444 | 2016-06-11 22:24:15 | 55665 | 2011-04-14 00:00:00 | 55299.411875 | 2010-04-13 09:53:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504040010/ | Quick Look | ![]() |
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1236 | A3391&A3395 FILAMENT | 96.6913 | -54.1225 | 96.432969 | -54.090694 | 107.900065 | -77.146986 | 262.85175229 | -25.18315788 | 316.4875 | 56791.0860532407 | 2014-05-14 02:03:55 | 56792.4794328704 | 2014-05-15 11:30:23 | 809033010 | 88.6134 | 92 | 88.6134 | 88.6134 | 0 | 88.6134 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.2448 | 15.2448 | 23.346 | 0 | PROCESSED | 57615.0916319445 | 2016-08-15 02:11:57 | 57227 | 2015-07-24 00:00:00 | 56861.4967361111 | 2014-07-23 11:55:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090082 | To investigate hot gas properties of a large scale filament, we propose Suzaku observation (92 ks) of a filamentary structure between Abell 3391 and Abell 3395. A3391 and A3395 are located in Horologium supercluster and expected to be in an initial phase of a cluster merger. With Suzaku fs high sensitivity observation, we will (i) determine the physical conditions of IntraCluster Medium by measuring the temperature and density distribution, (ii) unveil the origin of the filamentary structure from distribution of abundance, pressure and entropy. Our study will reveal the formation history of the filament and provide a useful information for the future Sunyaev-Zeldovich effect observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOSHITAKA ISHISAKI | JAP | 9 | AO9 | INVESTIGATION OF THE ORIGIN OF THE FILAMENTARY STRUCTURE BETWEEN ABELL 3391 AND ABELL 3395 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809033010/ | Quick Look | ![]() |
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1237 | RXJ1713-3946-BKGD1 | 257.3853 | -38.8228 | 256.526519 | -38.759945 | 259.804008 | -15.82642 | 347.63223985 | 0.70836337 | 270.0091 | 53638.7997685185 | 2005-09-25 19:11:40 | 53639.6542708333 | 2005-09-26 15:42:09 | 100026020 | 34.9284 | 40 | 34.9284 | 34.9284 | 34.9284 | 34.9284 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.3713 | 28.3713 | 73.8199 | 0 | PROCESSED | 57527.432349537 | 2016-05-19 10:22:35 | 54247 | 2007-05-27 00:00:00 | 54035.5347453704 | 2006-10-27 12:50:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JAP | 0 | SWG | Observation of RXJ1713.7-3946 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100026020/ | Quick Look | ![]() |
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1238 | EXTENDED CHIMNEY | 265.9856 | -29.2095 | 265.189699 | -29.188076 | 266.46906 | -5.817544 | 359.57541621 | 0.16970004 | 69.9995 | 54896.1105555556 | 2009-03-06 02:39:12 | 54899.1218171296 | 2009-03-09 02:55:25 | 503072010 | 140.5733 | 133 | 140.5733 | 140.5733 | 0 | 140.5733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135.4784 | 135.4784 | 260.128 | 1 | PROCESSED | 57545.7802546296 | 2016-06-06 18:43:34 | 55330 | 2010-05-14 00:00:00 | 54916.5067361111 | 2009-03-26 12:09:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | TAKESHI TSURU | JAP | 3 | AO3 | THE CHIMNEY OF SGR C : A PART OF A SUPER BUBBLE = A SUPER SHELL ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503072010/ | Quick Look | ![]() |
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1239 | BLOWOUT4 | 312.7282 | 31.6832 | 312.213719 | 31.495234 | 327.721378 | 46.935084 | 74.77065214 | -7.91349372 | 242.7253 | 55160.4733564815 | 2009-11-25 11:21:38 | 55161.0044444445 | 2009-11-26 00:06:24 | 504014010 | 17.7696 | 15 | 17.8257 | 17.7696 | 0 | 17.8256 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14.2657 | 14.2657 | 45.876 | 0 | PROCESSED | 57549.5615509259 | 2016-06-10 13:28:38 | 55545 | 2010-12-15 00:00:00 | 55176.2692939815 | 2009-12-11 06:27:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504014010/ | Quick Look | ![]() |
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1240 | GALACTICDISC3-2 | 16.1096 | 72.7817 | 15.228315 | 72.513728 | 58.016186 | 57.534015 | 123.90816526 | 9.93459858 | 241.5401 | 55216.0250115741 | 2010-01-20 00:36:01 | 55217.5772685185 | 2010-01-21 13:51:16 | 504039010 | 73.5282 | 70 | 73.5282 | 73.5282 | 0 | 73.5282 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.648 | 54.648 | 134.1058 | 1 | PROCESSED | 57550.3049884259 | 2016-06-11 07:19:11 | 55602 | 2011-02-10 00:00:00 | 55236.1178240741 | 2010-02-09 02:49:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | SHUNSUKE KIMURA | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504039010/ | Quick Look | ![]() |
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1241 | CYGNUS LOOP 16 | 312.8966 | 29.5255 | 312.371396 | 29.336949 | 326.707962 | 44.890523 | 73.15999246 | -9.37678246 | 49.3574 | 55343.7003125 | 2010-05-27 16:48:27 | 55344.4932407407 | 2010-05-28 11:50:16 | 505024010 | 34.8338 | 34 | 34.8338 | 34.8338 | 0 | 34.8338 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.4182 | 32.4182 | 68.5079 | 1 | PROCESSED | 57551.6200231482 | 2016-06-12 14:52:50 | 55287 | 2010-04-01 00:00:00 | 55355.2000115741 | 2010-06-08 04:48:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505024010/ | Quick Look | ![]() |
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1242 | HB21 SOUTH | 311.2245 | 50.5821 | 310.838387 | 50.399364 | 342.625257 | 64.000491 | 88.82715261 | 4.80607932 | 6.557 | 55767.8922337963 | 2011-07-25 21:24:49 | 55768.4953819444 | 2011-07-26 11:53:21 | 506005020 | 23.4607 | 20 | 23.4687 | 23.4767 | 0 | 23.4607 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.2649 | 26.2649 | 52.1039 | 1 | PROCESSED | 57602.6622685185 | 2016-08-02 15:53:40 | 56159 | 2012-08-20 00:00:00 | 55792.1611458333 | 2011-08-19 03:52:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA BAMBA | JAP | 6 | AO6 | ORIGIN OF OVER-IONIZATION OF SNR PLASMAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506005020/ | Quick Look | ![]() |
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1243 | JUPITER | 28.6779 | 10.4549 | 28.01316 | 10.209883 | 30.347447 | -1.217435 | 147.25964186 | -49.40473582 | 249.1856 | 55929.8714467593 | 2012-01-03 20:54:53 | 55930.8243865741 | 2012-01-04 19:47:07 | 506006010 | 33.5331 | 160 | 33.5331 | 33.5331 | 0 | 33.5331 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.1369 | 32.1369 | 82.3239 | 1 | PROCESSED | 57604.310625 | 2016-08-04 07:27:18 | 56316 | 2013-01-24 00:00:00 | 55946.1978472222 | 2012-01-20 04:44:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006010/ | Quick Look | ![]() |
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1244 | VELA JR WEST1 | 131.7706 | -46.5645 | 131.349361 | -46.379775 | 158.374389 | -60.478179 | 265.90247722 | -2.02224689 | 126.9994 | 56630.5848611111 | 2013-12-04 14:02:12 | 56631.1640162037 | 2013-12-05 03:56:11 | 508036010 | 28.5509 | 30 | 28.5589 | 28.5589 | 0 | 28.5509 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.35 | 27.35 | 50.0179 | 0 | PROCESSED | 57613.5034375 | 2016-08-13 12:04:57 | 57061 | 2015-02-08 00:00:00 | 56695.6005092593 | 2014-02-07 14:24:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDETOSHI SANO | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508036010/ | Quick Look | ![]() |
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1245 | THE MOON | 132.8593 | 12.3218 | 132.173537 | 12.509929 | 131.851232 | -5.111118 | 215.15290673 | 32.14399459 | 282.2504 | 56783.6861921296 | 2014-05-06 16:28:07 | 56783.8127083333 | 2014-05-06 19:30:18 | 809001020 | 4.6445 | 45 | 4.6445 | 4.6445 | 0 | 4.6605 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.9299 | 4.9299 | 10.9199 | 0 | PROCESSED | 57615.0434143518 | 2016-08-15 01:02:31 | 57162 | 2015-05-20 00:00:00 | 56793.5180324074 | 2014-05-16 12:25:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001020/ | Quick Look | ![]() |
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1246 | CYGNUS_LOOP_P19 | 311.8094 | 30.0818 | 311.288879 | 29.89716 | 325.768852 | 45.764417 | 73.00862935 | -8.2918477 | 237.4997 | 54087.3411805556 | 2006-12-18 08:11:18 | 54087.8245833333 | 2006-12-18 19:47:24 | 501036010 | 18.595 | 17 | 18.595 | 18.595 | 0 | 18.595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.355 | 18.355 | 41.7559 | 0 | PROCESSED | 57536.3627199074 | 2016-05-28 08:42:19 | 54744 | 2008-10-05 00:00:00 | 54096.1443171296 | 2006-12-27 03:27:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501036010/ | Quick Look | ![]() |
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1247 | 1RXS J062518.2+73343 | 96.3307 | 73.5671 | 94.750009 | 73.593987 | 92.79758 | 50.188181 | 140.86801575 | 24.12512545 | 262.0383 | 54570.0388310185 | 2008-04-14 00:55:55 | 54571.1252777778 | 2008-04-15 03:00:24 | 403004010 | 50.3267 | 50 | 50.3267 | 50.3267 | 0 | 50.3267 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.1253 | 50.1253 | 93.8488 | 0 | PROCESSED | 57542.3202430556 | 2016-06-03 07:41:09 | 54953 | 2009-05-02 00:00:00 | 54581.2328472222 | 2008-04-25 05:35:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | MANABU ISHIDA | JAP | 3 | AO3 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403004010/ | Quick Look | ![]() |
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1248 | MARS-P17 | 103.5439 | 25.0908 | 102.776216 | 25.154177 | 102.256232 | 2.224275 | 190.5741012 | 11.71183533 | 298.237 | 54560.6601041667 | 2008-04-04 15:50:33 | 54560.743287037 | 2008-04-04 17:50:20 | 403006170 | 1.9782 | 100 | 1.9782 | 1.9782 | 0 | 1.9782 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.9596 | 1.9596 | 7.182 | 0 | PROCESSED | 57542.0674074074 | 2016-06-03 01:37:04 | 54953 | 2009-05-02 00:00:00 | 54578.0406597222 | 2008-04-22 00:58:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | YUICHIRO EZOE | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006170/ | Quick Look | ![]() |
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1249 | MBM12 | 43.9954 | 19.5008 | 43.287121 | 19.299344 | 47.246432 | 2.625648 | 159.17119109 | -34.46234987 | 73.4994 | 55776.7501388889 | 2011-08-03 18:00:12 | 55780.4398263889 | 2011-08-07 10:33:21 | 506026010 | 150.3202 | 150 | 150.3202 | 150.3202 | 0 | 150.3202 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 143.5349 | 143.5349 | 280.7618 | 5 | PROCESSED | 57602.8321180556 | 2016-08-02 19:58:15 | 56169 | 2012-08-30 00:00:00 | 55802.465625 | 2011-08-29 11:10:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI YOSHITAKE | JAP | 6 | AO6 | OBSERVATION TOWARD MOLECULAR CLOUD MBM12 : VERIFYING SOLAR WIND CHARGE EXCHANGE EMISSION IN THE HELIOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506026010/ | Quick Look | ![]() |
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1250 | W44_WEST | 283.939 | 1.3216 | 283.304324 | 1.256024 | 285.27764 | 24.025907 | 34.60037354 | -0.35787423 | 254.9999 | 56589.5109953704 | 2013-10-24 12:15:50 | 56590.9655324074 | 2013-10-25 23:10:22 | 508002010 | 61.1078 | 60 | 61.1398 | 61.1078 | 0 | 61.1398 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.4458 | 58.4458 | 125.6678 | 1 | PROCESSED | 57613.10125 | 2016-08-13 02:25:48 | 56970 | 2014-11-09 00:00:00 | 56603.7391087963 | 2013-11-07 17:44:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508002010/ | Quick Look | ![]() |
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1251 | A2142 | 239.5312 | 27.2879 | 239.014287 | 27.430116 | 229.09968 | 46.49364 | 44.29837206 | 48.74478569 | 138.1624 | 54104.1546990741 | 2007-01-04 03:42:46 | 54105.3891666667 | 2007-01-05 09:20:24 | 801055010 | 51.4525 | 60 | 51.4605 | 51.4525 | 0 | 51.4605 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.2098 | 49.2098 | 106.632 | 1 | PROCESSED | 57536.4705555556 | 2016-05-28 11:17:36 | 54735 | 2008-09-26 00:00:00 | 54111.417037037 | 2007-01-11 10:00:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | NOBUHIRO OKABE | JAP | 1 | AO1 | REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801055010/ | Quick Look | ![]() |
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1252 | 1RXSJ194246.3+103339 | 295.6976 | 10.5399 | 295.103359 | 10.420476 | 299.93501 | 31.348954 | 48.24168916 | -6.37340779 | 280.0002 | 55848.1433564815 | 2011-10-14 03:26:26 | 55848.635625 | 2011-10-14 15:15:18 | 406035010 | 20.4889 | 20 | 20.4889 | 20.4889 | 0 | 20.4889 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 17.142 | 17.142 | 42.508 | 0 | PROCESSED | 57603.4189583333 | 2016-08-03 10:03:18 | 56240 | 2012-11-09 00:00:00 | 55873.0004861111 | 2011-11-08 00:00:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROMITSU TAKAHASHI | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406035010/ | Quick Look | ![]() |
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1253 | SXDB2 | 305.4808 | 37.2375 | 305.012336 | 37.076849 | 322.528101 | 54.400691 | 75.63404607 | 0.19419319 | 72.9993 | 57170.7872453704 | 2015-05-28 18:53:38 | 57171.5090972222 | 2015-05-29 12:13:06 | 410014010 | 29.3922 | 30 | 29.3959 | 29.3947 | 0 | 29.3922 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.772650463 | 2016-08-18 18:32:37 | 57558 | 2016-06-19 00:00:00 | 57190.4609259259 | 2015-06-17 11:03:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100037 | The soft X-ray sky below 1 keV is spatially smooth after subtracting the local extended emission structures although the interstellar X-ray absorption column density is high enough to block the extragalactic X-ray photons below 1 keV totally in the Galactic disk. Suzaku reveals the existence of "excess" emissions in the Galactic disk and our observations will allow us to study a spatial distribution of the emissions and constrain the origin. | GALACTIC POINT SOURCES | 4 | C | IKUYUKI MITSUISHI | JAP | 10 | AO10 | EXPLORING THE ORIGIN OF SOFT X-RAY DIFFUSE BACKGROUND IN THE GALACTIC DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/410014010/ | Quick Look | ![]() |
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1254 | LMC X -3 | 84.7048 | -64.0785 | 84.635001 | -64.10439 | 45.912813 | -86.683865 | 273.57060216 | -32.09537201 | 185.5067 | 54822.3015856482 | 2008-12-22 07:14:17 | 54823.8675694444 | 2008-12-23 20:49:18 | 403020010 | 73.9738 | 60 | 73.9738 | 73.9818 | 0 | 73.9875 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.0505 | 70.0505 | 135.2838 | 1 | PROCESSED | 57545.0347800926 | 2016-06-06 00:50:05 | 55206 | 2010-01-10 00:00:00 | 54840.5013310185 | 2009-01-09 12:01:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | AYA KUBOTA | JAP | 3 | AO3 | SEARCH FOR IRON K ABSORPTION LINES FROM LMC X-3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403020010/ | Quick Look | ![]() |
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1255 | RIM1 | 311.6421 | 31.883 | 311.130799 | 31.698954 | 326.587321 | 47.481782 | 74.34868893 | -7.06658523 | 247.7276 | 55152.9451273148 | 2009-11-17 22:40:59 | 55153.9488888889 | 2009-11-18 22:46:24 | 504005010 | 40.7473 | 38 | 40.7473 | 40.7473 | 0 | 40.7473 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.5112 | 34.5112 | 86.7159 | 0 | PROCESSED | 57549.4623726852 | 2016-06-10 11:05:49 | 55534 | 2010-12-04 00:00:00 | 55166.4923148148 | 2009-12-01 11:48:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504005010/ | Quick Look | ![]() |
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1256 | W28_CENTER | 270.074 | -23.3664 | 269.312952 | -23.364911 | 270.05835 | 0.07446 | 6.46943001 | -0.00256773 | 84.9544 | 55289.3078935185 | 2010-04-03 07:23:22 | 55290.9918287037 | 2010-04-04 23:48:14 | 505005010 | 73.0036 | 70 | 73.0437 | 73.0036 | 0 | 73.0436 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 57.2981 | 57.2981 | 145.4519 | 2 | PROCESSED | 57551.1131944444 | 2016-06-12 02:43:00 | 55287 | 2010-04-01 00:00:00 | 55322.3694675926 | 2010-05-06 08:52:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505005010/ | Quick Look | ![]() |
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1257 | FERMI_BUBBLE_N7 | 234.5505 | 3.1681 | 233.922592 | 3.3308 | 231.347519 | 21.977572 | 9.28415113 | 43.5333275 | 287.4999 | 56147.9630787037 | 2012-08-08 23:06:50 | 56148.4306944444 | 2012-08-09 10:20:12 | 507007010 | 22.7991 | 20 | 22.8071 | 22.7991 | 0 | 22.8151 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0084 | 21.0084 | 40.3999 | 0 | PROCESSED | 57606.8138541667 | 2016-08-06 19:31:57 | 56536 | 2013-09-01 00:00:00 | 56169.1051388889 | 2012-08-30 02:31:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 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 | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507007010/ | Quick Look | ![]() |
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1258 | W49B | 287.7842 | 9.1154 | 287.185843 | 9.031744 | 290.654437 | 31.289753 | 43.28107632 | -0.18330097 | 82.0063 | 57125.7127893518 | 2015-04-13 17:06:25 | 57128.6891087963 | 2015-04-16 16:32:19 | 509001020 | 103.0426 | 400 | 103.0426 | 113.1875 | 0 | 113.1795 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0199537037 | 2016-08-18 00:28:44 | 56748 | 2014-04-01 00:00:00 | 57142.3645138889 | 2015-04-30 08:44:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001020/ | Quick Look | ![]() |
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1259 | HOT BLOB 3 | 127.507 | 51.0389 | 126.590865 | 51.206602 | 116.529664 | 30.99487 | 167.88407696 | 36.01101877 | 263.6154 | 57139.1338657407 | 2015-04-27 03:12:46 | 57140.9141319444 | 2015-04-28 21:56:21 | 509009010 | 81.1183 | 80 | 81.1183 | 81.5423 | 0 | 81.5503 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57644.5780902778 | 2016-09-13 13:52:27 | 57591 | 2016-07-22 00:00:00 | 57224.4589351852 | 2015-07-21 11:00:52 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090044 | Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIO SEKIYA | JAP | 9 | AO9 | ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509009010/ | Quick Look | ![]() |
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