DARTS Astro

total 1259

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 Crab Nebula 83.6449 22.0152 82.892626 21.982571 84.11016 -1.295832 184.56274906 -5.77473152 84.9987 53614.1083449074 2005-09-01 02:36:01 53614.1771759259 2005-09-01 04:15:08 100015030 2.1 5 2.1 2.1 2.1 2.1 1 1 1 1 1 0 0 2.3074 2.3074 5.9439 0 PROCESSED 57527.235150463 2016-05-19 05:38:37 54247 2007-05-27 00:00:00 54109.3966782407 2007-01-09 09:31:13 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000015 CALIBRATION 1 A SWG JAP 0 SWG HXD boresight check with Crab N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015030/
2 E0102-72 15.9884 -72.0403 15.58329 -72.308299 314.593543 -65.036118 301.56673438 -45.05476105 119.5512 53595.2489236111 2005-08-13 05:58:27 53595.4618518518 2005-08-13 11:05:04 100001020 4.1598 10 4.1598 4.1598 4.1598 4.1598 1 1 1 2 0 0 0 0 0 0 0 PROCESSED 57520.6779861111 2016-05-12 16:16:18 54247 2007-05-27 00:00:00 54035.6312731482 2006-10-27 15:09:02 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000001 XIS door open with a SMC SNR E0102-72 CALIBRATION 1 A SWG JAP 0 SWG XIS door open N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100001020/ Quick Look
3 N132D 81.2751 -69.6506 81.377584 -69.69262 312.405312 -85.522517 280.31335191 -32.77744994 53.3312 53598.2402777778 2005-08-16 05:46:00 53598.5140046296 2005-08-16 12:20:10 100002060 5.9635 7 5.9635 5.9635 5.9635 5.9635 1 1 1 1 0 0 0 0 0 0 0 PROCESSED 57520.6925115741 2016-05-12 16:37:13 54247 2007-05-27 00:00:00 54038.4700810185 2006-10-30 11:16:55 3.0.22.43 6 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG JAP 0 SWG HXD HV ON WITH N132D N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002060/ Quick Look
4 DEM_L71/N23 76.4474 -67.958 76.476582 -68.023213 338.826937 -84.59461 278.75859594 -34.83581885 70.5849 53598.5206365741 2005-08-16 12:29:43 53599.6042592593 2005-08-17 14:30:08 100003010 5.7897 40 5.7897 5.7897 5.7897 5.7897 2 2 2 2 0 0 0 0 0 93.6061 0 PROCESSED 57520.7098611111 2016-05-12 17:02:12 54247 2007-05-27 00:00:00 54035.7018171296 2006-10-27 16:50:37 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000003 LMC SNRs L71/N23 CALIBRATION 1 A SWG JAP 0 SWG LMC SNRs N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100003010/ Quick Look
5 A 2052 229.2779 6.8766 228.662841 7.059342 224.77082 24.150691 9.31339919 49.96215441 281.2328 53602.4238078704 2005-08-20 10:10:17 53602.743287037 2005-08-20 17:50:20 100006010 13.9021 20 13.9021 13.9021 13.9021 13.9021 1 1 1 1 1 0 0 13.4163 13.4163 27.5839 0 PROCESSED 57520.7207407407 2016-05-12 17:17:52 53705 2005-12-01 00:00:00 53905.4607523148 2006-06-19 11:03:29 3.0.22.43 11 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000006 CALIBRATION 1 A SWG JAP 0 SWG Outer region of A 2052 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006010/ Quick Look
6 A 2052 229.3237 7.1059 228.709513 7.288472 224.747048 24.38343 9.64711471 50.05514889 281.2373 53602.7440393518 2005-08-20 17:51:25 53603.3406944445 2005-08-21 08:10:36 100006020 25.7431 20 25.7431 25.7431 25.7431 25.7431 1 1 1 1 1 0 0 21.0642 21.0642 51.5199 0 PROCESSED 57520.7246527778 2016-05-12 17:23:30 53705 2005-12-01 00:00:00 53905.4610300926 2006-06-19 11:03:53 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000006 CALIBRATION 1 A SWG JAP 0 SWG Outer region of A 2052 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006020/ Quick Look
7 A 2052 229.0933 7.1516 228.479191 7.335016 224.492199 24.361996 9.50335527 50.26933049 281.2093 53603.3412615741 2005-08-21 08:11:25 53603.6114351852 2005-08-21 14:40:28 100006030 12.969 20 12.969 12.969 12.969 12.969 1 1 1 1 1 0 0 13.1413 13.1413 23.3279 0 PROCESSED 57520.7271527778 2016-05-12 17:27:06 53705 2005-12-01 00:00:00 53905.4613310185 2006-06-19 11:04:19 3.0.22.43 9 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000006 CALIBRATION 1 A SWG JAP 0 SWG Outer region of A 2052 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006030/ Quick Look
8 A 2052 229.3311 7.2632 228.717502 7.445744 224.705557 24.536292 9.85579143 50.13807877 91.2371 53762.482650463 2006-01-27 11:35:01 53762.9209953704 2006-01-27 22:06:14 100006050 22.366 20 22.366 22.366 22.366 22.366 2 2 2 2 1 0 0 20.388 20.388 37.8659 0 PROCESSED 57532.800162037 2016-05-24 19:12:14 54247 2007-05-27 00:00:00 54040.5318634259 2006-11-01 12:45:53 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000006 CALIBRATION 1 A SWG JAP 0 SWG Outer region of A 2052 XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100006050/ Quick Look
9 NGC 4945 196.3681 -49.4152 195.638243 -49.147517 216.98939 -38.593586 305.27752827 13.39262005 96.1296 53750.3365625 2006-01-15 08:04:39 53752.9655092593 2006-01-17 23:10:20 100008030 95.0663 10 95.0817 95.1297 95.0663 95.1063 2 2 2 2 1 0 0 84.9813 84.9813 227.1157 2 PROCESSED 57532.7353240741 2016-05-24 17:38:52 54247 2007-05-27 00:00:00 54040.3587615741 2006-11-01 08:36:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000008 CALIBRATION 1 A SWG JAP 0 SWG NGC 4945 HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100008030/ Quick Look
10 PSR1509-58 228.4798 -59.0943 227.494741 -58.907902 243.862404 -39.360151 320.34145971 -1.12587132 287.6342 53605.36 2005-08-23 08:38:24 53606.8597569444 2005-08-24 20:38:03 100009010 65.1618 60 65.1618 65.3227 65.2427 65.2427 3 3 3 3 1 0 0 49.7357 49.7357 129.5298 4 PROCESSED 57526.9045486111 2016-05-18 21:42:33 53705 2005-12-01 00:00:00 53905.4622337963 2006-06-19 11:05:37 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000009 HXD spectrum and timing check CALIBRATION 1 A SWG JAP 0 SWG PSR1509-58 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100009010/ Quick Look
11 Crab Nebula 83.6267 22.0751 82.874095 22.042383 84.095945 -1.235244 184.50282132 -5.75691305 86.8655 53607.0070833333 2005-08-25 00:10:12 53607.1389814815 2005-08-25 03:20:08 100010010 2.9379 5 2.9379 2.9379 2.9379 2.9379 2 2 2 2 1 0 0 3.4387 3.4387 11.3819 0 PROCESSED 57526.8678703704 2016-05-18 20:49:44 54247 2007-05-27 00:00:00 54118.9886689815 2007-01-18 23:43:41 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010010/ Quick Look
12 Crab nebula 83.6336 21.9568 82.881657 21.924117 84.097114 -1.353715 184.60669551 -5.81484075 86.8687 53607.1394560185 2005-08-25 03:20:49 53607.2779282407 2005-08-25 06:40:13 100010020 3.6533 5 3.6533 3.6533 3.6533 3.6533 1 1 1 1 1 0 0 3.8067 3.8067 11.934 0 PROCESSED 57526.8772337963 2016-05-18 21:03:13 54247 2007-05-27 00:00:00 54118.9337615741 2007-01-18 22:24:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010020/ Quick Look
13 Crab nebula 83.6511 21.6763 82.900722 21.643705 84.100986 -1.634666 184.85366771 -5.95118505 86.8795 53607.5153125 2005-08-25 12:22:03 53607.7153472222 2005-08-25 17:10:06 100010040 9.5806 5 9.5806 9.5806 9.5806 9.5806 1 1 1 1 1 0 0 8.1783 8.1783 17.248 0 PROCESSED 57526.8981828704 2016-05-18 21:33:23 54247 2007-05-27 00:00:00 54118.943125 2007-01-18 22:38:06 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010040/ Quick Look
14 Crab nebula 83.5677 22.0135 82.815455 21.980499 84.038563 -1.294359 184.52566905 -5.83608695 86.8444 53607.9175810185 2005-08-25 22:01:19 53608.0695023148 2005-08-26 01:40:05 100010060 4.8779 5 4.8779 4.8779 4.8779 4.8779 1 1 1 1 1 0 0 5.0217 5.0217 13.076 0 PROCESSED 57526.9066087963 2016-05-18 21:45:31 54247 2007-05-27 00:00:00 54122.4195486111 2007-01-22 10:04:09 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010060/ Quick Look
15 Crab nebula 83.6922 22.0221 82.939876 21.989699 84.154283 -1.290862 184.58047361 -5.73399538 86.8671 53608.0699768518 2005-08-26 01:40:46 53608.2084027778 2005-08-26 05:00:06 100010070 4.0899 5 4.0899 4.0899 4.0899 4.0899 1 1 1 1 1 0 0 4.2283 4.2283 11.9259 0 PROCESSED 57526.9072222222 2016-05-18 21:46:24 54247 2007-05-27 00:00:00 54119.0149074074 2007-01-19 00:21:28 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010070/ Quick Look
16 Crab nebula 83.5807 22.8483 82.82374 22.81535 84.087744 -0.460898 183.82410841 -5.37832099 86.8677 53608.3175810185 2005-08-26 07:37:19 53608.5139583333 2005-08-26 12:20:06 100010090 6.716 5 6.716 6.716 6.716 6.716 1 1 1 1 1 0 0 6.3768 6.3768 16.9501 0 PROCESSED 57526.9164699074 2016-05-18 21:59:43 54247 2007-05-27 00:00:00 54119.0235648148 2007-01-19 00:33:56 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010090/ Quick Look
17 Crab nebula 83.5122 24.0135 82.748583 23.980205 84.077056 0.70598 182.80375415 -4.80497322 86.8675 53608.7179976852 2005-08-26 17:13:55 53608.930625 2005-08-26 22:20:06 100010110 9.4805 5 9.4805 9.4805 9.4805 9.4805 1 1 1 1 1 0 0 7.363 7.363 18.336 0 PROCESSED 57526.9265162037 2016-05-18 22:14:11 54247 2007-05-27 00:00:00 54118.98625 2007-01-18 23:40:12 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010110/ Quick Look
18 Crab nebula 83.6374 21.9009 82.885769 21.868236 84.09817 -1.409717 184.65605757 -5.84178049 86.8664 53608.9333217593 2005-08-26 22:23:59 53609.069525463 2005-08-27 01:40:07 100010120 4.7456 5 4.7456 4.7456 4.7456 4.7456 2 2 2 2 1 0 0 5.1787 5.1787 11.7579 1 PROCESSED 57526.9343287037 2016-05-18 22:25:26 54247 2007-05-27 00:00:00 54118.9946180556 2007-01-18 23:52:15 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010120/ Quick Look
19 Crab nebula 83.5044 22.0116 82.752181 21.978293 83.979835 -1.293628 184.49566519 -5.88665136 86.8658 53609.0701388889 2005-08-27 01:41:00 53609.2014583333 2005-08-27 04:50:06 100010130 4.222 5 4.222 4.222 4.222 4.222 1 1 1 1 1 0 0 4.3724 4.3724 11.3359 0 PROCESSED 57526.9346180556 2016-05-18 22:25:51 54247 2007-05-27 00:00:00 54119.0454282407 2007-01-19 01:05:25 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010130/ Quick Look
20 Galactic bulge 236.4313 -31.7013 235.648361 -31.545749 241.296308 -11.543137 340.99994533 17.99808229 283.5446 53609.4365856482 2005-08-27 10:28:41 53611.060625 2005-08-29 01:27:18 100011010 61.133 70 61.133 61.133 61.133 61.133 1 1 1 1 1 0 0 47.9834 47.9834 140.282 2 PROCESSED 57526.962037037 2016-05-18 23:05:20 54247 2007-05-27 00:00:00 54034.8288310185 2006-10-26 19:53:31 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000011 CALIBRATION 1 A SWG JAP 0 SWG Galactic bulge N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100011010/ Quick Look
21 Eta Carinae 161.281 -59.6845 160.794333 -59.421136 202.162077 -58.916082 287.6040589 -0.62575348 343.8621 53611.0750347222 2005-08-29 01:48:03 53612.0627546296 2005-08-30 01:30:22 100012010 49.782 40 49.79 49.782 49.782 49.798 2 2 2 2 1 0 0 55.9607 55.9607 85.2529 0 PROCESSED 57526.9773032407 2016-05-18 23:27:19 53705 2005-12-01 00:00:00 53905.4648842593 2006-06-19 11:09:26 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000012 CALIBRATION 1 A SWG JAP 0 SWG Eta Carinae N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100012010/ Quick Look
22 N103B 77.2315 -68.7507 77.290508 -68.812132 329.838884 -84.691105 279.61119012 -34.36730962 73.8586 53612.0740162037 2005-08-30 01:46:35 53613.0626273148 2005-08-31 01:30:11 100013010 33.0646 40 33.0646 33.0646 33.0646 33.0646 2 2 2 2 1 0 0 37.2814 37.2814 85.4059 1 PROCESSED 57526.9730324074 2016-05-18 23:21:10 54247 2007-05-27 00:00:00 54034.8733449074 2006-10-26 20:57:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000013 CALIBRATION 1 A SWG JAP 0 SWG N103B N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100013010/ Quick Look
23 E0102-72 15.9813 -72.0378 15.57605 -72.305808 314.596715 -65.033076 301.56958331 -45.05740554 140.1798 53613.0710648148 2005-08-31 01:42:20 53613.7640509259 2005-08-31 18:20:14 100014010 24.3339 20 24.3339 24.3339 24.3339 24.3339 2 2 2 2 1 0 0 24.5144 24.5144 59.8639 2 PROCESSED 57511.5174884259 2016-05-03 12:25:11 53705 2005-12-01 00:00:00 53905.4615740741 2006-06-19 11:04:40 3.0.22.43 13 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000014 CALIBRATION 1 A SWG JAP 0 SWG XIS monitor with E0102-72 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100014010/ Quick Look
24 Crab Nebula 83.6296 22.1792 82.876409 22.146495 84.103227 -1.131361 184.41590928 -5.69889955 84.9998 53613.9762152778 2005-08-31 23:25:45 53614.1077314815 2005-09-01 02:35:08 100015020 4.95 5 4.95 4.95 4.95 4.95 1 1 1 1 1 0 0 5.1178 5.1178 11.3599 0 PROCESSED 57527.2276388889 2016-05-19 05:27:48 54247 2007-05-27 00:00:00 54109.1090972222 2007-01-09 02:37:06 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000015 CALIBRATION 1 A SWG JAP 0 SWG HXD boresight check with Crab N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015020/ Quick Look
25 SN1006 SW BG 224.655 -42.4005 223.837497 -42.201017 234.783022 -24.341132 326.632731 14.54333558 310.4886 53624.9999189815 2005-09-11 23:59:53 53626.0071643518 2005-09-13 00:10:19 100019040 32.3334 50 32.3334 32.3494 32.3414 32.3414 2 2 2 2 1 0 0 24.6736 24.6736 87.0159 5 PROCESSED 57527.3647453704 2016-05-19 08:45:14 54247 2007-05-27 00:00:00 54035.4482638889 2006-10-27 10:45:30 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000019 CALIBRATION 1 A SWG JAP 0 SWG SN1006 observation with XIS and HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019040/ Quick Look
26 SN1006 SW BG 224.6468 -42.4025 223.829311 -42.202989 234.777387 -24.344913 326.62625739 14.54451897 100.3489 53761.7199652778 2006-01-26 17:16:45 53762.4752777778 2006-01-27 11:24:24 100019060 27.9813 50 27.9813 27.9893 27.9973 27.9973 2 2 2 2 1 0 0 29.5504 29.5504 65.2499 2 PROCESSED 57532.7989814815 2016-05-24 19:10:32 54247 2007-05-27 00:00:00 54040.5663541667 2006-11-01 13:35:33 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000019 CALIBRATION 1 A SWG JAP 0 SWG SN1006 observation with XIS and HXD XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019060/ Quick Look
27 Fornax Cluster 54.6395 -35.4918 54.160816 -35.653913 38.755932 -52.830853 236.7850293 -53.61976834 103.5002 53626.0756018518 2005-09-13 01:48:52 53627.5002662037 2005-09-14 12:00:23 100020010 76.0782 100 76.0782 76.0782 76.0782 76.0782 2 2 2 2 1 0 0 71.1128 71.1128 123.0639 3 PROCESSED 57527.3377430556 2016-05-19 08:06:21 54247 2007-05-27 00:00:00 54035.4442013889 2006-10-27 10:39:39 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000020 CALIBRATION 1 A SWG JAP 0 SWG Fornax Cluster N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100020010/ Quick Look
28 Crab Nebula 82.7325 21.9883 81.980613 21.951274 83.263643 -1.282782 184.12771921 -6.50224239 88.0978 53628.3006828704 2005-09-15 07:12:59 53628.5835416667 2005-09-15 14:00:18 100022020 10.9198 10 10.9198 10.9198 10.9198 10.9198 1 1 1 1 1 0 0 6.3401 6.3401 24.4 2 PROCESSED 57527.3262615741 2016-05-19 07:49:49 54247 2007-05-27 00:00:00 54109.1486342593 2007-01-09 03:34:02 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000022 Crab at 50arcmin off from the XIS aimpoint to study stray light. CALIBRATION 1 A SWG JAP 0 SWG Crab at 50 arcmin off N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022020/ Quick Look
29 Crab Nebula 84.5289 22.0469 83.776247 22.018539 84.930453 -1.297747 184.974122 -5.06424795 87.5879 53629.0921759259 2005-09-16 02:12:44 53629.368275463 2005-09-16 08:50:19 100022030 12.8244 10 12.8404 12.8324 12.8244 12.8484 2 2 2 2 1 0 0 10.3518 10.3518 23.824 1 PROCESSED 57527.3478009259 2016-05-19 08:20:50 54247 2007-05-27 00:00:00 54109.1621527778 2007-01-09 03:53:30 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000022 Crab at 50arcmin off from the XIS aimpoint to study stray light. CALIBRATION 1 A SWG JAP 0 SWG Crab at 50 arcmin off N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100022030/ Quick Look
30 Crab Nebula 83.6282 22.0761 82.875589 22.04339 84.097378 -1.234306 184.5027205 -5.75520363 87.79 53628.5852199074 2005-09-15 14:02:43 53628.8265393518 2005-09-15 19:50:13 100023010 11.9978 10 11.9978 11.9978 11.9978 11.9978 1 1 1 1 1 0 0 10.5132 10.5132 20.8239 0 PROCESSED 57527.3355902778 2016-05-19 08:03:15 54247 2007-05-27 00:00:00 54109.2268287037 2007-01-09 05:26:38 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000023 Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths. CALIBRATION 1 A SWG JAP 0 SWG Crab at nominal positions N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100023010/ Quick Look
31 BD +30 3639 293.6887 30.5051 293.198078 30.394341 303.540216 51.224252 64.77556877 5.01383279 277.8713 53634.3814930556 2005-09-21 09:09:21 53635.2473842593 2005-09-22 05:56:14 100025010 35.2146 40 35.2306 35.2306 35.2146 35.2226 2 2 2 2 1 0 0 33.3728 33.3728 74.8039 1 PROCESSED 57527.3931597222 2016-05-19 09:26:09 54247 2007-05-27 00:00:00 54035.4664583333 2006-10-27 11:11:42 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000025 The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time. CALIBRATION 1 A SWG JAP 0 SWG Observation of planetary nebula BD +30 3639 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100025010/ Quick Look
32 RXJ1713-3946-BKGD2 257.2742 -41.0338 256.397744 -40.970376 259.926088 -18.035902 345.80577047 -0.54060643 270.0033 53641.2980671296 2005-09-28 07:09:13 53642.1843055556 2005-09-29 04:25:24 100026030 37.5132 40 37.5372 37.5292 37.5132 37.5132 2 2 2 2 1 0 0 31.8982 31.8982 76.5659 0 PROCESSED 57527.4461574074 2016-05-19 10:42:28 54247 2007-05-27 00:00:00 54035.6187268518 2006-10-27 14:50:58 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000026 RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. CALIBRATION 1 A SWG JAP 0 SWG Observation of RXJ1713.7-3946 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100026030/ Quick Look
33 M82-Wind 148.8893 69.7655 147.850184 70.002482 118.869306 52.161633 141.33880284 40.49464345 137.7608 53647.5072800926 2005-10-04 12:10:29 53648.1418287037 2005-10-05 03:24:14 100033010 32.3274 100 32.3274 32.3274 32.3274 32.3274 2 2 2 2 1 0 0 30.2224 30.2224 54.8021 0 PROCESSED 57527.5155092593 2016-05-19 12:22:20 54247 2007-05-27 00:00:00 54037.0057175926 2006-10-29 00:08:14 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000033 We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. CALIBRATION 1 A SWG JAP 0 SWG Largely Extended Emission (~12kpc) around M82 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033010/ Quick Look
34 Sgr_A_west 266.3057 -29.1697 265.509983 -29.149828 266.748763 -5.770252 359.75546849 -0.04768885 264.9601 53637.5953356482 2005-09-24 14:17:17 53638.7273032407 2005-09-25 17:27:19 100027020 42.8148 50 42.8148 42.8148 42.8148 42.8148 2 2 2 2 1 0 0 36.091 36.091 97.8 0 PROCESSED 57527.4293865741 2016-05-19 10:18:19 54247 2007-05-27 00:00:00 54035.5135532407 2006-10-27 12:19:31 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG JAP 0 SWG Suzaku Observation of Galactic Center Region N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027020/ Quick Look
35 E0102-72 16.139 -72.1205 15.73725 -72.388297 314.467235 -65.111919 301.50933431 -44.97149935 119.4064 53593.3086458333 2005-08-11 07:24:27 53595.2485069444 2005-08-13 05:57:51 100001010 2.4068 70 2.4068 2.4068 2.4068 2.4068 1 1 1 1 0 0 0 0 0 0 0 PROCESSED 57520.6843287037 2016-05-12 16:25:26 54247 2007-05-27 00:00:00 54035.5925115741 2006-10-27 14:13:13 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000001 XIS door open with a SMC SNR E0102-72 CALIBRATION 1 A SWG JAP 0 SWG XIS door open N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100001010/ Quick Look
36 1E1743.1-2843(GC_BGD_3) 266.592 -28.6516 265.799503 -28.633124 266.987582 -5.246121 0.32828705 0.00813221 264.88 53638.7286111111 2005-09-25 17:29:12 53638.793275463 2005-09-25 19:02:19 100027050 1.9846 5 1.9846 1.9846 1.9846 1.9846 1 1 1 1 1 0 0 1.7934 1.7934 5.5679 0 PROCESSED 57527.4093055556 2016-05-19 09:49:24 54247 2007-05-27 00:00:00 53905.6343055556 2006-06-19 15:13:24 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG JAP 0 SWG Suzaku Observation of Galactic Center Region N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027050/ Quick Look
37 HESS J1616-508 244.1248 -50.8971 243.177731 -50.773494 251.629905 -29.09136 332.40352084 -0.15000913 282.8476 53632.5000231482 2005-09-19 12:00:02 53633.8183333333 2005-09-20 19:38:24 100028010 41.352 50 41.352 41.376 41.352 41.368 2 2 2 2 1 0 0 35.3731 35.3731 113.8899 0 PROCESSED 57527.3838194444 2016-05-19 09:12:42 54247 2007-05-27 00:00:00 54035.4361111111 2006-10-27 10:28:00 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000028 CALIBRATION 1 A SWG JAP 0 SWG New HESS sources and the Galactic ridge Background N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028010/ Quick Look
38 HESS J1616-508_BGD1 243.666 -51.1742 242.717138 -51.048595 251.369654 -29.420684 332.00349288 -0.15039556 283.0062 53631.9497222222 2005-09-18 22:47:36 53632.4990856482 2005-09-19 11:58:41 100028020 19.3277 25 19.3277 20.63 19.36 19.6323 1 1 1 1 1 0 0 16.6426 16.6426 47.4479 0 PROCESSED 57527.3573148148 2016-05-19 08:34:32 54247 2007-05-27 00:00:00 54035.1692476852 2006-10-27 04:03:43 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000028 CALIBRATION 1 A SWG JAP 0 SWG New HESS sources and the Galactic ridge Background N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028020/ Quick Look
39 GRO J1655-40 253.5027 -39.8455 252.639975 -39.764411 256.800671 -17.156383 344.98315976 2.45489032 268.0237 53635.3140625 2005-09-22 07:32:15 53636.2968055556 2005-09-23 07:07:24 100029010 35.2228 40 0 35.2336 35.2228 35.2308 0 1 2 2 1 0 0 28.7315 28.7315 84.9019 1 PROCESSED 57527.3997337963 2016-05-19 09:35:37 54247 2007-05-27 00:00:00 54035.4940625 2006-10-27 11:51:27 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000029 We propose to observe GRO J1655-40, a transient galactic black hole candidate. With M=~7 Msolar and distinct radio lobes, GRO J1655-40 has been classified as a microquasar. It was highly variable during the first few years after its discovery while showing irregular flaring and a wide range of continuum states. Discrete Fe K absorption structure was observed with ASCA. In the summer of 1997 it entered an extended quiescence that lasted for ~8 years. In March 2005 it became active again and XMM & Chandra have observed it since. Only Suzaku can provide the broadband sensitivity required to map the Fe K structure and the continuum as they change. GRO J1655-40 is rapidly declining and must be observed soon before it reenters quiescence. CALIBRATION 1 A SWG JAP 0 SWG GRO J1655-40 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100029010/ Quick Look
40 NGC3516 166.7299 72.5779 165.877553 72.848305 123.367172 57.997458 133.2179652 42.40001774 148.9366 53655.5813541667 2005-10-12 13:57:09 53658.3801388889 2005-10-15 09:07:24 100031010 134.4696 150 134.5096 134.5956 134.5096 134.4696 2 2 2 2 1 0 0 122.818 122.818 241.6848 0 PROCESSED 57527.6243634259 2016-05-19 14:59:05 54247 2007-05-27 00:00:00 54036.4704976852 2006-10-28 11:17:31 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000031 NGC 3516 is one of the brightest Seyfert 1s seen in BAT currently visible to Suzaku. Recent BAT and RXTE observations show that this source is ~2-3 mCrb in the 2-10 keV band and ~4-5 mCrb in 15-100 keV. NGC 3516 is currently much brighter than when XMM observed it in 2000 (e.g., it has since returned to "typical" flux). This source's Fe K line and Compton reflection hump are both quite strong (e.g., as seen with SAX; R is ~1.8 in SAX data). CALIBRATION 1 A SWG JAP 0 SWG NGC 3516 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100031010/ Quick Look
41 M82-Wind 148.894 69.7643 147.854963 70.001295 118.872596 52.161537 141.33883884 40.49666381 146.246 53662.0401273148 2005-10-19 00:57:47 53662.9390393518 2005-10-19 22:32:13 100033020 40.3586 100 40.3586 40.3826 40.3586 40.3666 2 2 2 2 1 0 0 38.3533 38.3533 77.658 0 PROCESSED 57527.6127546296 2016-05-19 14:42:22 54247 2007-05-27 00:00:00 54036.4196296296 2006-10-28 10:04:16 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000033 We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. CALIBRATION 1 A SWG JAP 0 SWG Largely Extended Emission (~12kpc) around M82 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033020/ Quick Look
42 M82-Wind 148.8885 69.7652 147.849381 70.00218 118.869202 52.16123 141.33933547 40.4945935 137.7608 53670.4681134259 2005-10-27 11:14:05 53671.1002199074 2005-10-28 02:24:19 100033030 28.3638 100 28.3798 28.3798 28.3718 28.3638 2 2 2 2 1 0 0 25.8121 25.8121 54.604 1 PROCESSED 57527.6784606482 2016-05-19 16:16:59 54247 2007-05-27 00:00:00 54036.8639467593 2006-10-28 20:44:05 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000033 We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. CALIBRATION 1 A SWG JAP 0 SWG Largely Extended Emission (~12kpc) around M82 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100033030/ Quick Look
43 Her X-1 254.465 35.3306 254.01442 35.406187 246.002276 57.482156 58.13562438 37.51514805 249.5714 53648.6450462963 2005-10-05 15:28:52 53649.4341898148 2005-10-06 10:25:14 100035010 36.1235 40 36.9235 36.1235 36.9235 36.9235 2 1 2 2 1 0 0 33.3229 33.3229 68.178 0 PROCESSED 57527.5593518518 2016-05-19 13:25:28 54247 2007-05-27 00:00:00 54036.0084375 2006-10-28 00:12:09 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000035 CALIBRATION 1 A SWG JAP 0 SWG HXD Performance Verification using Her X-1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100035010/ Quick Look
44 Sgr_A_west 266.3063 -29.1685 265.51059 -29.148631 266.749258 -5.769039 359.75676556 -0.04750971 264.9604 53642.1914467593 2005-09-29 04:35:41 53643.187025463 2005-09-30 04:29:19 100037010 43.7412 50 43.7412 43.7492 43.7492 43.7492 2 2 2 2 1 0 0 39.3941 39.3941 86.0139 0 PROCESSED 57527.4581828704 2016-05-19 10:59:47 54247 2007-05-27 00:00:00 54035.6663310185 2006-10-27 15:59:31 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000037 CALIBRATION 1 A SWG JAP 0 SWG Suzaku Obseration of Galactic Center region 2 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037010/ Quick Look
45 GRS1915+105 288.8014 10.9368 288.21144 10.848425 292.141211 32.943669 45.35928754 -0.22611181 260.5762 53659.6951967593 2005-10-16 16:41:05 53661.9724305556 2005-10-18 23:20:18 100039010 84.7777 80 85.0631 86.4305 85.0711 84.7777 3 3 3 3 1 0 0 68.8623 68.8623 196.7338 2 PROCESSED 57527.9188541667 2016-05-19 22:03:09 54247 2007-05-27 00:00:00 54043.8117476852 2006-11-04 19:28:55 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000039 This observation will be performed as a part of the big multiwavelength campain including Suzaku, VLA, Integral, RXTE, and Spitzer. CALIBRATION 1 A SWG JAP 0 SWG Campaign of coordinated observation of GRS 1915+105 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100039010/ Quick Look
46 RXJ1856.5-3754 284.1433 -37.91 283.291633 -37.976029 281.504649 -15.032837 358.59722216 -17.21146697 84.0127 53817.9388078704 2006-03-23 22:31:53 53819.4433217593 2006-03-25 10:38:23 100041020 79.169 80 79.177 79.169 79.177 79.177 2 2 2 2 1 0 0 53.2099 53.2099 129.9759 1 PROCESSED 57533.3325231482 2016-05-25 07:58:50 54247 2007-05-27 00:00:00 54042.2967824074 2006-11-03 07:07:22 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000041 We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. CALIBRATION 1 A SWG JAP 0 SWG LOW ENERGY QE CALIBRATION OF XIS XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100041020/ Quick Look
47 Crab nebula 83.6399 21.8519 82.888543 21.819249 84.098328 -1.458773 184.69891686 -5.86604099 86.8683 53604.3898263889 2005-08-22 09:21:21 53604.4890972222 2005-08-22 11:44:18 100007030 2.7861 5 2.7861 2.7861 2.7901 2.7861 1 1 1 1 1 0 0 2.1927 2.1927 8.5541 0 PROCESSED 57520.7416203704 2016-05-12 17:47:56 54247 2007-05-27 00:00:00 54105.2865393518 2007-01-05 06:52:37 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000007 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Nebula N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100007030/ Quick Look
48 Crab nebula 83.9887 22.0345 83.236236 22.00353 84.429494 -1.290207 184.71743044 -5.49499441 86.8666 53608.5155902778 2005-08-26 12:22:27 53608.7153472222 2005-08-26 17:10:06 100010100 9.694 5 9.694 9.694 9.694 9.694 1 1 1 1 1 0 0 7.5812 7.5812 17.2479 0 PROCESSED 57526.9259606482 2016-05-18 22:13:23 54247 2007-05-27 00:00:00 54122.4242939815 2007-01-22 10:10:59 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010100/ Quick Look
49 Vega 279.2264 38.7699 278.806278 38.72626 285.283614 61.72204 67.43212753 19.23869014 301.7896 53615.367349537 2005-09-02 08:48:59 53615.603587963 2005-09-02 14:29:10 100017010 11.3985 10 11.4065 11.4065 11.4065 11.3985 2 2 2 2 1 0 0 11.5751 11.5751 20.4039 0 PROCESSED 57527.2607407407 2016-05-19 06:15:28 54247 2007-05-27 00:00:00 53906.0764814815 2006-06-20 01:50:08 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000017 CALIBRATION 1 A SWG JAP 0 SWG XIS OBF check with Vega N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100017010/ Quick Look
50 A0535+026 84.7243 26.3189 83.946776 26.291426 85.267864 2.964757 181.44092218 -2.64422146 83.608 53627.5694907407 2005-09-14 13:40:04 53628.0418865741 2005-09-15 01:00:19 100021010 21.761 20 21.761 21.761 21.761 21.761 2 2 2 2 1 0 0 21.2572 21.2572 40.7839 1 PROCESSED 57527.3122337963 2016-05-19 07:29:37 54247 2007-05-27 00:00:00 54035.0644444444 2006-10-27 01:32:48 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000021 We propose to observe the X-ray binary pulsar A0535+26. The main objectives is measuring changes in the cyclotron resonance energy in an outburst decay.It is known from another X-ray pulsar 4U0115+63 that the cyclotron resonance energy increased from 11 keV to 16 keV, as the luminosity decreased across a threshold luminosity of 4x10^37 erg/s. The flare of A0535+26 is a chance to know whether this behavior is the RULE among binary pulsars or an EXCEPTION. A0535+26 is fading down and will reach 30mCrab (5-100keV) on September 17, which is 5x10^36 erg/s. It is better to be observed as soon as possible, before it fades out. CALIBRATION 1 A SWG JAP 0 SWG TOO Observation of A0535+026 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100021010/ Quick Look
51 Crab nebula 83.7552 22.0249 83.002845 21.992803 84.212769 -1.290605 184.60948321 -5.68314749 86.8656 53609.2022106482 2005-08-27 04:51:11 53609.3125810185 2005-08-27 07:30:07 100010140 3.419 5 3.419 3.419 3.419 3.419 1 1 1 1 1 0 0 3.7554 3.7554 9.5319 0 PROCESSED 57526.9383217593 2016-05-18 22:31:11 54247 2007-05-27 00:00:00 54118.9983796296 2007-01-18 23:57:40 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010140/ Quick Look
52 Crab Nebula 83.6309 22.0151 82.87863 21.982404 84.097185 -1.295359 184.55585082 -5.78574816 87.8466 53628.8269212963 2005-09-15 19:50:46 53629.0904976852 2005-09-16 02:10:19 100023020 12.5271 10 12.5311 12.5271 12.5364 12.5351 2 2 2 2 1 0 0 13.3529 13.3529 22.764 1 PROCESSED 57527.3409143518 2016-05-19 08:10:55 54247 2007-05-27 00:00:00 54109.193599537 2007-01-09 04:38:47 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000023 Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths. CALIBRATION 1 A SWG JAP 0 SWG Crab at nominal positions N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100023020/ Quick Look
53 NGC 2110 88.0444 -7.458 87.440268 -7.468978 87.743148 -30.884192 212.92660512 -16.54877043 103.4188 53629.3796296296 2005-09-16 09:06:40 53631.8308333333 2005-09-18 19:56:24 100024010 101.7487 100 101.9265 103.7601 101.7487 102.1483 2 2 2 2 1 0 0 86.0433 86.0433 211.7558 4 PROCESSED 57527.4030324074 2016-05-19 09:40:22 54247 2007-05-27 00:00:00 54035.4624189815 2006-10-27 11:05:53 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000024 The Narrow Emission Line Galaxy NGC 2110 was the brightest AGN in the initial BAT survey release (BAT flux of 2.1E-10 erg/cm2/sec) visible to Suzaku during Sept./Oct., and is still currently bright in BAT. A 2003 RXTE observation yielded F_2-10 keV = 4E-11 erg/cm2/sec. The source is currently almost 3 times brighter than during the SAX observations. The main goals are to measure the high energy cutoff and to place a strong limit on the presence of reflection. The Compton reflection hump is weak in SAX data (suggesting that the Fe K line originates in Compton-thin material). Determining the strength of the reflection component is critical for constraining the geometry of the accreting material. CALIBRATION 1 A SWG JAP 0 SWG Narrow Emission Line Galaxy NGC 2110 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100024010/ Quick Look
54 COMA CLUSTER OFFSET 194.6939 27.9466 194.090146 28.216217 181.281218 31.269541 60.06105128 88.1791818 318.0815 53885.0996412037 2006-05-30 02:23:29 53886.8384722222 2006-05-31 20:07:24 801044010 79.172 80 79.172 79.172 79.172 79.172 2 2 2 2 1 0 0 75.2282 75.2282 150.2049 2 PROCESSED 57534.5195949074 2016-05-26 12:28:13 54394 2007-10-21 00:00:00 53926.7587384259 2006-07-10 18:12:35 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010091 In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past. EXTRAGALACTIC DIFFUSE SOURCES 8 A KYOKO MATSUSHITA JAP 1 AO1 THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801044010/ Quick Look
55 SS 433 287.9527 4.99 287.334904 4.905608 290.182673 27.181461 39.69879316 -2.23786427 78.6446 53833.4611458333 2006-04-08 11:04:03 53834.4579166667 2006-04-09 10:59:24 401004010 40.1976 40 40.2216 40.1976 40.2296 40.2136 2 2 2 2 1 0 0 30.4749 30.4749 86.11 2 PROCESSED 57533.4357638889 2016-05-25 10:27:30 54400 2007-10-27 00:00:00 53906.5501736111 2006-06-20 13:12:15 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010031 SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. GALACTIC POINT SOURCES 4 A NOBUYUKI KAWAI JAP 1 AO1 SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/ Quick Look
56 MRK 1073 48.7759 41.9723 47.948749 41.787366 57.835678 23.02641 149.56255257 -13.3516285 258.3737 54135.7651851852 2007-02-04 18:21:52 54136.6641087963 2007-02-05 15:56:19 701007020 39.5111 40 39.5191 39.5111 0 39.5191 2 2 0 2 1 0 0 37.1814 37.1814 77.6519 0 PROCESSED 57537.3263657407 2016-05-29 07:49:58 54735 2008-09-26 00:00:00 54151.4969444445 2007-02-20 11:55:36 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010037 We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large EXTRAGALACTIC COMPACT SOURCES 7 B YUICHI TERASHIMA JAP 1 AO1 COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007020/ Quick Look
57 1E1207.4-5209 182.4916 -52.442 181.83735 -52.163724 209.144209 -45.784625 296.53791481 9.91413144 148.6893 54146.2087384259 2007-02-15 05:00:35 54147.6390509259 2007-02-16 15:20:14 401030020 49.8266 50 50.0734 49.8266 0 50.0894 1 2 0 1 1 0 0 44.4468 44.4468 123.576 2 PROCESSED 57537.4372337963 2016-05-29 10:29:37 54750 2008-10-11 00:00:00 54153.9886458333 2007-02-22 23:43:39 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010152 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. GALACTIC POINT SOURCES 4 B ATSUMASA YOSHIDA JAP 1 AO1 A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/ Quick Look
58 V1223 SGR 283.7445 -31.105 282.940068 -31.169256 281.851865 -8.228404 5.0082738 -14.31987205 79.9528 54203.4803240741 2007-04-13 11:31:40 54204.9418055556 2007-04-14 22:36:12 402002010 60.706 60 60.706 60.706 0 60.706 2 2 0 2 1 0 0 46.2861 46.2861 126.2719 2 PROCESSED 57538.1822800926 2016-05-30 04:22:29 54744 2008-10-05 00:00:00 54210.6596875 2007-04-20 15:49:57 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020008 The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. GALACTIC POINT SOURCES 4 A MANABU ISHIDA JAP 2 AO2 MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402002010/ Quick Look
59 PSR B1259-63 195.6556 -63.8839 194.86632 -63.61523 227.712317 -50.941906 304.16255435 -1.03887935 293.4832 54304.2811226852 2007-07-23 06:44:49 54304.6877777778 2007-07-23 16:30:24 402014050 19.7023 20 19.7023 19.7023 0 19.7023 1 1 0 1 1 0 0 17.7549 17.7549 35.1279 0 PROCESSED 57539.3024768518 2016-05-31 07:15:34 54707 2008-08-29 00:00:00 54339.2175347222 2007-08-27 05:13:15 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020059 We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. GALACTIC POINT SOURCES 4 A YASUNOBU UCHIYAMA JAP 2 AO2 THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402014050/ Quick Look
60 LS 5039 276.5633 -14.9109 275.848755 -14.941003 276.400444 8.383997 16.82651822 -1.31880921 270.412 54352.6780555556 2007-09-09 16:16:24 54358.4725 2007-09-15 11:20:24 402015010 203.2399 200 203.2399 203.2399 0 203.2399 2 2 0 2 1 0 0 181.095 181.095 442.0879 4 PROCESSED 57540.0947685185 2016-06-01 02:16:28 54745 2008-10-06 00:00:00 54384.7259027778 2007-10-11 17:25:18 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020062 The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system. GALACTIC POINT SOURCES 4 A TADAYUKI TAKAHASHI JAP 2 AO2 SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402015010/ Quick Look
61 SN1006 SW-Rim 225.5051 -42.0698 224.686984 -41.873221 235.327536 -23.832864 327.36692545 14.52303039 297.2712 53623.5862962963 2005-09-10 14:04:16 53624.993287037 2005-09-11 23:50:20 100019030 28.5245 50 28.5325 28.5245 28.5409 28.5405 2 2 2 2 1 0 0 27.0082 27.0082 121.5519 5 PROCESSED 57527.3126967593 2016-05-19 07:30:17 54247 2007-05-27 00:00:00 54034.9697453704 2006-10-26 23:16:26 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000019 CALIBRATION 1 A SWG JAP 0 SWG SN1006 observation with XIS and HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100019030/ Quick Look
62 4U 1700+24 256.6316 23.9071 256.110961 23.972677 252.098688 46.519124 45.07419011 32.98144858 280.149 54334.7787615741 2007-08-22 18:41:25 54335.875162037 2007-08-23 21:00:14 402023010 50.2445 50 50.2525 50.2605 0 50.2445 2 2 0 2 1 0 0 45.3268 45.3268 94.7158 2 PROCESSED 57539.6636226852 2016-05-31 15:55:37 54723 2008-09-14 00:00:00 54350.4606481482 2007-09-07 11:03:20 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020105 We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV. GALACTIC POINT SOURCES 4 B OSAMU NAGAE JAP 2 AO2 STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402023010/ Quick Look
63 CYG OB2 ASSOCIATION 308.2175 41.2935 307.768848 41.122144 329.008943 57.17316 80.16491027 0.83267098 220.3949 54452.9185532407 2007-12-18 22:02:43 54453.843912037 2007-12-19 20:15:14 402030010 41.1147 40 41.1147 41.1147 0 41.1147 2 2 0 2 1 0 0 37.9181 37.9181 79.9439 0 PROCESSED 57540.9006597222 2016-06-01 21:36:57 54828 2008-12-28 00:00:00 54460.6521643518 2007-12-26 15:39:07 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 020150 Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. GALACTIC POINT SOURCES 4 C SHUNJI KITAMOTO JAP 2 AO2 STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/402030010/ Quick Look
64 EMS0071 16.6433 48.9425 15.913472 48.675321 36.903288 38.099489 125.49064727 -13.85403968 69.9406 55392.4123148148 2010-07-15 09:53:44 55392.8855092593 2010-07-15 21:15:08 705010010 23.0102 20 23.0102 23.0102 0 23.0102 2 2 0 2 1 0 0 19.568 19.568 40.8819 0 PROCESSED 57552.6419560185 2016-06-13 15:24:25 55779 2011-08-06 00:00:00 55411.2637384259 2010-08-03 06:19:47 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050050 We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". EXTRAGALACTIC COMPACT SOURCES 7 A JUN KATAOKA JAP 5 AO5 SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705010010/ Quick Look
65 BD +30 3639 293.6993 30.5065 293.208675 30.395694 303.554886 51.223276 64.78119899 5.00649051 237.7342 53676.9934837963 2005-11-02 23:50:37 53677.8230324074 2005-11-03 19:45:10 100025020 31.1384 40 31.1384 31.1624 31.1464 31.1544 2 2 2 2 1 0 0 27.1258 27.1258 71.638 1 PROCESSED 57527.9315509259 2016-05-19 22:21:26 54247 2007-05-27 00:00:00 54037.1080902778 2006-10-29 02:35:39 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000025 The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time. CALIBRATION 1 A SWG JAP 0 SWG Observation of planetary nebula BD +30 3639 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100025020/ Quick Look
66 KS1741-293(GC_BGD_2) 266.2069 -29.3515 265.410046 -29.331146 266.666918 -5.954235 359.55541243 -0.06909433 265.0174 53637.5288541667 2005-09-24 12:41:33 53637.5946296296 2005-09-24 14:16:16 100027040 1.937 5 1.937 1.937 1.937 1.937 1 1 1 1 1 0 0 1.7637 1.7637 5.68 0 PROCESSED 57527.404525463 2016-05-19 09:42:31 54247 2007-05-27 00:00:00 53907.393275463 2006-06-21 09:26:19 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000027 We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. CALIBRATION 1 A SWG JAP 0 SWG Suzaku Observation of Galactic Center Region N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100027040/ Quick Look
67 HESS J1616-508_BGD2 244.4656 -50.6883 243.5199 -50.566183 251.824242 -28.844194 332.70353325 -0.14997577 283.1793 53633.8196412037 2005-09-20 19:40:17 53634.3120833333 2005-09-21 07:29:24 100028030 21.8735 25 21.8895 21.8895 21.8815 21.8735 1 1 1 1 1 0 0 18.2063 18.2063 42.5359 0 PROCESSED 57527.3722800926 2016-05-19 08:56:05 54247 2007-05-27 00:00:00 54035.4698842593 2006-10-27 11:16:38 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000028 CALIBRATION 1 A SWG JAP 0 SWG New HESS sources and the Galactic ridge Background N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100028030/ Quick Look
68 GC_SOUTH_1 268.0988 -29.4771 267.30082 -29.465922 268.32614 -6.047082 0.29758282 -1.54591478 274.6002 56190.0385069444 2012-09-20 00:55:27 56191.3341435185 2012-09-21 08:01:10 507028010 51.7619 50 51.7619 51.7699 0 51.7699 3 3 0 3 1 0 0 41.1534 41.1534 111.9318 1 PROCESSED 57607.1304398148 2016-08-07 03:07:50 56584 2013-10-19 00:00:00 56218.5464930556 2012-10-18 13:06:57 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 070042 We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. GALACTIC DIFFUSE EMISSION 5 A SHINYA NAKASHIMA JAP 7 AO7 OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507028010/ Quick Look
69 ULXs in NGC 1313 49.5245 -66.5352 49.373425 -66.716272 341.380796 -74.178462 283.41323765 -44.63106544 172.6337 53658.556400463 2005-10-15 13:21:13 53659.6252777778 2005-10-16 15:00:24 100032010 32.878 40 32.878 32.878 32.878 32.878 1 1 1 1 1 0 0 30.38 30.38 92.3439 1 PROCESSED 57527.587349537 2016-05-19 14:05:47 54247 2007-05-27 00:00:00 54036.1929398148 2006-10-28 04:37:50 3.0.22.43 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000032 We propose Suzaku observation of a nearby (4.5 Mpc) galaxy NGC 1313 hosting two prototypical ULXs. These ASCA specta of many ULXs were described with a "high temperature diskbb" model, spectra obtained with XMM (and Chandra) prefer a "power-law plus low-temperature disk" modeling. The superior 5-10 keV sensitivity of Suzaku allows us to examine whether the spectra of luminous ULXs indeed exhibit a turn-over around 5 keV or extend up to 10 keV. CALIBRATION 1 A SWG JAP 0 SWG ULXs in NGC 1313 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100032010/ Quick Look
70 JUPITER 104.4639 23.0622 103.708176 23.129949 103.287865 0.285992 192.81439153 11.62759441 264.6138 56767.1149421296 2014-04-20 02:45:31 56767.448125 2014-04-20 10:45:18 508023110 16.7417 160 16.7417 16.7737 0 16.7657 1 1 0 1 0 0 0 0 0 0 0 PROCESSED 57614.9630671296 2016-08-14 23:06:49 57212 2015-07-09 00:00:00 56789.801712963 2014-05-12 19:14:28 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080061 Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. GALACTIC DIFFUSE EMISSION 5 A YUICHIRO EZOE JAP 8 AO8 SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023110/ Quick Look
71 CYGNUS LOOP BLOWOUT3 312.3799 29.0257 311.853293 28.839005 325.853846 44.599011 72.47923846 -9.33489782 78.1517 55688.6493981482 2011-05-07 15:35:08 55689.9654976852 2011-05-08 23:10:19 506013010 60.2669 60 60.2669 60.2749 0 60.2669 2 2 0 2 1 0 0 55.9803 55.9803 113.6288 1 PROCESSED 57601.9873611111 2016-08-01 23:41:48 56066 2012-05-19 00:00:00 55700.4602083333 2011-05-19 11:02:42 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060053 The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. GALACTIC DIFFUSE EMISSION 5 A HIROYUKI UCHIDA JAP 6 AO6 MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506013010/ Quick Look
72 HYDRA A-2 139.672 -11.9467 139.069416 -11.735403 146.240414 -26.215979 242.89463155 25.29884455 94.9986 55509.1804861111 2010-11-09 04:19:54 55510.3008680556 2010-11-10 07:13:15 805008010 41.8231 40 41.8311 41.8231 0 41.8311 2 2 0 2 1 0 0 34.5896 34.5896 96.7898 2 PROCESSED 57554.050162037 2016-06-15 01:12:14 55890 2011-11-25 00:00:00 55524.1344791667 2010-11-24 03:13:39 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050012 X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster EXTRAGALACTIC DIFFUSE SOURCES 8 C KYOKO MATSUSHITA JAP 5 AO5 DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805008010/ Quick Look
73 A 3376 90.5561 -39.9584 90.148808 -39.956705 90.960808 -63.398292 246.50686261 -25.98989573 107.6124 53649.6153703704 2005-10-06 14:46:08 53653.4495833333 2005-10-10 10:47:24 100034010 118.7792 150 118.7792 121.7373 118.8498 119.3357 2 2 2 2 1 0 0 100.5401 100.5401 331.2537 3 PROCESSED 57527.6218171296 2016-05-19 14:55:25 54247 2007-05-27 00:00:00 54109.6396990741 2007-01-09 15:21:10 3.0.22.43 5 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000034 Abell 3376 (z=0.046) is a merging cluster with a T=4 keV (*3) hosting a pair of strong radio halos (see figure). It is one of the few clusters from which BeppoSAX positively detected excess hard X-rays (Nevalainen et al. ApJ 608, 166, 2004). Because of the relatively low temperature, the HXD-PIN energy band is expected to be relatively free from thermal emission, making this object ideal to the search for non-thermal signals. We expect the non-thermal flux to be 4-5% of the PIN background at 20 keV, and a 150 ksec on-source exposure would be needed to securely detect this. To know the current background over the full COR range, an off-source exposure for one day or a ~40 ksec exposure onto a very soft source, would be required immediately before or after the on-source data acquisition. CALIBRATION 1 A SWG JAP 0 SWG Diffuse Hard X-rays from Clusters N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100034010/ Quick Look
74 1E1743.1-2843 GCBGD3 266.5944 -28.6526 265.801896 -28.634135 266.98972 -5.247071 0.32852719 0.00581314 264.8798 53644.2657523148 2005-10-01 06:22:41 53644.3162268518 2005-10-01 07:35:22 100037050 2.4 5 2.4 2.4 2.4 2.4 2 2 2 2 1 0 0 2.2329 2.2329 4.3539 0 PROCESSED 57527.4530902778 2016-05-19 10:52:27 54247 2007-05-27 00:00:00 54056.1970833333 2006-11-17 04:43:48 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000037 CALIBRATION 1 A SWG JAP 0 SWG Suzaku Obseration of Galactic Center region 2 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100037050/ Quick Look
75 1E 1048.1-5937 162.5452 -59.8394 162.049535 -59.57411 203.219635 -58.558248 288.24102095 -0.47209541 101.4368 54800.9597337963 2008-11-30 23:02:01 54802.5927083333 2008-12-02 14:13:30 403005010 100.4231 100 100.443 100.4231 0 100.4231 2 2 0 2 1 0 0 68.1049 68.1049 141.0819 0 PROCESSED 57544.6078472222 2016-06-05 14:35:18 55178 2009-12-13 00:00:00 54812.0471875 2008-12-12 01:07:57 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030013 Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs. GALACTIC POINT SOURCES 4 C JUMPEI TAKATA JAP 3 AO3 X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403005010/ Quick Look
76 MARS-P3 102.9612 25.1565 102.192848 25.217116 101.724463 2.241555 190.28784034 11.26022306 298.032 54559.4933796296 2008-04-03 11:50:28 54559.5766087963 2008-04-03 13:50:19 403006030 3.886 100 3.886 3.91 0 3.894 1 1 0 1 1 0 0 3.1134 3.1134 7.1839 0 PROCESSED 57542.0373148148 2016-06-03 00:53:44 54953 2009-05-02 00:00:00 54577.0484259259 2008-04-21 01:09:44 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006030/ Quick Look
77 MARS-P11 103.2936 25.1207 102.525618 25.182892 102.027614 2.233108 190.44969799 11.5184009 298.1493 54560.1601041667 2008-04-04 03:50:33 54560.2433333333 2008-04-04 05:50:24 403006110 4.6198 100 4.6278 4.6198 0 4.6358 1 1 0 1 1 0 0 4.0749 4.0749 7.1839 0 PROCESSED 57542.0559490741 2016-06-03 01:20:34 54953 2009-05-02 00:00:00 54577.1745023148 2008-04-21 04:11:17 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006110/ Quick Look
78 MARS-P13 103.3779 25.1101 102.610021 25.172691 102.104653 2.229561 190.49210676 11.58330245 298.1799 54560.3267708333 2008-04-04 07:50:33 54560.41 2008-04-04 09:50:24 403006130 4.2518 100 4.2678 4.2518 0 4.2678 1 1 0 1 1 0 0 3.529 3.529 7.1839 0 PROCESSED 57542.0605671296 2016-06-03 01:27:13 54953 2009-05-02 00:00:00 54577.9292939815 2008-04-21 22:18:11 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006130/ Quick Look
79 MARS-P16 103.503 25.0968 102.735261 25.159983 102.218767 2.2268 190.55275085 11.68067717 298.2223 54560.5768171296 2008-04-04 13:50:37 54560.66 2008-04-04 15:50:24 403006160 2.3262 100 2.3262 2.3262 0 2.3262 2 2 0 2 1 0 0 2.134 2.134 7.1799 0 PROCESSED 57542.0664236111 2016-06-03 01:35:39 54953 2009-05-02 00:00:00 54577.9478935185 2008-04-21 22:44:58 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006160/ Quick Look
80 MARS-P21 103.7101 25.0688 102.942627 25.132964 102.408276 2.21649 190.65860601 11.8395058 298.2947 54560.9933217593 2008-04-04 23:50:23 54561.0765509259 2008-04-05 01:50:14 403006210 2.8808 100 2.8808 2.8808 0 2.8808 1 1 0 1 1 0 0 3.4516 3.4516 7.1839 0 PROCESSED 57542.0774884259 2016-06-03 01:51:35 54953 2009-05-02 00:00:00 54578.0612847222 2008-04-22 01:28:15 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006210/ Quick Look
81 MARS-P23 103.7955 25.0599 103.028122 25.124467 102.486187 2.214951 190.69976585 11.90614711 298.325 54561.1600347222 2008-04-05 03:50:27 54561.2432175926 2008-04-05 05:50:14 403006230 4.5188 100 4.5268 4.5188 0 4.5348 1 1 0 1 1 0 0 3.6868 3.6868 7.1839 0 PROCESSED 57542.0791898148 2016-06-03 01:54:02 54953 2009-05-02 00:00:00 54578.1176157407 2008-04-22 02:49:22 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006230/ Quick Look
82 MARS-P25 103.8803 25.0503 103.113021 25.115268 102.56363 2.212708 190.74132534 11.97202775 298.3546 54561.3266550926 2008-04-05 07:50:23 54561.4098842593 2008-04-05 09:50:14 403006250 4.2612 100 4.2692 4.2612 0 4.2692 1 1 0 1 1 0 0 3.2511 3.2511 7.1839 0 PROCESSED 57542.2336458333 2016-06-03 05:36:27 54953 2009-05-02 00:00:00 54578.1323032407 2008-04-22 03:10:31 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006250/ Quick Look
83 MARS-P26 103.921 25.0474 103.153759 25.112561 102.600638 2.213348 190.75967691 12.00436516 298.3671 54561.4100347222 2008-04-05 09:50:27 54561.4932175926 2008-04-05 11:50:14 403006260 4.7976 100 4.8136 4.7976 0 4.8216 1 1 0 1 1 0 0 3.7622 3.7622 7.1839 0 PROCESSED 57542.2337962963 2016-06-03 05:36:40 54953 2009-05-02 00:00:00 54578.1374074074 2008-04-22 03:17:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030015 We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. GALACTIC POINT SOURCES 4 A YUICHIRO EZOE JAP 3 AO3 SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403006260/ Quick Look
84 COMA SUBHALO2 194.5069 27.3689 193.901795 27.638743 181.411119 30.679028 42.63932899 88.51577103 315.0001 56452.5504976852 2013-06-09 13:12:43 56453.0265046296 2013-06-10 00:38:10 808020010 21.1563 20 21.1563 21.1563 0 21.1563 1 1 0 1 1 0 0 17.608 17.608 41.1199 1 PROCESSED 57611.5058564815 2016-08-11 12:08:26 56872 2014-08-03 00:00:00 56506.7547222222 2013-08-02 18:06:48 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080023 We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. EXTRAGALACTIC DIFFUSE SOURCES 8 A NOBUHIRO OKABE JAP 8 AO8 SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808020010/ Quick Look
85 A3376 NORTH 90.6541 -39.7108 90.244762 -39.708634 91.122885 -63.149983 246.26196714 -25.85404299 80.8001 56553.3109143518 2013-09-18 07:27:43 56554.8453935185 2013-09-19 20:17:22 808029010 57.6912 57 57.6912 57.6992 0 57.7072 2 2 0 2 1 0 0 50.8185 50.8185 132.57 0 PROCESSED 57612.703275463 2016-08-12 16:52:43 56956 2014-10-26 00:00:00 56588.7436689815 2013-10-23 17:50:53 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080037 Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. EXTRAGALACTIC DIFFUSE SOURCES 8 B TAKAYA OHASHI JAP 8 AO8 SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808029010/ Quick Look
86 NORTH POLAR SPUR 260.5905 4.7489 259.972652 4.795886 259.371969 27.842624 26.83412197 21.95376599 264.1143 53646.4785763889 2005-10-03 11:29:09 53647.4515277778 2005-10-04 10:50:12 100038010 43.0689 50 43.1489 44.2129 43.0689 43.2929 2 2 2 2 1 0 0 40.7715 40.7715 84.0019 0 PROCESSED 57527.5342824074 2016-05-19 12:49:22 54247 2007-05-27 00:00:00 54035.8928009259 2006-10-27 21:25:38 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000038 We propose to observe the North Polar Spur for 100 ksec. The main objectives are below (1) Search for emission lines of N and C that originates from low kT emission (2) Precisely determine the abundance of the NPS The measurement of N and C lines will be the first for XIS. This is also the first for extended sources. The first trial to measure the emission from the C-band (below 0.3keV) by using BI. This will be a guide line how to use the C-band data. Since the C-band intensity is already known, this will be the first calibration of the BI at low energy. The scientific objectives are already given in the mail distributed in the swg. CALIBRATION 1 A SWG JAP 0 SWG North Polar Spur N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100038010/ Quick Look
87 ARCHES CLUSTER 266.4808 -28.778 265.687528 -28.758983 266.892731 -5.374834 0.16960578 0.02569084 109.9998 54911.0857407407 2009-03-21 02:03:28 54913.7681712963 2009-03-23 18:26:10 403009010 110.7933 100 110.7933 110.7933 0 110.7933 2 2 0 2 1 0 0 91.6578 91.6578 231.7417 3 PROCESSED 57545.9555787037 2016-06-06 22:56:02 55330 2010-05-14 00:00:00 54924.3822106482 2009-04-03 09:10:23 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030029 We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring. GALACTIC POINT SOURCES 4 B MASAHIRO TSUJIMOTO JAP 3 AO3 A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403009010/ Quick Look
88 LS I+61 303_1 40.1455 61.188 39.183267 60.973753 59.828193 42.868734 135.69810374 1.0510579 270.0003 54853.9515856482 2009-01-22 22:50:17 54854.8648032407 2009-01-23 20:45:19 403015010 40.5514 40 40.5514 40.5514 0 40.5514 2 2 0 2 1 0 0 25.7312 25.7312 78.868 0 PROCESSED 57545.3022916667 2016-06-06 07:15:18 55329 2010-05-13 00:00:00 54880.5343865741 2009-02-18 12:49:31 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A YASUSHI FUKAZAWA JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403015010/ Quick Look
89 LS I+61 303_2 40.1457 61.1877 39.18347 60.973453 59.828143 42.868421 135.69831419 1.05082335 270.0006 54856.6966087963 2009-01-25 16:43:07 54858.1766666667 2009-01-27 04:14:24 403016010 61.0667 60 61.0784 61.0667 0 61.0784 2 2 0 2 1 0 0 26.6591 26.6591 127.8398 1 PROCESSED 57545.3828819444 2016-06-06 09:11:21 55329 2010-05-13 00:00:00 54880.5522106482 2009-02-18 13:15:11 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A YASUSHI FUKAZAWA JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403016010/ Quick Look
90 LS I+61 303_3 40.2018 61.1949 39.239095 60.980826 59.865781 42.86376 135.72005286 1.06843757 246.2753 54872.1842592593 2009-02-10 04:25:20 54873.7252199074 2009-02-11 17:24:19 403017010 68.6273 60 68.6273 68.6273 0 68.6273 2 2 0 2 1 0 0 65.0685 65.0685 133.1218 1 PROCESSED 57545.5290856482 2016-06-06 12:41:53 55330 2010-05-14 00:00:00 54893.4210300926 2009-03-03 10:06:17 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030077 We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. GALACTIC POINT SOURCES 4 A YASUSHI FUKAZAWA JAP 3 AO3 X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403017010/ Quick Look
91 A1689-OFFSET3 197.7048 -1.4241 197.062246 -1.158416 196.866357 5.631394 312.98436439 61.06880263 289.9992 54672.423599537 2008-07-25 10:09:59 54673.474525463 2008-07-26 11:23:19 803026010 44.0942 40 44.0942 44.0942 0 44.0942 2 2 0 2 1 0 0 37.7063 37.7063 90.7878 1 PROCESSED 57543.149537037 2016-06-04 03:35:20 55076 2009-09-02 00:00:00 54707.1173263889 2008-08-29 02:48:57 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030100 We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. EXTRAGALACTIC DIFFUSE SOURCES 8 A NOBUHIRO OKABE JAP 3 AO3 UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803026010/ Quick Look
92 IGR J16194-2810 244.8908 -28.0663 244.116394 -27.946439 247.849887 -6.534784 349.1669856 15.58223604 95.1879 54867.1762152778 2009-02-05 04:13:45 54868.4314236111 2009-02-06 10:21:15 403024010 45.5687 50 45.5687 45.5738 0 45.5687 2 2 0 2 1 0 0 38.7859 38.7859 108.4358 1 PROCESSED 57545.4895023148 2016-06-06 11:44:53 55329 2010-05-13 00:00:00 54880.5743518518 2009-02-18 13:47:04 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030121 We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source. GALACTIC POINT SOURCES 4 C OSAMU NAGAE JAP 3 AO3 ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403024010/ Quick Look
93 V709 CAS 7.1951 59.3013 6.498819 59.024957 38.349683 49.774418 120.03837674 -3.44309479 84.0816 54637.4334837963 2008-06-20 10:24:13 54638.1542824074 2008-06-21 03:42:10 403025010 35.8982 30 35.8982 35.8982 0 35.8982 2 2 0 2 1 0 0 33.3823 33.3823 62.2679 0 PROCESSED 57542.8811921296 2016-06-03 21:08:55 55014 2009-07-02 00:00:00 54648.3358101852 2008-07-01 08:03:34 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B KEN EBISAWA JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403025010/ Quick Look
94 RX J1940.1-1025 295.0445 -10.4193 294.356962 -10.535652 295.074294 10.867465 28.98688715 -15.49869645 79.7405 54572.8979976852 2008-04-16 21:33:07 54573.743275463 2008-04-17 17:50:19 403027010 32.4536 30 32.4536 32.4536 0 32.4536 2 2 0 2 1 0 0 26.4657 26.4657 73.0219 2 PROCESSED 57542.3241087963 2016-06-03 07:46:43 54953 2009-05-02 00:00:00 54587.0481481482 2008-05-01 01:09:20 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 030140 Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. GALACTIC POINT SOURCES 4 B KEN EBISAWA JAP 3 AO3 IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/403027010/ Quick Look
95 Crab Nebula 83.6372 22.097 82.884469 22.064333 84.106634 -1.213794 184.48946706 -5.73697 84.9994 53613.8323032407 2005-08-31 19:58:31 53613.975787037 2005-08-31 23:25:08 100015010 5.6587 5 5.6587 5.6587 5.6587 5.6587 1 1 1 1 1 0 0 5.7907 5.7907 12.3879 0 PROCESSED 57527.2296412037 2016-05-19 05:30:41 54247 2007-05-27 00:00:00 54109.1053240741 2007-01-09 02:31:40 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000015 CALIBRATION 1 A SWG JAP 0 SWG HXD boresight check with Crab N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100015010/ Quick Look
96 GS 1826-238 277.3735 -23.8572 276.610421 -23.891095 276.73109 -0.588705 9.22092987 -6.12003001 267.2862 55125.8488310185 2009-10-21 20:22:19 55127.9502777778 2009-10-23 22:48:24 404007010 102.5154 100 102.5154 102.5314 0 102.5372 2 2 0 2 1 0 0 87.9996 87.9996 181.5418 2 PROCESSED 57549.0104976852 2016-06-10 00:15:07 55534 2010-12-04 00:00:00 55166.4220833333 2009-12-01 10:07:48 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040035 We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations. GALACTIC POINT SOURCES 4 B KAZUTAKA YAMAOKA JAP 4 AO4 SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238 HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404007010/ Quick Look
97 EUVE J0317-85.5 48.9864 -85.5003 51.11405 -85.679196 278.533864 -69.749958 299.84736337 -30.72881529 65.46 55028.6017476852 2009-07-16 14:26:31 55030.1460185185 2009-07-18 03:30:16 404019010 63.0843 60 63.0843 63.0843 0 63.0843 2 2 0 2 1 0 0 56.8965 56.8965 133.4138 1 PROCESSED 57547.8712847222 2016-06-08 20:54:39 55406 2010-07-29 00:00:00 55040.2674305556 2009-07-28 06:25:06 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040083 Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects. GALACTIC POINT SOURCES 4 B ATSUSHI HARAYAMA JAP 4 AO4 FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404019010/ Quick Look
98 TT ARI 31.7181 15.2972 31.038138 15.059527 34.795947 2.311089 148.52228749 -43.79443 71.0668 55018.4424652778 2009-07-06 10:37:09 55019.3023611111 2009-07-07 07:15:24 404021010 35.7421 35 35.7421 35.7796 0 35.7876 2 2 0 2 1 0 0 31.794 31.794 74.2578 1 PROCESSED 57547.7822453704 2016-06-08 18:46:26 55399 2010-07-22 00:00:00 55029.236712963 2009-07-17 05:40:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040095 The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. GALACTIC POINT SOURCES 4 B KEI SAITOU JAP 4 AO4 IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404021010/ Quick Look
99 TX COL 85.7822 -41.0648 85.383592 -41.086265 82.635964 -64.399356 246.79781267 -29.77494364 322.4827 54963.6800578704 2009-05-12 16:19:17 54965.2502199074 2009-05-14 06:00:19 404031010 59.7818 40 59.7898 59.7898 0 59.7818 2 2 0 2 1 0 0 51.123 51.123 135.654 0 PROCESSED 57546.5734143518 2016-06-07 13:45:43 55345 2010-05-29 00:00:00 54978.2105439815 2009-05-27 05:03:11 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040113 We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. GALACTIC POINT SOURCES 4 A TAKAYUKI YUASA JAP 4 AO4 SURVEY OBSERVATION OF INTERMEDIATE POLARS HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404031010/ Quick Look
100 Crab nebula 83.6105 22.3483 82.856361 22.315501 84.093042 -0.96164 184.26290563 -5.62323625 86.8596 53607.2790509259 2005-08-25 06:41:50 53607.5139583333 2005-08-25 12:20:06 100010030 8.1129 5 8.1129 8.1129 8.1129 8.1129 2 2 2 2 1 0 0 7.8359 7.8359 20.264 1 PROCESSED 57526.8876388889 2016-05-18 21:18:12 54247 2007-05-27 00:00:00 54118.9698958333 2007-01-18 23:16:39 3.0.22.43 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000010 Crab nebula multi pointings CALIBRATION 1 A SWG JAP 0 SWG Crab Offset 1 N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100010030/ Quick Look
101 DA 240 EAST LOBE 117.3573 55.877 116.349381 56.002734 108.151975 34.146502 161.8466677 30.16323196 293.7777 55274.9306134259 2010-03-19 22:20:05 55276.7238657407 2010-03-21 17:22:22 704020010 81.7834 80 81.7834 81.7914 0 81.7914 2 2 0 2 1 0 0 74.3033 74.3033 154.9218 1 PROCESSED 57550.9753587963 2016-06-11 23:24:31 55654 2011-04-03 00:00:00 55286.3268518518 2010-03-31 07:50:40 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 040096 Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. EXTRAGALACTIC COMPACT SOURCES 7 B NAOKI ISOBE JAP 4 AO4 SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704020010/ Quick Look
102 N132D 81.2794 -69.6524 81.381964 -69.694399 312.375338 -85.522525 280.31514531 -32.77566051 53.3291 53595.4703125 2005-08-13 11:17:15 53597.5313541667 2005-08-15 12:45:09 100002010 7.4066 80 7.4066 7.4066 7.4066 7.4066 2 2 2 2 0 0 0 0 0 0 0 PROCESSED 57520.7109606482 2016-05-12 17:03:47 54247 2007-05-27 00:00:00 54038.5875925926 2006-10-30 14:06:08 3.0.22.43 6 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 000002 HXD HV ON WITH N132D, and 5 pointings with XIS CALIBRATION 1 A SWG JAP 0 SWG HXD HV ON WITH N132D N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/100002010/ Quick Look
103 NGC 5044 OFFSET1 198.8505 -16.143 198.184446 -15.87899 203.499232 -7.562902 311.28196707 46.33985641 290.0004 53919.3604398148 2006-07-03 08:39:02 53920.9599305556 2006-07-04 23:02:18 801047010 54.6204 60 54.6204 54.6204 54.6204 54.6204 2 2 2 2 1 0 0 45.8033 45.8033 138.1899 1 PROCESSED 57534.8941203704 2016-05-26 21:27:32 54394 2007-10-21 00:00:00 53942.4615740741 2006-07-26 11:04:40 3.0.22.43 6 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 010092 We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. EXTRAGALACTIC DIFFUSE SOURCES 8 A KYOKO MATSUSHITA JAP 1 AO1 THE METAL DISTRIBUTION OF THE NGC 5044 GROUP XIS N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801047010/ Quick Look
104 V773TAU 63.5571 28.1952 62.783682 28.069565 66.716115 6.867305 168.22500409 -16.34364304 260.6557 55610.1581712963 2011-02-18 03:47:46 55611.9815277778 2011-02-19 23:33:24 405011010 82.2463 80 82.2543 82.2463 0 82.2543 2 2 0 2 1 0 0 72.8287 72.8287 157.5258 2 PROCESSED 57601.0256134259 2016-08-01 00:36:53 55990 2012-03-04 00:00:00 55621.2978703704 2011-03-01 07:08:56 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050033 We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. GALACTIC POINT SOURCES 4 B YOHKO TSUBOI JAP 5 AO5 NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405011010/ Quick Look
105 1E 1547.0-5408 237.7284 -54.3676 236.761869 -54.21692 248.127922 -33.347549 327.20000551 -0.18012949 271.1663 55415.1611921296 2010-08-07 03:52:07 55415.9633796296 2010-08-07 23:07:16 405024010 51.6728 50 51.6728 51.7928 0 52.1529 2 2 0 1 1 0 0 42.7812 42.7812 69.2999 0 PROCESSED 57552.8870949074 2016-06-13 21:17:25 55793 2011-08-20 00:00:00 55427.247025463 2010-08-19 05:55:43 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050099 Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks. GALACTIC POINT SOURCES 4 B HIROYUKI NISHIOKA JAP 5 AO5 OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE HXD N https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405024010/ Quick Look
106 EMS1150 263.083 -32.7212 262.264926 -32.685689 264.095488 -9.421504 355.27740066 0.39306698 91.2452 55611.9964930556 2011-02-19 23:54:57 55612.6968055556 2011-02-20 16:43:24 405026010 20.9186 20 20.9186 20.9186 0 20.9186 1 1 0 1 1 0 0 17.2639 17.2639 60.5039 0 PROCESSED 57600.9777893518 2016-07-31 23:28:01 55988 2012-03-02 00:00:00 55621.1440740741 2011-03-01 03:27:28 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050104 Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. GALACTIC POINT SOURCES 4 A YASUYUKI TANAKA JAP 5 AO5 SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405026010/ Quick Look
107 ABELL1835 OFFSET2 210.2863 2.6798 209.652404 2.920968 207.209815 14.079845 340.21334307 60.40388756 306.816 55384.1224884259 2010-07-07 02:56:23 55385.4667939815 2010-07-08 11:12:11 805038010 45.6036 50 45.6036 45.6276 0 45.6116 2 2 0 2 1 0 0 41.2826 41.2826 116.1298 0 PROCESSED 57552.5623611111 2016-06-13 13:29:48 55801 2011-08-28 00:00:00 55434.3364930556 2010-08-26 08:04:33 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 050040 We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. EXTRAGALACTIC DIFFUSE SOURCES 8 B NOBUHIRO OKABE JAP 5 AO5 UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805038010/ Quick Look
108 4U1812-12 273.8053 -12.0935 273.104949 -12.110284 273.784611 11.297146 18.04900466 2.37362039 267.159 55838.1400347222 2011-10-04 03:21:39 55839.9168981482 2011-10-05 22:00:20 406008010 62.0143 60 62.0143 62.0143 0 62.0143 2 2 0 2 1 0 0 53.5441 53.5441 153.5099 1 PROCESSED 57603.3255902778 2016-08-03 07:48:51 56226 2012-10-26 00:00:00 55858.3124768518 2011-10-24 07:29:58 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060012 Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state. GALACTIC POINT SOURCES 4 A SOKI SAKURAI JAP 6 AO6 REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406008010/ Quick Look
109 VW HYI 62.3084 -71.2978 62.399199 -71.427045 322.000013 -79.107776 284.88912946 -38.12913625 338.7313 56049.8124305556 2012-05-02 19:29:54 56050.1668171296 2012-05-03 04:00:13 406009040 16.8177 20 16.8257 16.8257 0 16.8177 2 1 0 2 1 0 0 13.9478 13.9478 30.6159 0 PROCESSED 57605.3312847222 2016-08-05 07:57:03 56449 2013-06-06 00:00:00 56083.0857060185 2012-06-05 02:03:25 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060023 SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. GALACTIC POINT SOURCES 4 B KEI SAITOU JAP 6 AO6-TOO TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406009040/ Quick Look
110 CYG X-1 299.5916 35.1745 299.121401 35.038023 313.64901 54.223609 71.31236822 3.05181611 279.5001 55839.9245023148 2011-10-05 22:11:17 55840.9169328704 2011-10-06 22:00:23 406013010 3.7027 40 3.832 3.7027 0 40.2718 1 1 0 1 1 0 0 32.9625 32.9625 85.7339 1 PROCESSED 57603.3954166667 2016-08-03 09:29:24 56582 2013-10-17 00:00:00 56212.7247916667 2012-10-12 17:23:42 3.0.22.44 4 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 060057 We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks. GALACTIC POINT SOURCES 4 A SHIN'YA YAMADA JAP 6 AO6 REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/406013010/ Quick Look
111 AXP 4U 0142+614 26.5682 61.7591 25.700455 61.509234 52.151654 46.394786 129.37061357 -0.42523158 40.384 55811.6552314815 2011-09-07 15:43:32 55812.5731134259 2011-09-08 13:45:17 406031010 38.6497 60 38.6497 38.6497 0 38.6825 2 2 0 2 1 0 0 42.1964 42.1964 79.292 0 PROCESSED 57603.1220138889 2016-08-03 02:55:42