DARTS Astro

total 337

No.
target_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
proposal_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
hxd_burst_num
processing_status
processing_end_time_mjd
processing_end_time
public_date_mjd
public_date
distribute_start_date_mjd
distribute_start_date
processing_version
processing_quantity
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle_count
observation_type
proposal_title
main_detector
xis_injection_flag
data_access_url
ql_access_url
ql_image_url
1 THE CRAB OFFSETS 83.536 22.0119 82.783772 21.978746 84.009124 -1.294644 184.51119717 -5.8617583 85.703 53984.8198263889 2006-09-06 19:40:33 53984.8891666667 2006-09-06 21:20:24 101011150 3.37 2 3.37 3.37 3.37 3.37 1 1 1 1 1 0 0 3.3472 3.3472 5.9839 0 PROCESSED 57535.4824189815 2016-05-27 11:34:41 53826 2006-04-01 00:00:00 54104.9730439815 2007-01-04 23:21:11 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011150/ Quick Look
2 E0102.2-7219 16.0278 -72.0394 15.623254 -72.307346 314.607654 -65.046746 301.54948943 -45.0548182 34.4136 53876.719525463 2006-05-21 17:16:07 53877.1793287037 2006-05-22 04:18:14 101005020 18.1619 20 18.1619 18.1939 18.1619 18.1939 2 1 2 1 1 0 0 17.7633 17.7633 39.7199 0 PROCESSED 57534.3838425926 2016-05-26 09:12:44 53826 2006-04-01 00:00:00 53926.1422222222 2006-07-10 03:24:48 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005020/ Quick Look
3 E0102.2-7219 15.9978 -72.0424 15.592857 -72.310386 314.59194 -65.039632 301.56284618 -45.05246644 92.9794 53933.2656597222 2006-07-17 06:22:33 53933.9030439815 2006-07-17 21:40:23 101005040 22.0634 20 22.0634 22.1034 22.0634 22.0954 4 2 4 2 1 0 0 20.9823 20.9823 55.0479 1 PROCESSED 57534.9613888889 2016-05-26 23:04:24 53826 2006-04-01 00:00:00 53942.4630092593 2006-07-26 11:06:44 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005040/ Quick Look
4 E0102.2-7219 15.9812 -72.0315 15.575859 -72.299509 314.610205 -65.030381 301.5690149 -45.06369281 159.2453 53997.2263425926 2006-09-19 05:25:56 53997.562662037 2006-09-19 13:30:14 101005060 10.7907 40 10.8067 10.8067 10.7907 10.7987 2 2 2 2 1 0 0 10.3223 10.3223 29.05 0 PROCESSED 57535.6263541667 2016-05-27 15:01:57 53826 2006-04-01 00:00:00 54021.1325115741 2006-10-13 03:10:49 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005060/ Quick Look
5 E0102.2-7219 15.9801 -72.0277 15.574689 -72.29571 314.618019 -65.028464 301.56912514 -45.06750714 192.8855 54029.650625 2006-10-21 15:36:54 54030.2265625 2006-10-22 05:26:15 101005070 37.1305 40 37.1705 37.1305 37.1705 37.1625 3 3 3 3 1 0 0 36.4716 36.4716 49.76 0 PROCESSED 57535.9063425926 2016-05-27 21:45:08 53826 2006-04-01 00:00:00 54055.5631828704 2006-11-16 13:30:59 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005070/ Quick Look
6 E0102.2-7219 16.0137 -72.0201 15.608673 -72.288065 314.644734 -65.034638 301.5537348 -45.07437383 265.9905 54115.1395023148 2007-01-15 03:20:53 54115.6655555556 2007-01-15 15:58:24 101005100 22.614 20 22.614 22.614 0 22.614 1 1 0 1 1 0 0 19.1496 19.1496 45.424 1 PROCESSED 57536.8323263889 2016-05-28 19:58:33 53826 2006-04-01 00:00:00 54132.8509490741 2007-02-01 20:25:22 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005100/ Quick Look
7 PKS2155-304 329.7138 -30.2259 328.989973 -30.465459 321.184272 -16.770452 17.72949775 -52.24318888 57.9013 53856.2600925926 2006-05-01 06:14:32 53857.2501041667 2006-05-02 06:00:09 101006010 38.5515 30 38.5515 38.5515 38.5515 38.5515 2 2 2 2 1 0 0 23.9476 23.9476 85.5141 2 PROCESSED 57533.6080787037 2016-05-25 14:35:38 53826 2006-04-01 00:00:00 53913.2773842593 2006-06-27 06:39:26 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101006010/ Quick Look
8 RXJ1856.5-3754 284.1489 -37.9077 283.297255 -37.973755 281.50944 -15.030994 358.6011477 -17.21474589 254.2953 54028.5128472222 2006-10-20 12:18:30 54029.6405208333 2006-10-21 15:22:21 101009010 40.7841 40 40.7841 40.7841 40.7841 40.7841 2 2 2 2 1 0 0 35.1699 35.1699 97.4039 1 PROCESSED 57535.9219675926 2016-05-27 22:07:38 53826 2006-04-01 00:00:00 54055.4732523148 2006-11-16 11:21:29 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101009010/ Quick Look
9 CRAB 83.6301 22.0172 82.877819 21.9845 84.096537 -1.293228 184.55366892 -5.78525038 85.7026 53983.2227430556 2006-09-05 05:20:45 53983.8196643518 2006-09-05 19:40:19 101010010 20.7175 20 20.8775 20.7175 20.8935 20.8855 3 2 3 3 1 0 0 19.6071 19.6071 51.5699 1 PROCESSED 57535.464224537 2016-05-27 11:08:29 53826 2006-04-01 00:00:00 54024.6695833333 2006-10-16 16:04:12 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015014 HXD cal. CALIBRATION 1 A KAZUHIRO NAKAZAWA JAP 1 AO1 CRAB CAL FOR HXD ON 2006 AUTUMN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101010010/ Quick Look
10 THE CRAB OFFSETS 83.6209 22.1323 82.867975 22.099554 84.093103 -1.177861 184.45137768 -5.73082135 85.7132 53983.8199537037 2006-09-05 19:40:44 53983.8891087963 2006-09-05 21:20:19 101011010 3.348 2 3.348 3.348 3.348 3.348 1 1 1 1 1 0 0 3.676 3.676 5.9679 0 PROCESSED 57535.4548263889 2016-05-27 10:54:57 53826 2006-04-01 00:00:00 54104.4418287037 2007-01-04 10:36:14 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011010/ Quick Look
11 THE CRAB OFFSETS 83.6254 22.076 82.87279 22.043276 84.094781 -1.234292 184.50140903 -5.75744861 85.7164 53983.951712963 2006-09-05 22:50:28 53984.0904976852 2006-09-06 02:10:19 101011030 6.703 2 6.703 6.703 6.703 6.703 1 1 1 1 1 0 0 5.4458 5.4458 11.9839 0 PROCESSED 57535.4650462963 2016-05-27 11:09:40 53826 2006-04-01 00:00:00 54104.972650463 2007-01-04 23:20:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011030/ Quick Look
12 THE CRAB OFFSETS 83.6338 21.931 82.882001 21.898319 84.09616 -1.379498 184.62870178 -5.82849289 87.5103 53996.9516550926 2006-09-18 22:50:23 53997.0140509259 2006-09-19 00:20:14 101011070 2.636 2 2.636 2.636 2.636 2.636 1 1 1 1 1 0 0 2.157 2.157 5.3839 0 PROCESSED 57535.6130092593 2016-05-27 14:42:44 53826 2006-04-01 00:00:00 54104.4160069444 2007-01-04 09:59:03 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011070/ Quick Look
13 THE CRAB OFFSETS 83.7555 22.0251 83.003144 21.993005 84.213055 -1.290417 184.60946275 -5.68280554 87.8963 53997.0840625 2006-09-19 02:01:03 53997.1529282407 2006-09-19 03:40:13 101011090 1.895 2 1.895 1.895 1.895 1.895 2 2 2 2 1 0 0 2.0815 2.0815 5.9459 0 PROCESSED 57535.6191435185 2016-05-27 14:51:34 53826 2006-04-01 00:00:00 54104.4517708333 2007-01-04 10:50:33 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011090/ Quick Look
14 THE CRAB OFFSETS 83.6927 22.0229 82.940372 21.990502 84.154781 -1.290083 184.58004352 -5.7331758 85.756 53984.5680092593 2006-09-06 13:37:56 53984.6252199074 2006-09-06 15:00:19 101011110 2.6354 2 2.6354 2.6354 2.6354 2.6354 1 1 1 1 1 0 0 2.4573 2.4573 4.942 0 PROCESSED 57535.4715046296 2016-05-27 11:18:58 53826 2006-04-01 00:00:00 54104.4321527778 2007-01-04 10:22:18 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011110/ Quick Look
15 THE CRAB OFFSETS 83.6616 22.0194 82.909299 21.986852 84.125816 -1.292316 184.56751127 -5.75940556 85.7473 53984.6253703704 2006-09-06 15:00:32 53984.6876967593 2006-09-06 16:30:17 101011120 2.9761 2 2.9761 2.9761 2.9761 2.9761 2 2 2 2 1 0 0 2.802 2.802 5.38 0 PROCESSED 57535.4738425926 2016-05-27 11:22:20 53826 2006-04-01 00:00:00 54104.4254513889 2007-01-04 10:12:39 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011120/ Quick Look
16 THE CRAB OFFSETS 83.5991 22.0137 82.846846 21.98085 84.067662 -1.295453 184.54117278 -5.81139714 85.7249 53984.6879398148 2006-09-06 16:30:38 53984.7572222222 2006-09-06 18:10:24 101011130 3.3661 2 3.3661 3.3661 3.3661 3.3661 1 1 1 1 1 0 0 3.19 3.19 5.9839 0 PROCESSED 57535.4770486111 2016-05-27 11:26:57 53826 2006-04-01 00:00:00 54104.4575 2007-01-04 10:58:48 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011130/ Quick Look
17 PERSEUS CLUSTER 49.9542 41.5047 49.126761 41.324082 58.607992 22.330697 150.58204074 -13.26559499 258.6515 54136.6651388889 2007-02-05 15:57:48 54137.6043287037 2007-02-06 14:30:14 101012020 43.8714 40 43.8954 43.8794 0 43.8714 2 2 0 2 1 0 0 41.5732 41.5732 81.1379 1 PROCESSED 57537.3356944444 2016-05-29 08:03:24 53826 2006-04-01 00:00:00 54151.6542361111 2007-02-20 15:42:06 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101012020/ Quick Look
18 JUPITER 226.5694 -16.1887 225.870685 -15.99606 228.664382 1.239883 343.96536778 35.7224308 118.4901 53790.7643402778 2006-02-24 18:20:39 53791.7940277778 2006-02-25 19:03:24 401001010 37.7594 36 37.7674 37.7594 37.7674 37.7674 2 2 2 2 1 0 0 32.8361 32.8361 88.9361 1 PROCESSED 57533.0781597222 2016-05-25 01:52:33 54401 2007-10-28 00:00:00 53905.533900463 2006-06-19 12:48:49 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C RONALD ELSNER USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001010/ Quick Look
19 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
20 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
21 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
22 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
23 HR 9024 357.4125 36.4308 356.782155 36.152799 14.165064 34.009987 109.27773456 -24.79729068 49.8624 53939.0616782407 2006-07-23 01:28:49 53940.6016087963 2006-07-24 14:26:19 401032010 58.7757 60 58.7997 58.7757 58.7837 58.7917 2 2 2 2 1 0 0 56.0116 56.0116 133.0398 1 PROCESSED 57535.042025463 2016-05-27 01:00:31 54401 2007-10-28 00:00:00 53950.2624074074 2006-08-03 06:17:52 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011022 Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. GALACTIC POINT SOURCES 4 B PAOLA TESTA USA 1 AO1 GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401032010/ Quick Look
24 BETA LYR 282.5098 33.3716 282.047998 33.312385 288.857806 55.996493 63.19266924 14.79477853 53.4974 53867.1260185185 2006-05-12 03:01:28 53867.6252199074 2006-05-12 15:00:19 401036020 21.4962 20 21.4962 21.4962 21.4962 21.4962 1 1 1 1 1 0 0 19.1642 19.1642 43.1199 2 PROCESSED 57534.2764814815 2016-05-26 06:38:08 54401 2007-10-28 00:00:00 53914.2784143518 2006-06-28 06:40:55 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011031 The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. GALACTIC POINT SOURCES 4 A RICHARD IGNACE USA 1 AO1 AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036020/ Quick Look
25 4U 1705-44 257.2295 -44.1004 256.326357 -44.0367 260.194477 -21.092135 343.32321952 -2.34240238 264.0794 53976.2429166667 2006-08-29 05:49:48 53976.7731712963 2006-08-29 18:33:22 401046010 18.3155 20 18.3155 18.3155 18.3155 18.3155 2 2 2 2 1 0 0 15.3715 15.3715 45.8099 0 PROCESSED 57535.3889236111 2016-05-27 09:20:03 54526 2008-03-01 00:00:00 54021.306087963 2006-10-13 07:20:46 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011112 We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. GALACTIC POINT SOURCES 4 A ANDREW YOUNG USA 1 AO1 REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046010/ Quick Look
26 4U 1636-536 250.2262 -53.7541 249.22979 -53.657603 256.460667 -31.236861 332.91086545 -4.81751491 91.2457 54140.3877546296 2007-02-09 09:18:22 54140.99125 2007-02-09 23:47:24 401050010 24.232 19 24.232 24.232 0 24.232 2 1 0 2 1 0 0 21.6895 21.6895 52.136 0 PROCESSED 57537.3410069445 2016-05-29 08:11:03 54525 2008-02-29 00:00:00 54151.5052893518 2007-02-20 12:07:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A JEROEN HOMAN USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050010/ Quick Look
27 IGRJ16195-4945 244.8541 -49.816 243.916706 -49.695602 251.909406 -27.940354 333.49117084 0.29973526 284.0301 53998.8508333333 2006-09-20 20:25:12 53999.7231481482 2006-09-21 17:21:20 401056010 39.1486 40 39.1486 39.1486 39.1486 39.1486 2 2 2 2 1 0 0 42.2652 42.2652 75.3579 1 PROCESSED 57535.652662037 2016-05-27 15:39:50 54526 2008-03-01 00:00:00 54020.9227199074 2006-10-12 22:08:43 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A RANDALL SMITH USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401056010/ Quick Look
28 CYGNUS X-1 299.6124 35.133 299.141904 34.996436 313.652571 54.178807 71.28577556 3.01567368 256.2202 54038.1501273148 2006-10-30 03:36:11 54038.8225 2006-10-30 19:44:24 401059010 27.7068 30 27.7068 27.7378 27.7068 27.7068 2 1 2 2 1 0 0 27.6892 27.6892 58.0839 0 PROCESSED 57535.9949768518 2016-05-27 23:52:46 54526 2008-03-01 00:00:00 54063.4924884259 2006-11-24 11:49:11 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011141 We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. GALACTIC POINT SOURCES 4 B MICHAEL NOWAK USA 1 AO1 ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401059010/ Quick Look
29 CYGNUS LOOP 314.0133 31.992 313.497685 31.799479 329.365567 46.782128 75.70987313 -8.56406979 213.2117 54090.6869791667 2006-12-21 16:29:15 54091.1175231482 2006-12-22 02:49:14 101013020 21.004 20 21.004 21.004 0 21.004 1 1 0 1 1 0 0 18.8719 18.8719 37.168 1 PROCESSED 57536.3885185185 2016-05-28 09:19:28 53826 2006-04-01 00:00:00 54132.7085763889 2007-02-01 17:00:21 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013020/ Quick Look
30 LOCKMAN HOLE 162.9366 57.2557 162.165538 57.521221 137.120397 45.113941 149.70344314 53.20093146 281.8721 53872.7389583333 2006-05-17 17:44:06 53874.7939583333 2006-05-19 19:03:18 101002010 80.3982 80 80.3982 80.4062 80.4062 80.4062 3 3 3 3 1 0 0 88.854 88.854 177.5138 4 PROCESSED 57534.3694212963 2016-05-26 08:51:58 53826 2006-04-01 00:00:00 53927.7689814815 2006-07-11 18:27:20 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015003 We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD. CALIBRATION 1 A MOTOHIDE KOKUBUN JAP 1 AO1 SUZAKU OBSERVATION OF LOCKMANHOLE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101002010/ Quick Look
31 E0102.2-7219 15.9824 -72.0369 15.577154 -72.304907 314.598987 -65.033002 301.56901677 -45.05828014 133.8232 53972.2052662037 2006-08-25 04:55:35 53973.3933333333 2006-08-26 09:26:24 101005050 68.3632 20 68.9872 68.3632 68.9872 68.9712 5 5 5 6 1 0 0 68.0024 68.0024 102.6339 1 PROCESSED 57535.3618402778 2016-05-27 08:41:03 53826 2006-04-01 00:00:00 54020.9929050926 2006-10-12 23:49:47 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005050/ Quick Look
32 E0102.2-7219 16.0273 -72.0256 15.62255 -72.293547 314.637137 -65.04077 301.54834682 -45.06859544 302.8131 54141.9262384259 2007-02-10 22:13:47 54142.812662037 2007-02-11 19:30:14 101005110 36.0938 20 36.1018 36.0938 0 36.1018 1 1 0 1 1 0 0 52.7038 52.7038 76.5759 1 PROCESSED 57537.3567592593 2016-05-29 08:33:44 53826 2006-04-01 00:00:00 54153.2227430556 2007-02-22 05:20:45 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005110/ Quick Look
33 THE CRAB OFFSETS 83.7241 22.023 82.971763 21.990753 84.183875 -1.291252 184.59560566 -5.70852703 87.5484 53997.1534490741 2006-09-19 03:40:58 53997.2154513889 2006-09-19 05:10:15 101011100 1.545 2 1.545 1.545 1.545 1.545 1 1 1 1 1 0 0 1.806 1.806 5.356 0 PROCESSED 57535.619537037 2016-05-27 14:52:08 53826 2006-04-01 00:00:00 54104.4337731482 2007-01-04 10:24:38 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011100/ Quick Look
34 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
35 GRB070328 65.0965 -34.1127 64.627027 -34.231006 53.193977 -54.420072 235.19366633 -44.98909931 291.3415 54187.3163773148 2007-03-28 07:35:35 54188.4585416667 2007-03-29 11:00:18 901005010 52.5653 40 52.5653 52.5653 0 52.5653 2 2 0 2 1 0 0 48.2428 48.2428 98.6819 2 PROCESSED 57538.0113888889 2016-05-30 00:16:24 54187 2007-03-28 00:00:00 54209.5955324074 2007-04-19 14:17:34 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 017004 TOO Observation of GRB 070328, REPORTED BY GCN 6224 EXTRAGALACTIC COMPACT SOURCES 9 A SUZAKU GRB TEAM JAP 1 TOO TOO OBSERVATION OF GRB 070328 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901005010/ Quick Look
36 A1831 209.8007 27.9693 209.233208 28.211522 195.74505 37.218341 40.05378223 74.96810077 288.1207 53937.1181828704 2006-07-21 02:50:11 53937.5106481482 2006-07-21 12:15:20 801077010 18.0796 18 18.0796 18.0796 18.0796 18.0796 2 2 2 2 1 0 0 17.0891 17.0891 33.8979 1 PROCESSED 57535.0011805556 2016-05-27 00:01:42 54401 2007-10-28 00:00:00 53943.553599537 2006-07-27 13:17:11 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B CALEB SCHARF USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/ Quick Look
37 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
38 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
39 A1800 207.3618 28.0973 206.789109 28.345144 193.256107 36.394356 40.59651819 77.12066844 302.3644 53936.635625 2006-07-20 15:15:18 53937.1140509259 2006-07-21 02:44:14 801078010 20.0437 17 20.0473 20.0553 20.0553 20.0437 2 2 2 2 1 0 0 19.0003 19.0003 41.3319 0 PROCESSED 57535.0036458333 2016-05-27 00:05:15 54401 2007-10-28 00:00:00 53943.5299652778 2006-07-27 12:43:09 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B CALEB SCHARF USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/ Quick Look
40 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
41 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
42 A2665 357.7161 6.1352 357.076736 5.857083 0.350497 6.536022 96.94047732 -53.65177278 245.9817 54078.2252893518 2006-12-09 05:24:25 54078.562037037 2006-12-09 13:29:20 801076010 13.944 15 13.944 13.944 0 13.944 2 2 0 2 1 0 0 11.6073 11.6073 29.0879 0 PROCESSED 57536.2715393518 2016-05-28 06:31:01 54695 2008-08-17 00:00:00 54089.271412037 2006-12-20 06:30:50 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B CALEB SCHARF USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/ Quick Look
43 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
44 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
45 THE CRAB OFFSETS 83.5056 22.0085 82.753398 21.975199 83.980807 -1.296775 184.49889553 -5.88737418 85.6939 53984.8892708333 2006-09-06 21:20:33 53984.935 2006-09-06 22:26:24 101011160 2.7651 2 2.7651 2.7651 2.7651 2.7651 1 1 1 1 1 0 0 2.152 2.152 3.9439 0 PROCESSED 57535.4827083333 2016-05-27 11:35:06 53826 2006-04-01 00:00:00 54104.4508449074 2007-01-04 10:49:13 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011160/ Quick Look
46 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
47 CRAB 83.6569 21.9577 82.904946 21.92513 84.118749 -1.353767 184.61755594 -5.79610428 250.9424 53830.5463425926 2006-04-05 13:06:44 53831.5925115741 2006-04-06 14:13:13 101003010 37.8323 40 37.8323 37.8533 37.8323 37.8323 1 1 1 1 1 0 0 30.989 30.989 90.3799 1 PROCESSED 57533.4323726852 2016-05-25 10:22:37 53826 2006-04-01 00:00:00 53907.1306944445 2006-06-21 03:08:12 3.0.22.43 6 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015004 Crab cal at the XIS and HXD nominal positions. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101003010/ Quick Look
48 CRAB 83.6371 22.0108 82.884853 21.978134 84.10274 -1.299909 184.56259415 -5.78319491 253.3318 53824.652650463 2006-03-30 15:39:49 53825.1668865741 2006-03-31 04:00:19 101004010 16.3632 20 16.3632 16.3728 16.365 16.365 1 1 1 1 1 0 0 9.7616 9.7616 44.426 0 PROCESSED 57533.3378009259 2016-05-25 08:06:26 53826 2006-04-01 00:00:00 53906.0621875 2006-06-20 01:29:33 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015004 Crab cal at the XIS and HXD nominal positions. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101004010/ Quick Look
49 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
50 HER X-1 254.4224 35.4083 253.972328 35.484085 245.910127 57.551397 58.22535664 37.56185232 67.8783 53823.7669907407 2006-03-29 18:24:28 53824.640462963 2006-03-30 15:22:16 101001010 33.0621 40 33.0621 38.8045 33.0621 33.0701 4 3 4 4 1 0 0 26.2228 26.2228 75.4379 0 PROCESSED 57526.8178703704 2016-05-18 19:37:44 53826 2006-04-01 00:00:00 53906.9875925926 2006-06-20 23:42:08 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015002 The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO. CALIBRATION 1 A MOTOHIDE KOKUBUN JAP 1 AO1 SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATION HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101001010/ Quick Look
51 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
52 E0102.2-7219 16.0029 -72.0223 15.597746 -72.29028 314.636668 -65.03255 301.55865958 -45.07240987 252.2709 54082.7869907407 2006-12-13 18:53:16 54083.1279976852 2006-12-14 03:04:19 101005090 28.226 20 28.226 28.226 0 28.226 1 1 0 1 1 0 0 23.0546 23.0546 29.4559 0 PROCESSED 57536.3258101852 2016-05-28 07:49:10 53826 2006-04-01 00:00:00 54094.5930324074 2006-12-25 14:13:58 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005090/ Quick Look
53 CYGNUS LOOP 314.0118 31.9912 313.496184 31.798684 329.363396 46.781909 75.70842949 -8.56360013 217.4642 54090.3953935185 2006-12-21 09:29:22 54090.6848842593 2006-12-21 16:26:14 101013010 9.102 10 9.102 9.102 0 9.102 2 2 0 2 1 0 0 9.2126 9.2126 25.006 1 PROCESSED 57536.373275463 2016-05-28 08:57:31 53826 2006-04-01 00:00:00 54108.4571990741 2007-01-08 10:58:22 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013010/ Quick Look
54 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
55 AB DOR 82.2835 -65.427 82.246883 -65.464502 16.282788 -86.671062 275.26967334 -33.00819219 154.6774 54060.0265277778 2006-11-21 00:38:12 54061.4586111111 2006-11-22 11:00:24 401031010 53.4517 80 53.4517 53.4597 0 53.4614 2 2 0 2 1 0 0 48.0334 48.0334 123.708 1 PROCESSED 57536.170462963 2016-05-28 04:05:28 54502 2008-02-06 00:00:00 54133.0222916667 2007-02-02 00:32:06 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011021 We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. GALACTIC POINT SOURCES 4 B MARC AUDARD USA 1 AO1 NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031010/ Quick Look
56 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
57 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
58 M106 184.7117 47.2376 184.094273 47.515109 160.404745 44.085185 138.43381178 68.89762168 287.1938 53896.5413078704 2006-06-10 12:59:29 53898.7113425926 2006-06-12 17:04:20 701095010 99.8175 100 99.8815 99.8175 99.8815 99.8815 2 2 2 2 1 0 0 97.5229 97.5229 187.4839 1 PROCESSED 57534.6515393518 2016-05-26 15:38:13 54401 2007-10-28 00:00:00 53927.2308449074 2006-07-11 05:32:25 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 013151 We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. EXTRAGALACTIC COMPACT SOURCES 7 A TAKESHI ITOH CHRISTOPHER REYNOLDS JUS 1 AO1 OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701095010/ Quick Look
59 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
60 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
61 CYGNUS LOOP 314.0129 31.9925 313.497288 31.79998 329.365408 46.782722 75.71004378 -8.56348961 212.8468 54091.1180439815 2006-12-22 02:49:59 54091.6036342593 2006-12-22 14:29:14 101013030 19.7295 20 19.7295 19.7295 0 19.7295 2 2 0 2 1 0 0 20.1005 20.1005 41.9279 1 PROCESSED 57536.3931134259 2016-05-28 09:26:05 53826 2006-04-01 00:00:00 54132.7375694444 2007-02-01 17:42:06 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015017 we propose observations for the XIS flight calibrations during the left term of AO-1. CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS CALIBRATIONS FOR AO1 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013030/ Quick Look
62 A2495 342.5777 10.9124 341.95313 10.647232 348.269753 16.897696 81.20126485 -41.9387619 237.1467 54061.4694097222 2006-11-22 11:15:57 54062.0787037037 2006-11-23 01:53:20 801080010 18.0313 18 18.0313 18.3673 0 18.1193 2 2 0 2 1 0 0 16.3891 16.3891 52.6339 3 PROCESSED 57536.1381365741 2016-05-28 03:18:55 54695 2008-08-17 00:00:00 54088.9563194444 2006-12-19 22:57:06 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B CALEB SCHARF USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/ Quick Look
63 E0102.2-7219 16.0331 -72.0338 15.628552 -72.301739 314.621321 -65.04586 301.54662861 -45.06029066 8.2024 53841.404212963 2006-04-16 09:42:04 53841.9793865741 2006-04-16 23:30:19 101005010 21.324 40 21.34 21.324 21.332 21.34 1 1 1 1 1 0 0 16.6831 16.6831 49.6639 0 PROCESSED 57533.4651273148 2016-05-25 11:09:47 53826 2006-04-01 00:00:00 53905.6938425926 2006-06-19 16:39:08 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005010/ Quick Look
64 E0102.2-7219 16.0373 -72.0314 15.632779 -72.299334 314.627775 -65.046019 301.54456169 -45.06259438 341.0006 54177.8828587963 2007-03-18 21:11:19 54178.2994675926 2007-03-19 07:11:14 101005120 18.242 20 18.242 18.25 0 18.258 1 1 0 1 1 0 0 14.7551 14.7551 35.9839 0 PROCESSED 57537.6970601852 2016-05-29 16:43:46 53826 2006-04-01 00:00:00 54185.4459027778 2007-03-26 10:42:06 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015007 Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks CALIBRATION 1 A HIRONORI MATSUMOTO JAP 1 AO1 XIS FLIGHT CALIBRATION PLAN XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005120/ Quick Look
65 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
66 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
67 MRK 766 184.6154 29.8184 183.986779 30.095968 171.206094 28.943476 190.63186084 82.27243688 133.2599 54055.0242361111 2006-11-16 00:34:54 54057.363900463 2006-11-18 08:44:01 701035010 97.8693 150 98.1756 97.8693 0 98.1676 2 2 0 2 1 0 0 96.8931 96.8931 202.1299 2 PROCESSED 57536.189525463 2016-05-28 04:32:55 54800 2008-11-30 00:00:00 54132.8396990741 2007-02-01 20:09:10 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011328 X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components EXTRAGALACTIC COMPACT SOURCES 7 B TRACEY TURNER USA 1 AO1 DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035010/ Quick Look
68 MRK 1 19.06 33.0289 18.361574 32.765252 30.564721 23.029207 128.90716196 -29.55492804 249.7486 54111.5318171296 2007-01-11 12:45:49 54114.5836111111 2007-01-14 14:00:24 701047010 126.4441 120 126.4441 126.4441 0 126.4441 2 2 0 2 1 0 0 126.0122 126.0122 263.6237 2 PROCESSED 57637.5831944445 2016-09-06 13:59:48 54702 2008-08-24 00:00:00 54133.1552314815 2007-02-02 03:43:32 3.0.22.44 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011336 The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators. EXTRAGALACTIC COMPACT SOURCES 7 B NANCY LEVENSON USA 1 AO1 TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701047010/ Quick Look
69 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
70 PUP A : INTERIOR 125.5916 -42.8951 125.161363 -42.733897 147.106586 -59.478577 260.333956 -3.34905821 276.8883 53842.5813541667 2006-04-17 13:57:09 53842.9127199074 2006-04-17 21:54:19 501088010 20.2709 20 20.2924 20.2949 20.2789 20.2709 1 1 1 1 1 0 0 19.9519 19.9519 28.6239 0 PROCESSED 57533.5042476852 2016-05-25 12:06:07 54401 2007-10-28 00:00:00 53906.8948611111 2006-06-20 21:28:36 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011246 We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. GALACTIC DIFFUSE EMISSION 5 A UNA HWANG USA 1 AO1 MAPPING OXYGEN IN PUPPIS A XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501088010/ Quick Look
71 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
72 Z235 10.9622 24.4059 10.298374 24.132304 19.875378 18.073678 120.72614401 -38.43334342 59.0539 53944.0060185185 2006-07-28 00:08:40 53944.6148032407 2006-07-28 14:45:19 801083010 20.0335 20 20.0415 20.0415 20.0415 20.0335 2 2 2 2 1 0 0 19.5263 19.5263 52.5899 1 PROCESSED 57535.0666782407 2016-05-27 01:36:01 54401 2007-10-28 00:00:00 53955.6800925926 2006-08-08 16:19:20 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B CALEB SCHARF USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/ Quick Look
73 GRB060904A 237.7429 44.914 237.336952 45.063372 215.38839 62.37112 71.57699476 50.22047754 264.197 53982.4478935185 2006-09-04 10:44:58 53983.2113888889 2006-09-05 05:04:24 901001010 30.3363 30 30.3443 30.3363 30.3443 30.3443 2 2 2 2 1 0 0 28.347 28.347 65.966 0 PROCESSED 57535.45125 2016-05-27 10:49:48 53982 2006-09-04 00:00:00 54026.4650462963 2006-10-18 11:09:40 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 017001 N/A EXTRAGALACTIC COMPACT SOURCES 9 A SWG GRB TEAM JAP 1 TOO TOO OBSERVATION OF GRB060904A HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901001010/ Quick Look
74 SWIFTJ1010.1-5747 152.7309 -57.8539 152.293849 -57.606865 193.450641 -60.897616 282.8705066 -1.37559689 290.7012 53891.2175 2006-06-05 05:13:12 53891.5544560185 2006-06-05 13:18:25 401055010 19.1717 20 19.1717 19.1717 19.1717 19.1717 2 2 2 2 1 0 0 17.8778 17.8778 29.0879 0 PROCESSED 57534.4906944444 2016-05-26 11:46:36 54401 2007-10-28 00:00:00 53926.1075347222 2006-07-10 02:34:51 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011132 INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. GALACTIC POINT SOURCES 4 A RANDALL SMITH USA 1 AO1 HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401055010/ Quick Look
75 JUPITER 226.5948 -16.1928 225.896045 -16.000249 228.688969 1.24261 343.98613419 35.70433361 118.4906 53791.7941319445 2006-02-25 19:03:33 53792.7940277778 2006-02-26 19:03:24 401001020 37.704 36 37.704 37.704 37.704 37.704 1 1 1 1 1 0 0 32.7781 32.7781 86.36 1 PROCESSED 57533.0943981482 2016-05-25 02:15:56 54401 2007-10-28 00:00:00 53905.5035416667 2006-06-19 12:05:06 3.0.22.43 6 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011003 We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. GALACTIC POINT SOURCES 4 C RONALD ELSNER USA 1 AO1 JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001020/ Quick Look
76 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
77 SIGMA^2 CRB 243.6552 33.7881 243.181435 33.91264 231.394365 53.752123 54.56402364 46.14689859 281.1207 53969.4764467593 2006-08-22 11:26:05 53972.1925231482 2006-08-25 04:37:14 401034010 109.1604 110 109.1904 109.1604 109.1684 109.1764 2 2 2 2 1 0 0 98.8376 98.8376 234.6539 3 PROCESSED 57535.3877777778 2016-05-27 09:18:24 54526 2008-03-01 00:00:00 54021.2578587963 2006-10-13 06:11:19 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011025 Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD. GALACTIC POINT SOURCES 4 B ALEXANDER BROWN USA 1 AO1 SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401034010/ Quick Look
78 4U 1820-30 275.9207 -30.3623 275.117497 -30.389079 275.135384 -7.027059 2.78792233 -7.91550172 265.9754 53992.9234606482 2006-09-14 22:09:47 53993.6605902778 2006-09-15 15:51:15 401047010 25.7008 37 25.7008 25.8109 25.7239 25.7148 2 1 2 2 1 0 0 31.8782 31.8782 63.6339 1 PROCESSED 57535.6012962963 2016-05-27 14:25:52 54526 2008-03-01 00:00:00 54021.2227083333 2006-10-13 05:20:42 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011113 The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. GALACTIC POINT SOURCES 4 B JON MILLER USA 1 AO1 A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401047010/ Quick Look
79 4U 1636-536 250.2259 -53.7533 249.229501 -53.656802 256.460315 -31.236099 332.911352 -4.8168543 100.7755 54188.4720717593 2007-03-29 11:19:47 54188.7856944445 2007-03-29 18:51:24 401050050 12.2418 38 12.2498 12.2418 0 12.2498 2 1 0 2 1 0 0 11.804 11.804 27.088 0 PROCESSED 57537.9973148148 2016-05-29 23:56:08 54695 2008-08-17 00:00:00 54200.4687731482 2007-04-10 11:15:02 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011117 Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. GALACTIC POINT SOURCES 4 A JEROEN HOMAN USA 1 AO1 THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050050/ Quick Look
80 4U1907+09 287.4013 9.8378 286.806482 9.755913 290.334973 32.058259 43.74739314 0.48531727 60.2599 53857.2580324074 2006-05-02 06:11:34 53858.7322222222 2006-05-03 17:34:24 401057010 58.4403 60 58.4403 58.4563 58.4483 58.4563 2 2 2 2 1 0 0 38.8215 38.8215 127.3539 1 PROCESSED 57533.6690509259 2016-05-25 16:03:26 54401 2007-10-28 00:00:00 53913.4367476852 2006-06-27 10:28:55 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011133 We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''. GALACTIC POINT SOURCES 4 A KATJA POTTSCHMIDT USA 1 AO1 THE BROAD BAND SPECTRUM OF 4U1907+09 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401057010/ Quick Look
81 HESS J1731-347 263.0179 -34.7706 262.185573 -34.73474 264.142481 -11.47104 353.53173388 -0.68198005 79.8005 54154.7807060185 2007-02-23 18:44:13 54155.7432291667 2007-02-24 17:50:15 401099010 40.6189 38 40.6269 40.6189 0 40.6269 2 2 0 2 1 0 0 34.6479 34.6479 83.1559 0 PROCESSED 57537.4739351852 2016-05-29 11:22:28 54528 2008-03-03 00:00:00 54160.3931944444 2007-03-01 09:26:12 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012042 The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator. GALACTIC POINT SOURCES 4 A GERD PUEHLHOFER EUR 1 AO1 THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401099010/ Quick Look
82 A2572B 349.6066 18.7294 348.98329 18.45586 358.210513 21.259827 94.21850787 -38.90117923 59.1565 53922.7742939815 2006-07-06 18:34:59 53923.3002199074 2006-07-07 07:12:19 801073010 24.0595 21 24.0755 24.0595 24.0675 24.0755 2 2 2 2 1 0 0 21.4951 21.4951 45.3979 1 PROCESSED 57534.8583912037 2016-05-26 20:36:05 54401 2007-10-28 00:00:00 53930.6043055556 2006-07-14 14:30:12 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011422 We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. EXTRAGALACTIC DIFFUSE SOURCES 8 B CALEB SCHARF USA 1 AO1 A ZERO-REDSHIFT GALAXY CLUSTER BASELINE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/ Quick Look
83 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
84 THE CRAB OFFSETS 83.6274 22.0499 82.874936 22.017186 84.09548 -1.260449 184.52456216 -5.76985767 85.719 53984.0906018518 2006-09-06 02:10:28 53984.1529976852 2006-09-06 03:40:19 101011040 3.353 2 3.353 3.353 3.353 3.353 1 1 1 1 1 0 0 2.414 2.414 5.3839 0 PROCESSED 57535.4661921296 2016-05-27 11:11:19 53826 2006-04-01 00:00:00 54104.4143518518 2007-01-04 09:56:40 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011040/ Quick Look
85 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
86 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
87 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
88 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
89 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
90 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
91 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
92 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
93 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
94 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
95 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
96 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
97 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
98 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
99 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
100 G156.2+5.7NW 74.223 52.4174 73.2357 52.339427 79.010107 29.577951 155.48379099 5.80912082 273.883 54147.6530902778 2007-02-16 15:40:27 54148.7558333333 2007-02-17 18:08:24 501075010 50.5468 50 50.5468 50.5468 0 50.5468 2 2 0 2 1 0 0 46.1958 46.1958 95.2599 0 PROCESSED 57537.3885763889 2016-05-29 09:19:33 54695 2008-08-17 00:00:00 54153.2775 2007-02-22 06:39:36 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011235 G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. GALACTIC DIFFUSE EMISSION 5 C ROBERT PETRE USA 1 AO1 A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501075010/ Quick Look
101 SNR G93.3+6.9 CENTER 312.9805 55.373 312.634427 55.183848 352.046818 66.979241 93.25121789 6.97467523 40.9208 53905.2215509259 2006-06-19 05:19:02 53905.6480787037 2006-06-19 15:33:14 501079010 20.5372 20 20.5452 20.5452 20.5452 20.5372 2 2 2 2 1 0 0 20.008 20.008 36.8159 0 PROCESSED 57534.7200347222 2016-05-26 17:16:51 54401 2007-10-28 00:00:00 53926.792962963 2006-07-10 19:01:52 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B Q. DANIEL WANG USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501079010/ Quick Look
102 SNR G93.3+6.9 S1 313.1088 55.5284 312.76382 55.338789 352.457306 67.040407 93.41888838 7.01647125 40.6424 53905.6486458333 2006-06-19 15:34:03 53905.9696064815 2006-06-19 23:16:14 501080010 15.875 15 15.875 15.8902 15.891 15.883 1 1 1 1 1 0 0 12.7588 12.7588 27.7279 1 PROCESSED 57534.7111805556 2016-05-26 17:04:06 54401 2007-10-28 00:00:00 53926.199212963 2006-07-10 04:46:52 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B Q. DANIEL WANG USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501080010/ Quick Look
103 SNR G93.3+6.9 S4 312.7524 55.2472 312.406034 55.058863 351.58456 66.978212 93.07038921 6.99620044 39.4008 53906.7271296296 2006-06-20 17:27:04 53907.0550347222 2006-06-21 01:19:15 501083010 15.3662 15 15.3662 15.3662 15.3662 15.3662 2 2 2 2 1 0 0 14.4694 14.4694 28.3279 1 PROCESSED 57534.7341550926 2016-05-26 17:37:11 54401 2007-10-28 00:00:00 53926.117662037 2006-07-10 02:49:26 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 011242 The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. GALACTIC DIFFUSE EMISSION 5 B Q. DANIEL WANG USA 1 AO1 G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501083010/ Quick Look
104 HESS J1718-385 259.5512 -38.6075 258.69231 -38.554942 261.534502 -15.472357 348.79652534 -0.53531102 91.2393 54154.3587731482 2007-02-23 08:36:38 54154.7773611111 2007-02-23 18:39:24 501105010 20.744 19 20.744 20.744 0 20.744 1 1 0 1 1 0 0 15.8365 15.8365 36.1519 0 PROCESSED 57537.4491435185 2016-05-29 10:46:46 54527 2008-03-02 00:00:00 54158.2865740741 2007-02-27 06:52:40 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 012044 HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons. GALACTIC DIFFUSE EMISSION 5 A JAMES HINTON EUR 1 AO1 PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501105010/ Quick Look
105 G156.2+5.7 CENTER 74.723 51.7342 73.743251 51.658579 79.264036 28.862327 156.21466687 5.62934315 273.4473 54148.7568171296 2007-02-17 18:09:49 54149.9169444444 2007-02-18 22:00:24 501106010 51.2142 50 51.2222 51.2302 0 51.2142 1 1 0 1 1 0 0 46.482 46.482 100.1999 0 PROCESSED 57537.3992824074 2016-05-29 09:34:58 54695 2008-08-17 00:00:00 54158.4264351852 2007-02-27 10:14:04 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 013079 Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR. GALACTIC DIFFUSE EMISSION 5 B MASARU UENO ROBERT PETRE JUS 1 AO1 REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501106010/ Quick Look
106 VELA X (REGION A) 128.7666 -45.458 128.346603 -45.284447 153.579861 -60.62666 263.74862198 -2.99483781 337.7597 53927.7846990741 2006-07-11 18:49:58 53929.4703819444 2006-07-13 11:17:21 501107010 60.7735 60 60.7735 60.7735 60.7735 60.7735 2 2 2 2 1 0 0 54.1611 54.1611 145.6058 3 PROCESSED 57534.9641203704 2016-05-26 23:08:20 54401 2007-10-28 00:00:00 53942.4562037037 2006-07-26 10:56:56 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B OLEG KARGALTSEV KOJI MORI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501107010/ Quick Look
107 VELA X (REGION C) 127.7806 -46.2716 127.370041 -46.101802 153.218075 -61.676794 263.99736145 -4.03006469 349.189 53933.9133796296 2006-07-17 21:55:16 53934.7730787037 2006-07-18 18:33:14 501108010 29.2028 30 29.2028 29.2028 29.2028 29.2028 2 2 2 2 1 0 0 25.5929 25.5929 74.248 1 PROCESSED 57534.9868055556 2016-05-26 23:41:00 54404 2007-10-31 00:00:00 53943.4988773148 2006-07-27 11:58:23 3.0.22.43 7 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 014211 The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. GALACTIC DIFFUSE EMISSION 5 B OLEG KARGALTSEV KOJI MORI USJ 1 AO1 THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501108010/ Quick Look
108 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
109 THE CRAB OFFSETS 83.6343 21.9041 82.882652 21.871421 84.095437 -1.406393 184.65179297 -5.84249768 87.5094 53997.0141550926 2006-09-19 00:20:23 53997.0834953704 2006-09-19 02:00:14 101011080 2.251 2 2.251 2.251 2.251 2.251 1 1 1 1 1 0 0 2.275 2.275 5.9839 1 PROCESSED 57535.6182407407 2016-05-27 14:50:16 53826 2006-04-01 00:00:00 54104.4469675926 2007-01-04 10:43:38 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 015015 We propose observing multiple offset pointings of the Crab nebula. CALIBRATION 1 A YOSHITOMO MAEDA JAP 1 AO1 CRAB OFFSET POINTINGS SPE N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011080/ Quick Look
110 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