DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 337
No. |
object_name
|
center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
|
xis3_observation_mode
|
hxd_observation_mode
|
hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | THE CRAB OFFSETS | 83.536 | 22.0119 | 82.783772 | 21.978746 | 84.009124 | -1.294644 | 184.51119717 | -5.8617583 | 85.703 | 53984.8198263889 | 2006-09-06 19:40:33 | 53984.8891666667 | 2006-09-06 21:20:24 | 101011150 | 3.37 | 2 | 3.37 | 3.37 | 3.37 | 3.37 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.3472 | 3.3472 | 5.9839 | 0 | PROCESSED | 57535.4824189815 | 2016-05-27 11:34:41 | 53826 | 2006-04-01 00:00:00 | 54104.9730439815 | 2007-01-04 23:21:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011150/ | Quick Look | ![]() |
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2 | E0102.2-7219 | 16.0278 | -72.0394 | 15.623254 | -72.307346 | 314.607654 | -65.046746 | 301.54948943 | -45.0548182 | 34.4136 | 53876.719525463 | 2006-05-21 17:16:07 | 53877.1793287037 | 2006-05-22 04:18:14 | 101005020 | 18.1619 | 20 | 18.1619 | 18.1939 | 18.1619 | 18.1939 | 2 | 1 | 2 | 1 | 1 | 0 | 0 | 17.7633 | 17.7633 | 39.7199 | 0 | PROCESSED | 57534.3838425926 | 2016-05-26 09:12:44 | 53826 | 2006-04-01 00:00:00 | 53926.1422222222 | 2006-07-10 03:24:48 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005020/ | Quick Look | ![]() |
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3 | E0102.2-7219 | 15.9978 | -72.0424 | 15.592857 | -72.310386 | 314.59194 | -65.039632 | 301.56284618 | -45.05246644 | 92.9794 | 53933.2656597222 | 2006-07-17 06:22:33 | 53933.9030439815 | 2006-07-17 21:40:23 | 101005040 | 22.0634 | 20 | 22.0634 | 22.1034 | 22.0634 | 22.0954 | 4 | 2 | 4 | 2 | 1 | 0 | 0 | 20.9823 | 20.9823 | 55.0479 | 1 | PROCESSED | 57534.9613888889 | 2016-05-26 23:04:24 | 53826 | 2006-04-01 00:00:00 | 53942.4630092593 | 2006-07-26 11:06:44 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005040/ | Quick Look | ![]() |
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4 | E0102.2-7219 | 15.9812 | -72.0315 | 15.575859 | -72.299509 | 314.610205 | -65.030381 | 301.5690149 | -45.06369281 | 159.2453 | 53997.2263425926 | 2006-09-19 05:25:56 | 53997.562662037 | 2006-09-19 13:30:14 | 101005060 | 10.7907 | 40 | 10.8067 | 10.8067 | 10.7907 | 10.7987 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 10.3223 | 10.3223 | 29.05 | 0 | PROCESSED | 57535.6263541667 | 2016-05-27 15:01:57 | 53826 | 2006-04-01 00:00:00 | 54021.1325115741 | 2006-10-13 03:10:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005060/ | Quick Look | ![]() |
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5 | E0102.2-7219 | 15.9801 | -72.0277 | 15.574689 | -72.29571 | 314.618019 | -65.028464 | 301.56912514 | -45.06750714 | 192.8855 | 54029.650625 | 2006-10-21 15:36:54 | 54030.2265625 | 2006-10-22 05:26:15 | 101005070 | 37.1305 | 40 | 37.1705 | 37.1305 | 37.1705 | 37.1625 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 36.4716 | 36.4716 | 49.76 | 0 | PROCESSED | 57535.9063425926 | 2016-05-27 21:45:08 | 53826 | 2006-04-01 00:00:00 | 54055.5631828704 | 2006-11-16 13:30:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005070/ | Quick Look | ![]() |
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6 | E0102.2-7219 | 16.0137 | -72.0201 | 15.608673 | -72.288065 | 314.644734 | -65.034638 | 301.5537348 | -45.07437383 | 265.9905 | 54115.1395023148 | 2007-01-15 03:20:53 | 54115.6655555556 | 2007-01-15 15:58:24 | 101005100 | 22.614 | 20 | 22.614 | 22.614 | 0 | 22.614 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.1496 | 19.1496 | 45.424 | 1 | PROCESSED | 57536.8323263889 | 2016-05-28 19:58:33 | 53826 | 2006-04-01 00:00:00 | 54132.8509490741 | 2007-02-01 20:25:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005100/ | Quick Look | ![]() |
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7 | PKS2155-304 | 329.7138 | -30.2259 | 328.989973 | -30.465459 | 321.184272 | -16.770452 | 17.72949775 | -52.24318888 | 57.9013 | 53856.2600925926 | 2006-05-01 06:14:32 | 53857.2501041667 | 2006-05-02 06:00:09 | 101006010 | 38.5515 | 30 | 38.5515 | 38.5515 | 38.5515 | 38.5515 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23.9476 | 23.9476 | 85.5141 | 2 | PROCESSED | 57533.6080787037 | 2016-05-25 14:35:38 | 53826 | 2006-04-01 00:00:00 | 53913.2773842593 | 2006-06-27 06:39:26 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101006010/ | Quick Look | ![]() |
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8 | RXJ1856.5-3754 | 284.1489 | -37.9077 | 283.297255 | -37.973755 | 281.50944 | -15.030994 | 358.6011477 | -17.21474589 | 254.2953 | 54028.5128472222 | 2006-10-20 12:18:30 | 54029.6405208333 | 2006-10-21 15:22:21 | 101009010 | 40.7841 | 40 | 40.7841 | 40.7841 | 40.7841 | 40.7841 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.1699 | 35.1699 | 97.4039 | 1 | PROCESSED | 57535.9219675926 | 2016-05-27 22:07:38 | 53826 | 2006-04-01 00:00:00 | 54055.4732523148 | 2006-11-16 11:21:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101009010/ | Quick Look | ![]() |
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9 | CRAB | 83.6301 | 22.0172 | 82.877819 | 21.9845 | 84.096537 | -1.293228 | 184.55366892 | -5.78525038 | 85.7026 | 53983.2227430556 | 2006-09-05 05:20:45 | 53983.8196643518 | 2006-09-05 19:40:19 | 101010010 | 20.7175 | 20 | 20.8775 | 20.7175 | 20.8935 | 20.8855 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 19.6071 | 19.6071 | 51.5699 | 1 | PROCESSED | 57535.464224537 | 2016-05-27 11:08:29 | 53826 | 2006-04-01 00:00:00 | 54024.6695833333 | 2006-10-16 16:04:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015014 | HXD cal. | CALIBRATION | 1 | A | KAZUHIRO NAKAZAWA | JAP | 1 | AO1 | CRAB CAL FOR HXD ON 2006 AUTUMN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101010010/ | Quick Look | ![]() |
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10 | THE CRAB OFFSETS | 83.6209 | 22.1323 | 82.867975 | 22.099554 | 84.093103 | -1.177861 | 184.45137768 | -5.73082135 | 85.7132 | 53983.8199537037 | 2006-09-05 19:40:44 | 53983.8891087963 | 2006-09-05 21:20:19 | 101011010 | 3.348 | 2 | 3.348 | 3.348 | 3.348 | 3.348 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.676 | 3.676 | 5.9679 | 0 | PROCESSED | 57535.4548263889 | 2016-05-27 10:54:57 | 53826 | 2006-04-01 00:00:00 | 54104.4418287037 | 2007-01-04 10:36:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011010/ | Quick Look | ![]() |
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11 | THE CRAB OFFSETS | 83.6254 | 22.076 | 82.87279 | 22.043276 | 84.094781 | -1.234292 | 184.50140903 | -5.75744861 | 85.7164 | 53983.951712963 | 2006-09-05 22:50:28 | 53984.0904976852 | 2006-09-06 02:10:19 | 101011030 | 6.703 | 2 | 6.703 | 6.703 | 6.703 | 6.703 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5.4458 | 5.4458 | 11.9839 | 0 | PROCESSED | 57535.4650462963 | 2016-05-27 11:09:40 | 53826 | 2006-04-01 00:00:00 | 54104.972650463 | 2007-01-04 23:20:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011030/ | Quick Look | ![]() |
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12 | THE CRAB OFFSETS | 83.6338 | 21.931 | 82.882001 | 21.898319 | 84.09616 | -1.379498 | 184.62870178 | -5.82849289 | 87.5103 | 53996.9516550926 | 2006-09-18 22:50:23 | 53997.0140509259 | 2006-09-19 00:20:14 | 101011070 | 2.636 | 2 | 2.636 | 2.636 | 2.636 | 2.636 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.157 | 2.157 | 5.3839 | 0 | PROCESSED | 57535.6130092593 | 2016-05-27 14:42:44 | 53826 | 2006-04-01 00:00:00 | 54104.4160069444 | 2007-01-04 09:59:03 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011070/ | Quick Look | ![]() |
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13 | THE CRAB OFFSETS | 83.7555 | 22.0251 | 83.003144 | 21.993005 | 84.213055 | -1.290417 | 184.60946275 | -5.68280554 | 87.8963 | 53997.0840625 | 2006-09-19 02:01:03 | 53997.1529282407 | 2006-09-19 03:40:13 | 101011090 | 1.895 | 2 | 1.895 | 1.895 | 1.895 | 1.895 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.0815 | 2.0815 | 5.9459 | 0 | PROCESSED | 57535.6191435185 | 2016-05-27 14:51:34 | 53826 | 2006-04-01 00:00:00 | 54104.4517708333 | 2007-01-04 10:50:33 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011090/ | Quick Look | ![]() |
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14 | THE CRAB OFFSETS | 83.6927 | 22.0229 | 82.940372 | 21.990502 | 84.154781 | -1.290083 | 184.58004352 | -5.7331758 | 85.756 | 53984.5680092593 | 2006-09-06 13:37:56 | 53984.6252199074 | 2006-09-06 15:00:19 | 101011110 | 2.6354 | 2 | 2.6354 | 2.6354 | 2.6354 | 2.6354 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.4573 | 2.4573 | 4.942 | 0 | PROCESSED | 57535.4715046296 | 2016-05-27 11:18:58 | 53826 | 2006-04-01 00:00:00 | 54104.4321527778 | 2007-01-04 10:22:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011110/ | Quick Look | ![]() |
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15 | THE CRAB OFFSETS | 83.6616 | 22.0194 | 82.909299 | 21.986852 | 84.125816 | -1.292316 | 184.56751127 | -5.75940556 | 85.7473 | 53984.6253703704 | 2006-09-06 15:00:32 | 53984.6876967593 | 2006-09-06 16:30:17 | 101011120 | 2.9761 | 2 | 2.9761 | 2.9761 | 2.9761 | 2.9761 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.802 | 2.802 | 5.38 | 0 | PROCESSED | 57535.4738425926 | 2016-05-27 11:22:20 | 53826 | 2006-04-01 00:00:00 | 54104.4254513889 | 2007-01-04 10:12:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011120/ | Quick Look | ![]() |
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16 | THE CRAB OFFSETS | 83.5991 | 22.0137 | 82.846846 | 21.98085 | 84.067662 | -1.295453 | 184.54117278 | -5.81139714 | 85.7249 | 53984.6879398148 | 2006-09-06 16:30:38 | 53984.7572222222 | 2006-09-06 18:10:24 | 101011130 | 3.3661 | 2 | 3.3661 | 3.3661 | 3.3661 | 3.3661 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.19 | 3.19 | 5.9839 | 0 | PROCESSED | 57535.4770486111 | 2016-05-27 11:26:57 | 53826 | 2006-04-01 00:00:00 | 54104.4575 | 2007-01-04 10:58:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011130/ | Quick Look | ![]() |
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17 | PERSEUS CLUSTER | 49.9542 | 41.5047 | 49.126761 | 41.324082 | 58.607992 | 22.330697 | 150.58204074 | -13.26559499 | 258.6515 | 54136.6651388889 | 2007-02-05 15:57:48 | 54137.6043287037 | 2007-02-06 14:30:14 | 101012020 | 43.8714 | 40 | 43.8954 | 43.8794 | 0 | 43.8714 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.5732 | 41.5732 | 81.1379 | 1 | PROCESSED | 57537.3356944444 | 2016-05-29 08:03:24 | 53826 | 2006-04-01 00:00:00 | 54151.6542361111 | 2007-02-20 15:42:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101012020/ | Quick Look | ![]() |
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18 | JUPITER | 226.5694 | -16.1887 | 225.870685 | -15.99606 | 228.664382 | 1.239883 | 343.96536778 | 35.7224308 | 118.4901 | 53790.7643402778 | 2006-02-24 18:20:39 | 53791.7940277778 | 2006-02-25 19:03:24 | 401001010 | 37.7594 | 36 | 37.7674 | 37.7594 | 37.7674 | 37.7674 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.8361 | 32.8361 | 88.9361 | 1 | PROCESSED | 57533.0781597222 | 2016-05-25 01:52:33 | 54401 | 2007-10-28 00:00:00 | 53905.533900463 | 2006-06-19 12:48:49 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001010/ | Quick Look | ![]() |
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19 | COMA CLUSTER OFFSET | 194.6939 | 27.9466 | 194.090146 | 28.216217 | 181.281218 | 31.269541 | 60.06105128 | 88.1791818 | 318.0815 | 53885.0996412037 | 2006-05-30 02:23:29 | 53886.8384722222 | 2006-05-31 20:07:24 | 801044010 | 79.172 | 80 | 79.172 | 79.172 | 79.172 | 79.172 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.2282 | 75.2282 | 150.2049 | 2 | PROCESSED | 57534.5195949074 | 2016-05-26 12:28:13 | 54394 | 2007-10-21 00:00:00 | 53926.7587384259 | 2006-07-10 18:12:35 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010091 | In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801044010/ | Quick Look | ![]() |
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20 | SS 433 | 287.9527 | 4.99 | 287.334904 | 4.905608 | 290.182673 | 27.181461 | 39.69879316 | -2.23786427 | 78.6446 | 53833.4611458333 | 2006-04-08 11:04:03 | 53834.4579166667 | 2006-04-09 10:59:24 | 401004010 | 40.1976 | 40 | 40.2216 | 40.1976 | 40.2296 | 40.2136 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.4749 | 30.4749 | 86.11 | 2 | PROCESSED | 57533.4357638889 | 2016-05-25 10:27:30 | 54400 | 2007-10-27 00:00:00 | 53906.5501736111 | 2006-06-20 13:12:15 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010031 | SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. | GALACTIC POINT SOURCES | 4 | A | NOBUYUKI KAWAI | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401004010/ | Quick Look | ![]() |
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21 | MRK 1073 | 48.7759 | 41.9723 | 47.948749 | 41.787366 | 57.835678 | 23.02641 | 149.56255257 | -13.3516285 | 258.3737 | 54135.7651851852 | 2007-02-04 18:21:52 | 54136.6641087963 | 2007-02-05 15:56:19 | 701007020 | 39.5111 | 40 | 39.5191 | 39.5111 | 0 | 39.5191 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.1814 | 37.1814 | 77.6519 | 0 | PROCESSED | 57537.3263657407 | 2016-05-29 07:49:58 | 54735 | 2008-09-26 00:00:00 | 54151.4969444445 | 2007-02-20 11:55:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007020/ | Quick Look | ![]() |
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22 | 1E1207.4-5209 | 182.4916 | -52.442 | 181.83735 | -52.163724 | 209.144209 | -45.784625 | 296.53791481 | 9.91413144 | 148.6893 | 54146.2087384259 | 2007-02-15 05:00:35 | 54147.6390509259 | 2007-02-16 15:20:14 | 401030020 | 49.8266 | 50 | 50.0734 | 49.8266 | 0 | 50.0894 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 44.4468 | 44.4468 | 123.576 | 2 | PROCESSED | 57537.4372337963 | 2016-05-29 10:29:37 | 54750 | 2008-10-11 00:00:00 | 54153.9886458333 | 2007-02-22 23:43:39 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010152 | 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. | GALACTIC POINT SOURCES | 4 | B | ATSUMASA YOSHIDA | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030020/ | Quick Look | ![]() |
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23 | HR 9024 | 357.4125 | 36.4308 | 356.782155 | 36.152799 | 14.165064 | 34.009987 | 109.27773456 | -24.79729068 | 49.8624 | 53939.0616782407 | 2006-07-23 01:28:49 | 53940.6016087963 | 2006-07-24 14:26:19 | 401032010 | 58.7757 | 60 | 58.7997 | 58.7757 | 58.7837 | 58.7917 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56.0116 | 56.0116 | 133.0398 | 1 | PROCESSED | 57535.042025463 | 2016-05-27 01:00:31 | 54401 | 2007-10-28 00:00:00 | 53950.2624074074 | 2006-08-03 06:17:52 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011022 | Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. | GALACTIC POINT SOURCES | 4 | B | PAOLA TESTA | USA | 1 | AO1 | GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401032010/ | Quick Look | ![]() |
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24 | BETA LYR | 282.5098 | 33.3716 | 282.047998 | 33.312385 | 288.857806 | 55.996493 | 63.19266924 | 14.79477853 | 53.4974 | 53867.1260185185 | 2006-05-12 03:01:28 | 53867.6252199074 | 2006-05-12 15:00:19 | 401036020 | 21.4962 | 20 | 21.4962 | 21.4962 | 21.4962 | 21.4962 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.1642 | 19.1642 | 43.1199 | 2 | PROCESSED | 57534.2764814815 | 2016-05-26 06:38:08 | 54401 | 2007-10-28 00:00:00 | 53914.2784143518 | 2006-06-28 06:40:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036020/ | Quick Look | ![]() |
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25 | 4U 1705-44 | 257.2295 | -44.1004 | 256.326357 | -44.0367 | 260.194477 | -21.092135 | 343.32321952 | -2.34240238 | 264.0794 | 53976.2429166667 | 2006-08-29 05:49:48 | 53976.7731712963 | 2006-08-29 18:33:22 | 401046010 | 18.3155 | 20 | 18.3155 | 18.3155 | 18.3155 | 18.3155 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15.3715 | 15.3715 | 45.8099 | 0 | PROCESSED | 57535.3889236111 | 2016-05-27 09:20:03 | 54526 | 2008-03-01 00:00:00 | 54021.306087963 | 2006-10-13 07:20:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046010/ | Quick Look | ![]() |
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26 | 4U 1636-536 | 250.2262 | -53.7541 | 249.22979 | -53.657603 | 256.460667 | -31.236861 | 332.91086545 | -4.81751491 | 91.2457 | 54140.3877546296 | 2007-02-09 09:18:22 | 54140.99125 | 2007-02-09 23:47:24 | 401050010 | 24.232 | 19 | 24.232 | 24.232 | 0 | 24.232 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 21.6895 | 21.6895 | 52.136 | 0 | PROCESSED | 57537.3410069445 | 2016-05-29 08:11:03 | 54525 | 2008-02-29 00:00:00 | 54151.5052893518 | 2007-02-20 12:07:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050010/ | Quick Look | ![]() |
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27 | IGRJ16195-4945 | 244.8541 | -49.816 | 243.916706 | -49.695602 | 251.909406 | -27.940354 | 333.49117084 | 0.29973526 | 284.0301 | 53998.8508333333 | 2006-09-20 20:25:12 | 53999.7231481482 | 2006-09-21 17:21:20 | 401056010 | 39.1486 | 40 | 39.1486 | 39.1486 | 39.1486 | 39.1486 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.2652 | 42.2652 | 75.3579 | 1 | PROCESSED | 57535.652662037 | 2016-05-27 15:39:50 | 54526 | 2008-03-01 00:00:00 | 54020.9227199074 | 2006-10-12 22:08:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401056010/ | Quick Look | ![]() |
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28 | CYGNUS X-1 | 299.6124 | 35.133 | 299.141904 | 34.996436 | 313.652571 | 54.178807 | 71.28577556 | 3.01567368 | 256.2202 | 54038.1501273148 | 2006-10-30 03:36:11 | 54038.8225 | 2006-10-30 19:44:24 | 401059010 | 27.7068 | 30 | 27.7068 | 27.7378 | 27.7068 | 27.7068 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 27.6892 | 27.6892 | 58.0839 | 0 | PROCESSED | 57535.9949768518 | 2016-05-27 23:52:46 | 54526 | 2008-03-01 00:00:00 | 54063.4924884259 | 2006-11-24 11:49:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011141 | We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | B | MICHAEL NOWAK | USA | 1 | AO1 | ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401059010/ | Quick Look | ![]() |
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29 | CYGNUS LOOP | 314.0133 | 31.992 | 313.497685 | 31.799479 | 329.365567 | 46.782128 | 75.70987313 | -8.56406979 | 213.2117 | 54090.6869791667 | 2006-12-21 16:29:15 | 54091.1175231482 | 2006-12-22 02:49:14 | 101013020 | 21.004 | 20 | 21.004 | 21.004 | 0 | 21.004 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.8719 | 18.8719 | 37.168 | 1 | PROCESSED | 57536.3885185185 | 2016-05-28 09:19:28 | 53826 | 2006-04-01 00:00:00 | 54132.7085763889 | 2007-02-01 17:00:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013020/ | Quick Look | ![]() |
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30 | LOCKMAN HOLE | 162.9366 | 57.2557 | 162.165538 | 57.521221 | 137.120397 | 45.113941 | 149.70344314 | 53.20093146 | 281.8721 | 53872.7389583333 | 2006-05-17 17:44:06 | 53874.7939583333 | 2006-05-19 19:03:18 | 101002010 | 80.3982 | 80 | 80.3982 | 80.4062 | 80.4062 | 80.4062 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 88.854 | 88.854 | 177.5138 | 4 | PROCESSED | 57534.3694212963 | 2016-05-26 08:51:58 | 53826 | 2006-04-01 00:00:00 | 53927.7689814815 | 2006-07-11 18:27:20 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015003 | We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD. | CALIBRATION | 1 | A | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | SUZAKU OBSERVATION OF LOCKMANHOLE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101002010/ | Quick Look | ![]() |
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31 | E0102.2-7219 | 15.9824 | -72.0369 | 15.577154 | -72.304907 | 314.598987 | -65.033002 | 301.56901677 | -45.05828014 | 133.8232 | 53972.2052662037 | 2006-08-25 04:55:35 | 53973.3933333333 | 2006-08-26 09:26:24 | 101005050 | 68.3632 | 20 | 68.9872 | 68.3632 | 68.9872 | 68.9712 | 5 | 5 | 5 | 6 | 1 | 0 | 0 | 68.0024 | 68.0024 | 102.6339 | 1 | PROCESSED | 57535.3618402778 | 2016-05-27 08:41:03 | 53826 | 2006-04-01 00:00:00 | 54020.9929050926 | 2006-10-12 23:49:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005050/ | Quick Look | ![]() |
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32 | E0102.2-7219 | 16.0273 | -72.0256 | 15.62255 | -72.293547 | 314.637137 | -65.04077 | 301.54834682 | -45.06859544 | 302.8131 | 54141.9262384259 | 2007-02-10 22:13:47 | 54142.812662037 | 2007-02-11 19:30:14 | 101005110 | 36.0938 | 20 | 36.1018 | 36.0938 | 0 | 36.1018 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 52.7038 | 52.7038 | 76.5759 | 1 | PROCESSED | 57537.3567592593 | 2016-05-29 08:33:44 | 53826 | 2006-04-01 00:00:00 | 54153.2227430556 | 2007-02-22 05:20:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005110/ | Quick Look | ![]() |
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33 | THE CRAB OFFSETS | 83.7241 | 22.023 | 82.971763 | 21.990753 | 84.183875 | -1.291252 | 184.59560566 | -5.70852703 | 87.5484 | 53997.1534490741 | 2006-09-19 03:40:58 | 53997.2154513889 | 2006-09-19 05:10:15 | 101011100 | 1.545 | 2 | 1.545 | 1.545 | 1.545 | 1.545 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.806 | 1.806 | 5.356 | 0 | PROCESSED | 57535.619537037 | 2016-05-27 14:52:08 | 53826 | 2006-04-01 00:00:00 | 54104.4337731482 | 2007-01-04 10:24:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011100/ | Quick Look | ![]() |
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34 | NGC 5044 OFFSET1 | 198.8505 | -16.143 | 198.184446 | -15.87899 | 203.499232 | -7.562902 | 311.28196707 | 46.33985641 | 290.0004 | 53919.3604398148 | 2006-07-03 08:39:02 | 53920.9599305556 | 2006-07-04 23:02:18 | 801047010 | 54.6204 | 60 | 54.6204 | 54.6204 | 54.6204 | 54.6204 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.8033 | 45.8033 | 138.1899 | 1 | PROCESSED | 57534.8941203704 | 2016-05-26 21:27:32 | 54394 | 2007-10-21 00:00:00 | 53942.4615740741 | 2006-07-26 11:04:40 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801047010/ | Quick Look | ![]() |
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35 | GRB070328 | 65.0965 | -34.1127 | 64.627027 | -34.231006 | 53.193977 | -54.420072 | 235.19366633 | -44.98909931 | 291.3415 | 54187.3163773148 | 2007-03-28 07:35:35 | 54188.4585416667 | 2007-03-29 11:00:18 | 901005010 | 52.5653 | 40 | 52.5653 | 52.5653 | 0 | 52.5653 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.2428 | 48.2428 | 98.6819 | 2 | PROCESSED | 57538.0113888889 | 2016-05-30 00:16:24 | 54187 | 2007-03-28 00:00:00 | 54209.5955324074 | 2007-04-19 14:17:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017004 | TOO Observation of GRB 070328, REPORTED BY GCN 6224 | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SUZAKU GRB TEAM | JAP | 1 | TOO | TOO OBSERVATION OF GRB 070328 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901005010/ | Quick Look | ![]() |
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36 | A1831 | 209.8007 | 27.9693 | 209.233208 | 28.211522 | 195.74505 | 37.218341 | 40.05378223 | 74.96810077 | 288.1207 | 53937.1181828704 | 2006-07-21 02:50:11 | 53937.5106481482 | 2006-07-21 12:15:20 | 801077010 | 18.0796 | 18 | 18.0796 | 18.0796 | 18.0796 | 18.0796 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.0891 | 17.0891 | 33.8979 | 1 | PROCESSED | 57535.0011805556 | 2016-05-27 00:01:42 | 54401 | 2007-10-28 00:00:00 | 53943.553599537 | 2006-07-27 13:17:11 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/ | Quick Look | ![]() |
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37 | A1674 | 195.9676 | 67.5471 | 195.510877 | 67.814977 | 143.551001 | 62.83408 | 121.10331631 | 49.53698634 | 114.9985 | 54085.1434837963 | 2006-12-16 03:26:37 | 54087.0426388889 | 2006-12-18 01:01:24 | 801062010 | 68.4138 | 100 | 68.4218 | 68.4218 | 0 | 68.4138 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.0131 | 109.0131 | 164.064 | 2 | PROCESSED | 57536.3777546296 | 2016-05-28 09:03:58 | 54750 | 2008-10-11 00:00:00 | 54094.6003935185 | 2006-12-25 14:24:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010156 | A1674 is a nearby (z=0.106) richness class 3 clsuter with Abell galaxy count of 165, while its X-ray luminsity is as low as 6e43erg/s. We have observed this cluster with ASCA and XMM-Newton, and found iregular extended X-ray emission. The X-ray spectrum can be fitted with a thin thermal model of kT ~ 3keV, but the metal abundance is 0.07 with upper limit of 0.2. We assume this cluster may be a cluster under construction. Utilizing the low background level and high sensitivity of Suzaku XIS, we aim to obtain accurate X-ray spectrum of this cluster to constrain the metal abndance of each species. We also examine possible contribution of diffuse non-thermal emission in cluster scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801062010/ | Quick Look | ![]() |
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38 | CYGNUS_LOOP_P8 | 313.9965 | 31.4722 | 313.478406 | 31.279742 | 329.042886 | 46.311836 | 75.29540263 | -8.88432445 | 62.5181 | 53868.0059837963 | 2006-05-13 00:08:37 | 53868.1717476852 | 2006-05-13 04:07:19 | 501028010 | 4.8706 | 6 | 4.8706 | 4.8706 | 4.8706 | 4.8706 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.328 | 2.328 | 14.316 | 0 | PROCESSED | 57534.2851736111 | 2016-05-26 06:50:39 | 54394 | 2007-10-21 00:00:00 | 53914.3326157407 | 2006-06-28 07:58:58 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501028010/ | Quick Look | ![]() |
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39 | A1800 | 207.3618 | 28.0973 | 206.789109 | 28.345144 | 193.256107 | 36.394356 | 40.59651819 | 77.12066844 | 302.3644 | 53936.635625 | 2006-07-20 15:15:18 | 53937.1140509259 | 2006-07-21 02:44:14 | 801078010 | 20.0437 | 17 | 20.0473 | 20.0553 | 20.0553 | 20.0437 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.0003 | 19.0003 | 41.3319 | 0 | PROCESSED | 57535.0036458333 | 2016-05-27 00:05:15 | 54401 | 2007-10-28 00:00:00 | 53943.5299652778 | 2006-07-27 12:43:09 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/ | Quick Look | ![]() |
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40 | GC_SGR_B_EAST | 267.0203 | -28.3518 | 266.229607 | -28.335406 | 267.358668 | -4.938031 | 0.77973231 | -0.1584432 | 71.8708 | 54162.5141203704 | 2007-03-03 12:20:20 | 54164.5273726852 | 2007-03-05 12:39:25 | 501039010 | 96.4018 | 100 | 96.4018 | 96.4018 | 0 | 96.4018 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.0829 | 91.0829 | 173.9318 | 3 | PROCESSED | 57537.6522800926 | 2016-05-29 15:39:17 | 54736 | 2008-09-27 00:00:00 | 54171.4429050926 | 2007-03-12 10:37:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501039010/ | Quick Look | ![]() |
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41 | CYGNUS X-3 | 308.2593 | 40.981 | 307.808438 | 40.809488 | 328.80084 | 56.880196 | 79.93230299 | 0.62160244 | 252.424 | 54052.0902893518 | 2006-11-13 02:10:01 | 54054.3676388889 | 2006-11-15 08:49:24 | 401011010 | 99.7445 | 100 | 99.7462 | 99.7462 | 0 | 99.7445 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.3893 | 95.3893 | 196.745 | 1 | PROCESSED | 57536.1520717593 | 2016-05-28 03:38:59 | 54456 | 2007-12-22 00:00:00 | 54088.9545023148 | 2006-12-19 22:54:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010058 | We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3. | GALACTIC POINT SOURCES | 4 | C | SHUNJI KITAMOTO | JAP | 1 | AO1 | WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU | SPE | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401011010/ | Quick Look | ![]() |
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42 | A2665 | 357.7161 | 6.1352 | 357.076736 | 5.857083 | 0.350497 | 6.536022 | 96.94047732 | -53.65177278 | 245.9817 | 54078.2252893518 | 2006-12-09 05:24:25 | 54078.562037037 | 2006-12-09 13:29:20 | 801076010 | 13.944 | 15 | 13.944 | 13.944 | 0 | 13.944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.6073 | 11.6073 | 29.0879 | 0 | PROCESSED | 57536.2715393518 | 2016-05-28 06:31:01 | 54695 | 2008-08-17 00:00:00 | 54089.271412037 | 2006-12-20 06:30:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/ | Quick Look | ![]() |
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43 | DRACO HVC REGION B | 243.9603 | 59.1738 | 243.739297 | 59.296448 | 199.753416 | 76.165002 | 90.07720195 | 42.68363475 | 80.282 | 53816.0059953704 | 2006-03-22 00:08:38 | 53817.4148611111 | 2006-03-23 09:57:24 | 501005010 | 61.632 | 60 | 61.6447 | 61.644 | 61.632 | 61.636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.6865 | 60.6865 | 121.7099 | 2 | PROCESSED | 57533.3166319444 | 2016-05-25 07:35:57 | 54400 | 2007-10-27 00:00:00 | 53906.4964583333 | 2006-06-20 11:54:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010069 | High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501005010/ | Quick Look | ![]() |
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44 | CYGNUS_LOOP_P9 | 311.8173 | 30.594 | 311.299257 | 30.409327 | 326.059392 | 46.235255 | 73.41991066 | -7.98099126 | 239.9998 | 54416.7228935185 | 2007-11-12 17:20:58 | 54417.2502199074 | 2007-11-13 06:00:19 | 501019010 | 19.5656 | 15 | 19.5656 | 19.5656 | 0 | 19.5656 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.3446 | 17.3446 | 45.5379 | 0 | PROCESSED | 57540.4965393518 | 2016-06-01 11:55:01 | 54798 | 2008-11-28 00:00:00 | 54430.2327546296 | 2007-11-26 05:35:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501019010/ | Quick Look | ![]() |
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45 | THE CRAB OFFSETS | 83.5056 | 22.0085 | 82.753398 | 21.975199 | 83.980807 | -1.296775 | 184.49889553 | -5.88737418 | 85.6939 | 53984.8892708333 | 2006-09-06 21:20:33 | 53984.935 | 2006-09-06 22:26:24 | 101011160 | 2.7651 | 2 | 2.7651 | 2.7651 | 2.7651 | 2.7651 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.152 | 2.152 | 3.9439 | 0 | PROCESSED | 57535.4827083333 | 2016-05-27 11:35:06 | 53826 | 2006-04-01 00:00:00 | 54104.4508449074 | 2007-01-04 10:49:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011160/ | Quick Look | ![]() |
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46 | PKS 2356-61 | 359.7661 | -60.908 | 359.120501 | -61.186478 | 324.284485 | -53.222548 | 314.02525269 | -55.07790138 | 249.6445 | 54075.7140740741 | 2006-12-06 17:08:16 | 54078.21625 | 2006-12-09 05:11:24 | 801016010 | 100.8372 | 100 | 100.8452 | 100.8372 | 0 | 100.8532 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.1255 | 92.1255 | 216.1579 | 3 | PROCESSED | 57536.3143171296 | 2016-05-28 07:32:37 | 54456 | 2007-12-22 00:00:00 | 54088.6546759259 | 2006-12-19 15:42:44 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010059 | We propose a 100 ksec Suzaku observation of the radio galaxy PKS 2356-61. PKS 2356-61 is reported to reside in a group of galaxies, and a sign of a diffuse X-ray emission with a possibly high temperature surrounding PKS 2356-61 was suggested with ASCA. Our objective is the determination of the origin of the diffuse emission to evaluate AGN heating of the intragroup gas by PKS 2356-61. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SOOJING HONG | JAP | 1 | AO1 | HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801016010/ | Quick Look | ![]() |
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47 | CRAB | 83.6569 | 21.9577 | 82.904946 | 21.92513 | 84.118749 | -1.353767 | 184.61755594 | -5.79610428 | 250.9424 | 53830.5463425926 | 2006-04-05 13:06:44 | 53831.5925115741 | 2006-04-06 14:13:13 | 101003010 | 37.8323 | 40 | 37.8323 | 37.8533 | 37.8323 | 37.8323 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 30.989 | 30.989 | 90.3799 | 1 | PROCESSED | 57533.4323726852 | 2016-05-25 10:22:37 | 53826 | 2006-04-01 00:00:00 | 53907.1306944445 | 2006-06-21 03:08:12 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101003010/ | Quick Look | ![]() |
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48 | CRAB | 83.6371 | 22.0108 | 82.884853 | 21.978134 | 84.10274 | -1.299909 | 184.56259415 | -5.78319491 | 253.3318 | 53824.652650463 | 2006-03-30 15:39:49 | 53825.1668865741 | 2006-03-31 04:00:19 | 101004010 | 16.3632 | 20 | 16.3632 | 16.3728 | 16.365 | 16.365 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.7616 | 9.7616 | 44.426 | 0 | PROCESSED | 57533.3378009259 | 2016-05-25 08:06:26 | 53826 | 2006-04-01 00:00:00 | 53906.0621875 | 2006-06-20 01:29:33 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101004010/ | Quick Look | ![]() |
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49 | GALACTIC CENTER | 265.3803 | -29.7558 | 264.581055 | -29.731436 | 265.955939 | -6.379444 | 358.83357751 | 0.33021849 | 269 | 54016.4324074074 | 2006-10-08 10:22:40 | 54017.0968055556 | 2006-10-09 02:19:24 | 501049010 | 19.5627 | 20 | 19.5627 | 19.5627 | 19.5627 | 19.5627 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.6336 | 17.6336 | 57.3959 | 1 | PROCESSED | 57535.7944675926 | 2016-05-27 19:04:02 | 54735 | 2008-09-26 00:00:00 | 54053.4403356482 | 2006-11-14 10:34:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501049010/ | Quick Look | ![]() |
50 | HER X-1 | 254.4224 | 35.4083 | 253.972328 | 35.484085 | 245.910127 | 57.551397 | 58.22535664 | 37.56185232 | 67.8783 | 53823.7669907407 | 2006-03-29 18:24:28 | 53824.640462963 | 2006-03-30 15:22:16 | 101001010 | 33.0621 | 40 | 33.0621 | 38.8045 | 33.0621 | 33.0701 | 4 | 3 | 4 | 4 | 1 | 0 | 0 | 26.2228 | 26.2228 | 75.4379 | 0 | PROCESSED | 57526.8178703704 | 2016-05-18 19:37:44 | 53826 | 2006-04-01 00:00:00 | 53906.9875925926 | 2006-06-20 23:42:08 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015002 | The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO. | CALIBRATION | 1 | A | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATION | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101001010/ | Quick Look | ![]() |
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51 | RCW 86 | 221.2555 | -62.3618 | 220.269135 | -62.150858 | 241.140538 | -43.714444 | 315.68741681 | -2.33681001 | 278.3377 | 53959.4574652778 | 2006-08-12 10:58:45 | 53961.1294907407 | 2006-08-14 03:06:28 | 501037010 | 59.8054 | 60 | 59.8294 | 59.8054 | 59.8294 | 59.8214 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.405 | 54.405 | 144.42 | 1 | PROCESSED | 57535.2984259259 | 2016-05-27 07:09:44 | 54394 | 2007-10-21 00:00:00 | 54021.0740972222 | 2006-10-13 01:46:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010054 | We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | JAP | 1 | AO1 | RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501037010/ | Quick Look | ![]() |
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52 | E0102.2-7219 | 16.0029 | -72.0223 | 15.597746 | -72.29028 | 314.636668 | -65.03255 | 301.55865958 | -45.07240987 | 252.2709 | 54082.7869907407 | 2006-12-13 18:53:16 | 54083.1279976852 | 2006-12-14 03:04:19 | 101005090 | 28.226 | 20 | 28.226 | 28.226 | 0 | 28.226 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23.0546 | 23.0546 | 29.4559 | 0 | PROCESSED | 57536.3258101852 | 2016-05-28 07:49:10 | 53826 | 2006-04-01 00:00:00 | 54094.5930324074 | 2006-12-25 14:13:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005090/ | Quick Look | ![]() |
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53 | CYGNUS LOOP | 314.0118 | 31.9912 | 313.496184 | 31.798684 | 329.363396 | 46.781909 | 75.70842949 | -8.56360013 | 217.4642 | 54090.3953935185 | 2006-12-21 09:29:22 | 54090.6848842593 | 2006-12-21 16:26:14 | 101013010 | 9.102 | 10 | 9.102 | 9.102 | 0 | 9.102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.2126 | 9.2126 | 25.006 | 1 | PROCESSED | 57536.373275463 | 2016-05-28 08:57:31 | 53826 | 2006-04-01 00:00:00 | 54108.4571990741 | 2007-01-08 10:58:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013010/ | Quick Look | ![]() |
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54 | 1E1207.4-5209 | 182.5062 | -52.436 | 181.851861 | -52.157726 | 209.149793 | -45.774623 | 296.5458403 | 9.92149786 | 302.4939 | 53946.5682060185 | 2006-07-30 13:38:13 | 53948.2603587963 | 2006-08-01 06:14:55 | 401030010 | 96.3519 | 120 | 96.3519 | 102.2784 | 96.3679 | 96.3519 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 94.0498 | 94.0498 | 135.3799 | 1 | PROCESSED | 57535.1230787037 | 2016-05-27 02:57:14 | 54750 | 2008-10-11 00:00:00 | 54132.8187268518 | 2007-02-01 19:38:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010152 | 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. | GALACTIC POINT SOURCES | 4 | B | ATSUMASA YOSHIDA | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401030010/ | Quick Look | ![]() |
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55 | AB DOR | 82.2835 | -65.427 | 82.246883 | -65.464502 | 16.282788 | -86.671062 | 275.26967334 | -33.00819219 | 154.6774 | 54060.0265277778 | 2006-11-21 00:38:12 | 54061.4586111111 | 2006-11-22 11:00:24 | 401031010 | 53.4517 | 80 | 53.4517 | 53.4597 | 0 | 53.4614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.0334 | 48.0334 | 123.708 | 1 | PROCESSED | 57536.170462963 | 2016-05-28 04:05:28 | 54502 | 2008-02-06 00:00:00 | 54133.0222916667 | 2007-02-02 00:32:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | MARC AUDARD | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031010/ | Quick Look | ![]() |
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56 | RXJ1713-3946 | 258.1672 | -39.4231 | 257.303004 | -39.36394 | 260.487659 | -16.371231 | 347.50735004 | -0.13585591 | 267.9988 | 53989.9221643518 | 2006-09-11 22:07:55 | 53990.3106712963 | 2006-09-12 07:27:22 | 501065010 | 22.011 | 20 | 22.011 | 22.011 | 22.011 | 22.011 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.7973 | 20.7973 | 33.5579 | 0 | PROCESSED | 57535.5534606482 | 2016-05-27 13:16:59 | 54526 | 2008-03-01 00:00:00 | 54020.8390162037 | 2006-10-12 20:08:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501065010/ | Quick Look | ![]() |
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57 | GC SGR D | 267.0913 | -27.9356 | 266.303192 | -27.919557 | 267.412914 | -4.520645 | 1.16847417 | 0.00287016 | 108.7996 | 54174.7887847222 | 2007-03-15 18:55:51 | 54176.2127199074 | 2007-03-17 05:06:19 | 501059010 | 62.2372 | 63 | 62.2372 | 62.2452 | 0 | 62.2452 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.3697 | 54.3697 | 123.028 | 0 | PROCESSED | 57537.7233912037 | 2016-05-29 17:21:41 | 54736 | 2008-09-27 00:00:00 | 54185.4865740741 | 2007-03-26 11:40:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501059010/ | Quick Look | ![]() |
58 | M106 | 184.7117 | 47.2376 | 184.094273 | 47.515109 | 160.404745 | 44.085185 | 138.43381178 | 68.89762168 | 287.1938 | 53896.5413078704 | 2006-06-10 12:59:29 | 53898.7113425926 | 2006-06-12 17:04:20 | 701095010 | 99.8175 | 100 | 99.8815 | 99.8175 | 99.8815 | 99.8815 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 97.5229 | 97.5229 | 187.4839 | 1 | PROCESSED | 57534.6515393518 | 2016-05-26 15:38:13 | 54401 | 2007-10-28 00:00:00 | 53927.2308449074 | 2006-07-11 05:32:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013151 | We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKESHI ITOH | CHRISTOPHER REYNOLDS | JUS | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701095010/ | Quick Look | ![]() |
59 | CYGNUS_LOOP_P17 | 312.199 | 30.014 | 311.677424 | 29.82795 | 326.178147 | 45.573278 | 73.16561663 | -8.59879153 | 61.9999 | 53877.7613657407 | 2006-05-22 18:16:22 | 53878.0446064815 | 2006-05-23 01:04:14 | 501034010 | 14.1953 | 14 | 14.1993 | 14.2033 | 14.1993 | 14.1953 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.8231 | 14.8231 | 24.464 | 0 | PROCESSED | 57534.3944328704 | 2016-05-26 09:27:59 | 54394 | 2007-10-21 00:00:00 | 53926.1395833333 | 2006-07-10 03:21:00 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501034010/ | Quick Look | ![]() |
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60 | NGC 5044 OFFSET2 | 199.1117 | -16.388 | 198.444886 | -16.124395 | 203.827071 | -7.694393 | 311.59229028 | 46.06278821 | 290.7836 | 53920.9609143518 | 2006-07-04 23:03:43 | 53922.7598842593 | 2006-07-06 18:14:14 | 801048010 | 62.451 | 60 | 62.451 | 62.451 | 62.451 | 62.451 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57.1102 | 57.1102 | 155.3149 | 2 | PROCESSED | 57534.8962615741 | 2016-05-26 21:30:37 | 54422 | 2007-11-18 00:00:00 | 54034.2926736111 | 2006-10-26 07:01:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801048010/ | Quick Look | ![]() |
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61 | CYGNUS LOOP | 314.0129 | 31.9925 | 313.497288 | 31.79998 | 329.365408 | 46.782722 | 75.71004378 | -8.56348961 | 212.8468 | 54091.1180439815 | 2006-12-22 02:49:59 | 54091.6036342593 | 2006-12-22 14:29:14 | 101013030 | 19.7295 | 20 | 19.7295 | 19.7295 | 0 | 19.7295 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.1005 | 20.1005 | 41.9279 | 1 | PROCESSED | 57536.3931134259 | 2016-05-28 09:26:05 | 53826 | 2006-04-01 00:00:00 | 54132.7375694444 | 2007-02-01 17:42:06 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101013030/ | Quick Look | ![]() |
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62 | A2495 | 342.5777 | 10.9124 | 341.95313 | 10.647232 | 348.269753 | 16.897696 | 81.20126485 | -41.9387619 | 237.1467 | 54061.4694097222 | 2006-11-22 11:15:57 | 54062.0787037037 | 2006-11-23 01:53:20 | 801080010 | 18.0313 | 18 | 18.0313 | 18.3673 | 0 | 18.1193 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.3891 | 16.3891 | 52.6339 | 3 | PROCESSED | 57536.1381365741 | 2016-05-28 03:18:55 | 54695 | 2008-08-17 00:00:00 | 54088.9563194444 | 2006-12-19 22:57:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/ | Quick Look | ![]() |
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63 | E0102.2-7219 | 16.0331 | -72.0338 | 15.628552 | -72.301739 | 314.621321 | -65.04586 | 301.54662861 | -45.06029066 | 8.2024 | 53841.404212963 | 2006-04-16 09:42:04 | 53841.9793865741 | 2006-04-16 23:30:19 | 101005010 | 21.324 | 40 | 21.34 | 21.324 | 21.332 | 21.34 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 16.6831 | 16.6831 | 49.6639 | 0 | PROCESSED | 57533.4651273148 | 2016-05-25 11:09:47 | 53826 | 2006-04-01 00:00:00 | 53905.6938425926 | 2006-06-19 16:39:08 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005010/ | Quick Look | ![]() |
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64 | E0102.2-7219 | 16.0373 | -72.0314 | 15.632779 | -72.299334 | 314.627775 | -65.046019 | 301.54456169 | -45.06259438 | 341.0006 | 54177.8828587963 | 2007-03-18 21:11:19 | 54178.2994675926 | 2007-03-19 07:11:14 | 101005120 | 18.242 | 20 | 18.242 | 18.25 | 0 | 18.258 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.7551 | 14.7551 | 35.9839 | 0 | PROCESSED | 57537.6970601852 | 2016-05-29 16:43:46 | 53826 | 2006-04-01 00:00:00 | 54185.4459027778 | 2007-03-26 10:42:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005120/ | Quick Look | ![]() |
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65 | FORNAX A HOST GALAXY | 50.6684 | -37.2029 | 50.191244 | -37.380302 | 32.749558 | -53.117138 | 240.15407206 | -56.69497357 | 218.3809 | 54091.6179976852 | 2006-12-22 14:49:55 | 54092.8689699074 | 2006-12-23 20:51:19 | 801015010 | 48.7217 | 50 | 48.7217 | 48.7217 | 0 | 48.7217 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3987 | 48.3987 | 108.0839 | 1 | PROCESSED | 57536.4184837963 | 2016-05-28 10:02:37 | 54735 | 2008-09-26 00:00:00 | 54132.9200347222 | 2007-02-01 22:04:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010029 | We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO TASHIRO | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801015010/ | Quick Look | ![]() |
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66 | LMC X-2 | 80.025 | -71.9941 | 80.229686 | -72.041872 | 298.35324 | -83.539153 | 283.14092563 | -32.7117801 | 313.3022 | 53849.381712963 | 2006-04-24 09:09:40 | 53850.7731365741 | 2006-04-25 18:33:19 | 401012010 | 56.152 | 60 | 56.1657 | 56.1657 | 56.152 | 56.16 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 73.408 | 73.408 | 120.1938 | 1 | PROCESSED | 57533.5735300926 | 2016-05-25 13:45:53 | 54394 | 2007-10-21 00:00:00 | 53907.6288078704 | 2006-06-21 15:05:29 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010090 | We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not. | GALACTIC POINT SOURCES | 4 | B | HIROMITSU TAKAHASHI | JAP | 1 | AO1 | DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401012010/ | Quick Look | ![]() |
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67 | MRK 766 | 184.6154 | 29.8184 | 183.986779 | 30.095968 | 171.206094 | 28.943476 | 190.63186084 | 82.27243688 | 133.2599 | 54055.0242361111 | 2006-11-16 00:34:54 | 54057.363900463 | 2006-11-18 08:44:01 | 701035010 | 97.8693 | 150 | 98.1756 | 97.8693 | 0 | 98.1676 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.8931 | 96.8931 | 202.1299 | 2 | PROCESSED | 57536.189525463 | 2016-05-28 04:32:55 | 54800 | 2008-11-30 00:00:00 | 54132.8396990741 | 2007-02-01 20:09:10 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035010/ | Quick Look | ![]() |
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68 | MRK 1 | 19.06 | 33.0289 | 18.361574 | 32.765252 | 30.564721 | 23.029207 | 128.90716196 | -29.55492804 | 249.7486 | 54111.5318171296 | 2007-01-11 12:45:49 | 54114.5836111111 | 2007-01-14 14:00:24 | 701047010 | 126.4441 | 120 | 126.4441 | 126.4441 | 0 | 126.4441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 126.0122 | 126.0122 | 263.6237 | 2 | PROCESSED | 57637.5831944445 | 2016-09-06 13:59:48 | 54702 | 2008-08-24 00:00:00 | 54133.1552314815 | 2007-02-02 03:43:32 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011336 | The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NANCY LEVENSON | USA | 1 | AO1 | TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701047010/ | Quick Look | ![]() |
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69 | CYGNUS_LOOP_P10 | 311.5744 | 30.3992 | 311.055864 | 30.215413 | 325.67249 | 46.135207 | 73.13474548 | -7.93635975 | 240.0007 | 54417.2506944444 | 2007-11-13 06:01:00 | 54417.6043402778 | 2007-11-13 14:30:15 | 501020010 | 16.7958 | 10 | 16.7958 | 16.8198 | 0 | 16.8038 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6729 | 12.6729 | 30.5499 | 0 | PROCESSED | 57540.5008333333 | 2016-06-01 12:01:12 | 54798 | 2008-11-28 00:00:00 | 54430.1578472222 | 2007-11-26 03:47:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501020010/ | Quick Look | ![]() |
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70 | PUP A : INTERIOR | 125.5916 | -42.8951 | 125.161363 | -42.733897 | 147.106586 | -59.478577 | 260.333956 | -3.34905821 | 276.8883 | 53842.5813541667 | 2006-04-17 13:57:09 | 53842.9127199074 | 2006-04-17 21:54:19 | 501088010 | 20.2709 | 20 | 20.2924 | 20.2949 | 20.2789 | 20.2709 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.9519 | 19.9519 | 28.6239 | 0 | PROCESSED | 57533.5042476852 | 2016-05-25 12:06:07 | 54401 | 2007-10-28 00:00:00 | 53906.8948611111 | 2006-06-20 21:28:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501088010/ | Quick Look | ![]() |
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71 | NGC 4968 | 196.7464 | -23.7282 | 196.071371 | -23.461103 | 204.633939 | -15.321329 | 307.51234678 | 39.00523278 | 298.8345 | 53954.7307523148 | 2006-08-07 17:32:17 | 53955.6822222222 | 2006-08-08 16:22:24 | 701005010 | 39.0508 | 40 | 39.0508 | 39.0508 | 39.0508 | 39.0508 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.617 | 35.617 | 82.1979 | 1 | PROCESSED | 57535.2527546296 | 2016-05-27 06:03:58 | 54408 | 2007-11-04 00:00:00 | 54020.7898148148 | 2006-10-12 18:57:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701005010/ | Quick Look | ![]() |
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72 | Z235 | 10.9622 | 24.4059 | 10.298374 | 24.132304 | 19.875378 | 18.073678 | 120.72614401 | -38.43334342 | 59.0539 | 53944.0060185185 | 2006-07-28 00:08:40 | 53944.6148032407 | 2006-07-28 14:45:19 | 801083010 | 20.0335 | 20 | 20.0415 | 20.0415 | 20.0415 | 20.0335 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.5263 | 19.5263 | 52.5899 | 1 | PROCESSED | 57535.0666782407 | 2016-05-27 01:36:01 | 54401 | 2007-10-28 00:00:00 | 53955.6800925926 | 2006-08-08 16:19:20 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/ | Quick Look | ![]() |
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73 | GRB060904A | 237.7429 | 44.914 | 237.336952 | 45.063372 | 215.38839 | 62.37112 | 71.57699476 | 50.22047754 | 264.197 | 53982.4478935185 | 2006-09-04 10:44:58 | 53983.2113888889 | 2006-09-05 05:04:24 | 901001010 | 30.3363 | 30 | 30.3443 | 30.3363 | 30.3443 | 30.3443 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.347 | 28.347 | 65.966 | 0 | PROCESSED | 57535.45125 | 2016-05-27 10:49:48 | 53982 | 2006-09-04 00:00:00 | 54026.4650462963 | 2006-10-18 11:09:40 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017001 | N/A | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG GRB TEAM | JAP | 1 | TOO | TOO OBSERVATION OF GRB060904A | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901001010/ | Quick Look | ![]() |
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74 | SWIFTJ1010.1-5747 | 152.7309 | -57.8539 | 152.293849 | -57.606865 | 193.450641 | -60.897616 | 282.8705066 | -1.37559689 | 290.7012 | 53891.2175 | 2006-06-05 05:13:12 | 53891.5544560185 | 2006-06-05 13:18:25 | 401055010 | 19.1717 | 20 | 19.1717 | 19.1717 | 19.1717 | 19.1717 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.8778 | 17.8778 | 29.0879 | 0 | PROCESSED | 57534.4906944444 | 2016-05-26 11:46:36 | 54401 | 2007-10-28 00:00:00 | 53926.1075347222 | 2006-07-10 02:34:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401055010/ | Quick Look | ![]() |
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75 | JUPITER | 226.5948 | -16.1928 | 225.896045 | -16.000249 | 228.688969 | 1.24261 | 343.98613419 | 35.70433361 | 118.4906 | 53791.7941319445 | 2006-02-25 19:03:33 | 53792.7940277778 | 2006-02-26 19:03:24 | 401001020 | 37.704 | 36 | 37.704 | 37.704 | 37.704 | 37.704 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 32.7781 | 32.7781 | 86.36 | 1 | PROCESSED | 57533.0943981482 | 2016-05-25 02:15:56 | 54401 | 2007-10-28 00:00:00 | 53905.5035416667 | 2006-06-19 12:05:06 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001020/ | Quick Look | ![]() |
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76 | G11.2-0.3 | 272.8676 | 19.433 | 272.324919 | 19.420376 | 273.677117 | 42.836704 | 46.34586116 | 17.29738119 | 77.6432 | 53834.4626041667 | 2006-04-09 11:06:09 | 53835.6634143518 | 2006-04-10 15:55:19 | 401010010 | 43.9846 | 50 | 43.9926 | 43.9846 | 43.9926 | 43.9926 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.3879 | 37.3879 | 83.6799 | 1 | PROCESSED | 57533.4279166667 | 2016-05-25 10:16:12 | 54397 | 2007-10-24 00:00:00 | 53905.4671875 | 2006-06-19 11:12:45 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010049 | The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU. | GALACTIC POINT SOURCES | 4 | C | ASAMI HAYATO | JAP | 1 | AO1 | CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401010010/ | Quick Look | ![]() |
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77 | SIGMA^2 CRB | 243.6552 | 33.7881 | 243.181435 | 33.91264 | 231.394365 | 53.752123 | 54.56402364 | 46.14689859 | 281.1207 | 53969.4764467593 | 2006-08-22 11:26:05 | 53972.1925231482 | 2006-08-25 04:37:14 | 401034010 | 109.1604 | 110 | 109.1904 | 109.1604 | 109.1684 | 109.1764 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98.8376 | 98.8376 | 234.6539 | 3 | PROCESSED | 57535.3877777778 | 2016-05-27 09:18:24 | 54526 | 2008-03-01 00:00:00 | 54021.2578587963 | 2006-10-13 06:11:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011025 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD. | GALACTIC POINT SOURCES | 4 | B | ALEXANDER BROWN | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401034010/ | Quick Look | ![]() |
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78 | 4U 1820-30 | 275.9207 | -30.3623 | 275.117497 | -30.389079 | 275.135384 | -7.027059 | 2.78792233 | -7.91550172 | 265.9754 | 53992.9234606482 | 2006-09-14 22:09:47 | 53993.6605902778 | 2006-09-15 15:51:15 | 401047010 | 25.7008 | 37 | 25.7008 | 25.8109 | 25.7239 | 25.7148 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31.8782 | 31.8782 | 63.6339 | 1 | PROCESSED | 57535.6012962963 | 2016-05-27 14:25:52 | 54526 | 2008-03-01 00:00:00 | 54021.2227083333 | 2006-10-13 05:20:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | JON MILLER | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401047010/ | Quick Look | ![]() |
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79 | 4U 1636-536 | 250.2259 | -53.7533 | 249.229501 | -53.656802 | 256.460315 | -31.236099 | 332.911352 | -4.8168543 | 100.7755 | 54188.4720717593 | 2007-03-29 11:19:47 | 54188.7856944445 | 2007-03-29 18:51:24 | 401050050 | 12.2418 | 38 | 12.2498 | 12.2418 | 0 | 12.2498 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 11.804 | 11.804 | 27.088 | 0 | PROCESSED | 57537.9973148148 | 2016-05-29 23:56:08 | 54695 | 2008-08-17 00:00:00 | 54200.4687731482 | 2007-04-10 11:15:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050050/ | Quick Look | ![]() |
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80 | 4U1907+09 | 287.4013 | 9.8378 | 286.806482 | 9.755913 | 290.334973 | 32.058259 | 43.74739314 | 0.48531727 | 60.2599 | 53857.2580324074 | 2006-05-02 06:11:34 | 53858.7322222222 | 2006-05-03 17:34:24 | 401057010 | 58.4403 | 60 | 58.4403 | 58.4563 | 58.4483 | 58.4563 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.8215 | 38.8215 | 127.3539 | 1 | PROCESSED | 57533.6690509259 | 2016-05-25 16:03:26 | 54401 | 2007-10-28 00:00:00 | 53913.4367476852 | 2006-06-27 10:28:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011133 | We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''. | GALACTIC POINT SOURCES | 4 | A | KATJA POTTSCHMIDT | USA | 1 | AO1 | THE BROAD BAND SPECTRUM OF 4U1907+09 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401057010/ | Quick Look | ![]() |
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81 | HESS J1731-347 | 263.0179 | -34.7706 | 262.185573 | -34.73474 | 264.142481 | -11.47104 | 353.53173388 | -0.68198005 | 79.8005 | 54154.7807060185 | 2007-02-23 18:44:13 | 54155.7432291667 | 2007-02-24 17:50:15 | 401099010 | 40.6189 | 38 | 40.6269 | 40.6189 | 0 | 40.6269 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6479 | 34.6479 | 83.1559 | 0 | PROCESSED | 57537.4739351852 | 2016-05-29 11:22:28 | 54528 | 2008-03-03 00:00:00 | 54160.3931944444 | 2007-03-01 09:26:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012042 | The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator. | GALACTIC POINT SOURCES | 4 | A | GERD PUEHLHOFER | EUR | 1 | AO1 | THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401099010/ | Quick Look | ![]() |
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82 | A2572B | 349.6066 | 18.7294 | 348.98329 | 18.45586 | 358.210513 | 21.259827 | 94.21850787 | -38.90117923 | 59.1565 | 53922.7742939815 | 2006-07-06 18:34:59 | 53923.3002199074 | 2006-07-07 07:12:19 | 801073010 | 24.0595 | 21 | 24.0755 | 24.0595 | 24.0675 | 24.0755 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.4951 | 21.4951 | 45.3979 | 1 | PROCESSED | 57534.8583912037 | 2016-05-26 20:36:05 | 54401 | 2007-10-28 00:00:00 | 53930.6043055556 | 2006-07-14 14:30:12 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/ | Quick Look | ![]() |
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83 | IC 443 | 94.2972 | 22.4797 | 93.541644 | 22.498727 | 93.972502 | -0.901975 | 189.13057055 | 2.97563306 | 274.0001 | 54166.5158680556 | 2007-03-07 12:22:51 | 54167.612025463 | 2007-03-08 14:41:19 | 501006020 | 44.0135 | 40 | 44.0135 | 44.0375 | 0 | 44.0215 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.3209 | 36.3209 | 94.6999 | 1 | PROCESSED | 57537.6255324074 | 2016-05-29 15:00:46 | 54736 | 2008-09-27 00:00:00 | 54172.2247800926 | 2007-03-13 05:23:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010040 | IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. | GALACTIC DIFFUSE EMISSION | 5 | B | MASANOBU OZAKI | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006020/ | Quick Look | ![]() |
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84 | THE CRAB OFFSETS | 83.6274 | 22.0499 | 82.874936 | 22.017186 | 84.09548 | -1.260449 | 184.52456216 | -5.76985767 | 85.719 | 53984.0906018518 | 2006-09-06 02:10:28 | 53984.1529976852 | 2006-09-06 03:40:19 | 101011040 | 3.353 | 2 | 3.353 | 3.353 | 3.353 | 3.353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.414 | 2.414 | 5.3839 | 0 | PROCESSED | 57535.4661921296 | 2016-05-27 11:11:19 | 53826 | 2006-04-01 00:00:00 | 54104.4143518518 | 2007-01-04 09:56:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011040/ | Quick Look | ![]() |
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85 | IC 443 | 94.2975 | 22.7757 | 93.54026 | 22.794725 | 93.963954 | -0.606095 | 188.8694635 | 3.11574616 | 274.0004 | 54165.4446643518 | 2007-03-06 10:40:19 | 54166.5154398148 | 2007-03-07 12:22:14 | 501006010 | 42.0113 | 40 | 42.0113 | 42.0129 | 0 | 42.0209 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6934 | 34.6934 | 92.5099 | 2 | PROCESSED | 57537.6197337963 | 2016-05-29 14:52:25 | 54736 | 2008-09-27 00:00:00 | 54174.6613541667 | 2007-03-15 15:52:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010040 | IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. | GALACTIC DIFFUSE EMISSION | 5 | B | MASANOBU OZAKI | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501006010/ | Quick Look | ![]() |
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86 | CYGNUS_LOOP_P1 | 313.519 | 31.9657 | 313.004288 | 31.774919 | 328.788742 | 46.92673 | 75.41990185 | -8.25713566 | 240 | 54417.6059259259 | 2007-11-13 14:32:32 | 54418.0904976852 | 2007-11-14 02:10:19 | 501012010 | 16.7385 | 10 | 16.7385 | 16.7489 | 0 | 16.7425 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.7758 | 15.7758 | 41.86 | 1 | PROCESSED | 57540.5110648148 | 2016-06-01 12:15:56 | 54798 | 2008-11-28 00:00:00 | 54430.2159375 | 2007-11-26 05:10:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501012010/ | Quick Look | ![]() |
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87 | CYGNUS_LOOP_P4 | 312.8083 | 31.361 | 312.292075 | 31.17275 | 327.627486 | 46.612051 | 74.56035476 | -8.16867105 | 239.9997 | 54418.9382291667 | 2007-11-14 22:31:03 | 54419.3196643518 | 2007-11-15 07:40:19 | 501015010 | 18.279 | 15 | 18.287 | 18.279 | 0 | 18.287 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.286 | 14.286 | 32.9439 | 0 | PROCESSED | 57540.5253935185 | 2016-06-01 12:36:34 | 54798 | 2008-11-28 00:00:00 | 54430.2398726852 | 2007-11-26 05:45:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501015010/ | Quick Look | ![]() |
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88 | CYGNUS_LOOP_P5 | 312.5567 | 31.1701 | 312.040041 | 30.982753 | 327.230821 | 46.520779 | 74.2739834 | -8.12038976 | 239.9995 | 54419.3201388889 | 2007-11-15 07:41:00 | 54420.0627777778 | 2007-11-16 01:30:24 | 501016010 | 28.4062 | 22 | 28.4062 | 28.4062 | 0 | 28.4062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.37 | 25.37 | 64.1559 | 1 | PROCESSED | 57540.538900463 | 2016-06-01 12:56:01 | 54798 | 2008-11-28 00:00:00 | 54430.4318865741 | 2007-11-26 10:21:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501016010/ | Quick Look | ![]() |
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89 | CYGNUS_LOOP_P6 | 312.3057 | 30.9823 | 311.788615 | 30.795857 | 326.837045 | 46.431585 | 73.99029438 | -8.06939848 | 240.0003 | 54415.3923032407 | 2007-11-11 09:24:55 | 54416.1668287037 | 2007-11-12 04:00:14 | 501017010 | 28.7049 | 22 | 28.7049 | 28.7049 | 0 | 28.7049 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.8878 | 26.8878 | 66.9119 | 0 | PROCESSED | 57540.490474537 | 2016-06-01 11:46:17 | 54798 | 2008-11-28 00:00:00 | 54430.18875 | 2007-11-26 04:31:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501017010/ | Quick Look | ![]() |
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90 | CYGNUS_LOOP_P16 | 312.737 | 30.4592 | 312.216541 | 30.271212 | 327.037451 | 45.805605 | 73.81069789 | -8.68546284 | 61.9998 | 53877.1905439815 | 2006-05-22 04:34:23 | 53877.7605671296 | 2006-05-22 18:15:13 | 501033010 | 23.3375 | 22 | 23.3695 | 23.3375 | 23.3695 | 23.3695 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.1184 | 20.1184 | 49.2439 | 2 | PROCESSED | 57534.3873611111 | 2016-05-26 09:17:48 | 54398 | 2007-10-25 00:00:00 | 53926.8416319445 | 2006-07-10 20:11:57 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501033010/ | Quick Look | ![]() |
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91 | GC_SGR_B_NORTH | 266.6955 | -28.3829 | 265.90467 | -28.36493 | 267.072555 | -4.975375 | 0.60514127 | 0.06995468 | 271.4417 | 54002.2105555556 | 2006-09-24 05:03:12 | 54003.2919444444 | 2006-09-25 07:00:24 | 501040020 | 44.8295 | 38 | 44.8455 | 44.8295 | 44.8375 | 44.8535 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.9705 | 39.9705 | 93.4319 | 1 | PROCESSED | 57535.678125 | 2016-05-27 16:16:30 | 54744 | 2008-10-05 00:00:00 | 54021.2868055556 | 2006-10-13 06:53:00 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040020/ | Quick Look | ![]() |
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92 | HESS J1614-518 | 243.5851 | -51.743 | 242.630135 | -51.617031 | 251.446035 | -29.987821 | 331.574855 | -0.5276897 | 283.402 | 53993.6672222222 | 2006-09-15 16:00:48 | 53994.4571064815 | 2006-09-16 10:58:14 | 501042010 | 40.1777 | 50 | 40.1857 | 40.1777 | 40.1857 | 40.1857 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.5607 | 43.5607 | 68.2279 | 0 | PROCESSED | 57535.5776967593 | 2016-05-27 13:51:53 | 54526 | 2008-03-01 00:00:00 | 54020.8545833333 | 2006-10-12 20:30:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501042010/ | Quick Look | ![]() |
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93 | HESS J1614-518 BG | 242.0174 | -52.4329 | 241.059171 | -52.300176 | 250.522759 | -30.865237 | 330.3996927 | -0.37656553 | 291.2192 | 53994.4597569444 | 2006-09-16 11:02:03 | 53995.3015509259 | 2006-09-17 07:14:14 | 501043010 | 43.5554 | 50 | 43.5634 | 43.5634 | 43.5554 | 43.5634 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 50.5922 | 50.5922 | 72.7039 | 1 | PROCESSED | 57535.5823726852 | 2016-05-27 13:58:37 | 54526 | 2008-03-01 00:00:00 | 54020.8662268518 | 2006-10-12 20:47:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501043010/ | Quick Look | ![]() |
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94 | GALACTIC CENTER GC3 | 265.5781 | -29.4684 | 264.780645 | -29.444998 | 266.119721 | -6.086772 | 359.1684549 | 0.33584661 | 108.8001 | 54170.7951273148 | 2007-03-11 19:04:59 | 54171.3397453704 | 2007-03-12 08:09:14 | 501048010 | 27.4546 | 25 | 27.4786 | 27.4546 | 0 | 27.4786 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.0548 | 24.0548 | 47.0479 | 1 | PROCESSED | 57537.6483333333 | 2016-05-29 15:33:36 | 54736 | 2008-09-27 00:00:00 | 54182.2788425926 | 2007-03-23 06:41:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501048010/ | Quick Look | ![]() |
95 | GALACTIC CENTER | 265.9089 | -29.649 | 265.11021 | -29.627197 | 266.414403 | -6.258746 | 359.16615355 | -0.00387238 | 269 | 54017.0975115741 | 2006-10-09 02:20:25 | 54017.5690277778 | 2006-10-09 13:39:24 | 501050010 | 22.0477 | 20 | 22.0477 | 22.0477 | 22.0477 | 22.0477 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18.6256 | 18.6256 | 40.7359 | 0 | PROCESSED | 57535.8013194445 | 2016-05-27 19:13:54 | 54735 | 2008-09-26 00:00:00 | 54053.4127777778 | 2006-11-14 09:54:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501050010/ | Quick Look | ![]() |
96 | GALACTIC CENTER | 265.2994 | -30.4982 | 264.495374 | -30.473432 | 265.90984 | -7.123709 | 358.16648703 | -0.00302139 | 269.0003 | 54018.8881828704 | 2006-10-10 21:18:59 | 54019.4209953704 | 2006-10-11 10:06:14 | 501053010 | 21.9086 | 20 | 21.9086 | 21.9321 | 21.9166 | 21.9166 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.948 | 19.948 | 46.0319 | 0 | PROCESSED | 57535.8190393518 | 2016-05-27 19:39:25 | 54735 | 2008-09-26 00:00:00 | 54053.5019675926 | 2006-11-14 12:02:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501053010/ | Quick Look | ![]() |
97 | GC SGR D EAST | 267.2856 | -27.6502 | 266.49923 | -27.635104 | 267.579665 | -4.231943 | 1.50163715 | 0.00269695 | 108.7997 | 54176.2132407407 | 2007-03-17 05:07:04 | 54177.8737731482 | 2007-03-18 20:58:14 | 501060010 | 64.7953 | 63 | 64.7953 | 64.8267 | 0 | 64.8113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.6297 | 54.6297 | 143.4659 | 1 | PROCESSED | 57537.7151851852 | 2016-05-29 17:09:52 | 54736 | 2008-09-27 00:00:00 | 54185.4429050926 | 2007-03-26 10:37:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501060010/ | Quick Look | ![]() |
98 | RXJ1713-3946 | 258.5524 | -39.4291 | 257.687827 | -39.37177 | 260.79719 | -16.352329 | 347.6770378 | -0.38034705 | 267.9999 | 53997.5713773148 | 2006-09-19 13:42:47 | 53997.9140509259 | 2006-09-19 21:56:14 | 501069010 | 18.375 | 20 | 18.375 | 18.375 | 18.375 | 18.375 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14.2767 | 14.2767 | 29.5999 | 0 | PROCESSED | 57535.6332060185 | 2016-05-27 15:11:49 | 54526 | 2008-03-01 00:00:00 | 54021.1502546296 | 2006-10-13 03:36:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501069010/ | Quick Look | ![]() |
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99 | RXJ1713-3946 | 258.9408 | -39.7267 | 258.073523 | -39.671212 | 261.133474 | -16.624716 | 347.60984156 | -0.7970823 | 268.0009 | 54013.3138541667 | 2006-10-05 07:31:57 | 54013.877974537 | 2006-10-05 21:04:17 | 501072010 | 19.9817 | 20 | 19.9817 | 19.9817 | 19.9817 | 19.9817 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.2997 | 16.2997 | 48.718 | 1 | PROCESSED | 57535.7676736111 | 2016-05-27 18:25:27 | 54526 | 2008-03-01 00:00:00 | 54021.6599652778 | 2006-10-13 15:50:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501072010/ | Quick Look | ![]() |
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100 | G156.2+5.7NW | 74.223 | 52.4174 | 73.2357 | 52.339427 | 79.010107 | 29.577951 | 155.48379099 | 5.80912082 | 273.883 | 54147.6530902778 | 2007-02-16 15:40:27 | 54148.7558333333 | 2007-02-17 18:08:24 | 501075010 | 50.5468 | 50 | 50.5468 | 50.5468 | 0 | 50.5468 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1958 | 46.1958 | 95.2599 | 0 | PROCESSED | 57537.3885763889 | 2016-05-29 09:19:33 | 54695 | 2008-08-17 00:00:00 | 54153.2775 | 2007-02-22 06:39:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBERT PETRE | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501075010/ | Quick Look | ![]() |
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101 | SNR G93.3+6.9 CENTER | 312.9805 | 55.373 | 312.634427 | 55.183848 | 352.046818 | 66.979241 | 93.25121789 | 6.97467523 | 40.9208 | 53905.2215509259 | 2006-06-19 05:19:02 | 53905.6480787037 | 2006-06-19 15:33:14 | 501079010 | 20.5372 | 20 | 20.5452 | 20.5452 | 20.5452 | 20.5372 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.008 | 20.008 | 36.8159 | 0 | PROCESSED | 57534.7200347222 | 2016-05-26 17:16:51 | 54401 | 2007-10-28 00:00:00 | 53926.792962963 | 2006-07-10 19:01:52 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501079010/ | Quick Look | ![]() |
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102 | SNR G93.3+6.9 S1 | 313.1088 | 55.5284 | 312.76382 | 55.338789 | 352.457306 | 67.040407 | 93.41888838 | 7.01647125 | 40.6424 | 53905.6486458333 | 2006-06-19 15:34:03 | 53905.9696064815 | 2006-06-19 23:16:14 | 501080010 | 15.875 | 15 | 15.875 | 15.8902 | 15.891 | 15.883 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12.7588 | 12.7588 | 27.7279 | 1 | PROCESSED | 57534.7111805556 | 2016-05-26 17:04:06 | 54401 | 2007-10-28 00:00:00 | 53926.199212963 | 2006-07-10 04:46:52 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501080010/ | Quick Look | ![]() |
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103 | SNR G93.3+6.9 S4 | 312.7524 | 55.2472 | 312.406034 | 55.058863 | 351.58456 | 66.978212 | 93.07038921 | 6.99620044 | 39.4008 | 53906.7271296296 | 2006-06-20 17:27:04 | 53907.0550347222 | 2006-06-21 01:19:15 | 501083010 | 15.3662 | 15 | 15.3662 | 15.3662 | 15.3662 | 15.3662 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.4694 | 14.4694 | 28.3279 | 1 | PROCESSED | 57534.7341550926 | 2016-05-26 17:37:11 | 54401 | 2007-10-28 00:00:00 | 53926.117662037 | 2006-07-10 02:49:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501083010/ | Quick Look | ![]() |
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104 | HESS J1718-385 | 259.5512 | -38.6075 | 258.69231 | -38.554942 | 261.534502 | -15.472357 | 348.79652534 | -0.53531102 | 91.2393 | 54154.3587731482 | 2007-02-23 08:36:38 | 54154.7773611111 | 2007-02-23 18:39:24 | 501105010 | 20.744 | 19 | 20.744 | 20.744 | 0 | 20.744 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.8365 | 15.8365 | 36.1519 | 0 | PROCESSED | 57537.4491435185 | 2016-05-29 10:46:46 | 54527 | 2008-03-02 00:00:00 | 54158.2865740741 | 2007-02-27 06:52:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012044 | HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons. | GALACTIC DIFFUSE EMISSION | 5 | A | JAMES HINTON | EUR | 1 | AO1 | PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501105010/ | Quick Look | ![]() |
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105 | G156.2+5.7 CENTER | 74.723 | 51.7342 | 73.743251 | 51.658579 | 79.264036 | 28.862327 | 156.21466687 | 5.62934315 | 273.4473 | 54148.7568171296 | 2007-02-17 18:09:49 | 54149.9169444444 | 2007-02-18 22:00:24 | 501106010 | 51.2142 | 50 | 51.2222 | 51.2302 | 0 | 51.2142 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46.482 | 46.482 | 100.1999 | 0 | PROCESSED | 57537.3992824074 | 2016-05-29 09:34:58 | 54695 | 2008-08-17 00:00:00 | 54158.4264351852 | 2007-02-27 10:14:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013079 | Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | MASARU UENO | ROBERT PETRE | JUS | 1 | AO1 | REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501106010/ | Quick Look | ![]() |
106 | VELA X (REGION A) | 128.7666 | -45.458 | 128.346603 | -45.284447 | 153.579861 | -60.62666 | 263.74862198 | -2.99483781 | 337.7597 | 53927.7846990741 | 2006-07-11 18:49:58 | 53929.4703819444 | 2006-07-13 11:17:21 | 501107010 | 60.7735 | 60 | 60.7735 | 60.7735 | 60.7735 | 60.7735 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.1611 | 54.1611 | 145.6058 | 3 | PROCESSED | 57534.9641203704 | 2016-05-26 23:08:20 | 54401 | 2007-10-28 00:00:00 | 53942.4562037037 | 2006-07-26 10:56:56 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | OLEG KARGALTSEV | KOJI MORI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501107010/ | Quick Look | ![]() |
107 | VELA X (REGION C) | 127.7806 | -46.2716 | 127.370041 | -46.101802 | 153.218075 | -61.676794 | 263.99736145 | -4.03006469 | 349.189 | 53933.9133796296 | 2006-07-17 21:55:16 | 53934.7730787037 | 2006-07-18 18:33:14 | 501108010 | 29.2028 | 30 | 29.2028 | 29.2028 | 29.2028 | 29.2028 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.5929 | 25.5929 | 74.248 | 1 | PROCESSED | 57534.9868055556 | 2016-05-26 23:41:00 | 54404 | 2007-10-31 00:00:00 | 53943.4988773148 | 2006-07-27 11:58:23 | 3.0.22.43 | 7 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | OLEG KARGALTSEV | KOJI MORI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501108010/ | Quick Look | ![]() |
108 | XB1323-619 | 201.6454 | -62.1418 | 200.814994 | -61.88221 | 229.562797 | -47.947963 | 307.02498182 | 0.45033402 | 99.5731 | 54109.4794907407 | 2007-01-09 11:30:28 | 54110.9168402778 | 2007-01-10 22:00:15 | 401002010 | 55.9368 | 50 | 55.9368 | 55.9368 | 0 | 55.9368 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.8173 | 81.8173 | 124.1769 | 1 | PROCESSED | 57536.8666087963 | 2016-05-28 20:47:55 | 54735 | 2008-09-26 00:00:00 | 54133.0271759259 | 2007-02-02 00:39:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010002 | XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting. | GALACTIC POINT SOURCES | 4 | C | TADAYASU DOTANI | JAP | 1 | AO1 | BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401002010/ | Quick Look | ![]() |
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109 | THE CRAB OFFSETS | 83.6343 | 21.9041 | 82.882652 | 21.871421 | 84.095437 | -1.406393 | 184.65179297 | -5.84249768 | 87.5094 | 53997.0141550926 | 2006-09-19 00:20:23 | 53997.0834953704 | 2006-09-19 02:00:14 | 101011080 | 2.251 | 2 | 2.251 | 2.251 | 2.251 | 2.251 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.275 | 2.275 | 5.9839 | 1 | PROCESSED | 57535.6182407407 | 2016-05-27 14:50:16 | 53826 | 2006-04-01 00:00:00 | 54104.4469675926 | 2007-01-04 10:43:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011080/ | Quick Look | ![]() |
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110 | PKS 0558-504 | 89.9335 | -50.4395 | 89.62999 | -50.44058 | 89.864093 | -73.881363 | 257.95137808 | -28.57681508 | 212.4401 | 54121.9091203704 | 2007-01-21 21:49:08 | 54122.3529976852 | 2007-01-22 08:28:19 | 701011050 | 19.5154 | 20 | 19.5314 | 19.5154 | 0 | 19.5314 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.1236 | 16.1236 | 38.312 | 0 | PROCESSED | 57536.8983217593 | 2016-05-28 21:33:35 | 54735 | 2008-09-26 00:00:00 | 54137.0453240741 | 2007-02-06 01:05:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011050/ | Quick Look | ![]() |
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111 | SWIFT J0350.1-5019 | 57.6662 | -50.2998 | 57.309175 | -50.449494 | 28.967165 | -67.019674 | 259.65657878 | -48.95336771 | 180.7044 | 54062.0888078704 | 2006-11-23 02:07:53 | 54062.5647453704 | 2006-11-23 13:33:14 | 701017020 | 19.271 | 23 | 19.271 | 19.271 | 0 | 19.271 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.74 | 16.74 | 41.097 | 0 | PROCESSED | 57536.1549768518 | 2016-05-28 03:43:10 | 54750 | 2008-10-11 00:00:00 | 54088.5939583333 | 2006-12-19 14:15:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017020/ | Quick Look | ![]() |
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112 | BO 375 | 11.4476 | 41.6573 | 10.75946 | 41.384162 | 28.671168 | 33.427051 | 121.80050832 | -21.20204189 | 232.9596 | 54135.3691666667 | 2007-02-04 08:51:36 | 54135.7592476852 | 2007-02-04 18:13:19 | 701028010 | 12.7798 | 13 | 12.7798 | 12.7798 | 0 | 12.7798 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.8386 | 12.8386 | 33.664 | 1 | PROCESSED | 57536.9599189815 | 2016-05-28 23:02:17 | 54695 | 2008-08-17 00:00:00 | 54151.4930324074 | 2007-02-20 11:49:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028010/ | Quick Look | ![]() |
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113 | BO 375 | 11.4497 | 41.6556 | 10.761554 | 41.382464 | 28.671878 | 33.424815 | 121.80214792 | -21.2037783 | 231.6187 | 54137.6100810185 | 2007-02-06 14:38:31 | 54137.9737731482 | 2007-02-06 23:22:14 | 701028020 | 15.5371 | 13 | 15.5371 | 15.5371 | 0 | 15.5371 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.942 | 14.942 | 31.4159 | 0 | PROCESSED | 57537.3176967593 | 2016-05-29 07:37:29 | 54695 | 2008-08-17 00:00:00 | 54151.4987731482 | 2007-02-20 11:58:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028020/ | Quick Look | ![]() |
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114 | BO 375 | 11.4497 | 41.6556 | 10.761554 | 41.382464 | 28.671878 | 33.424815 | 121.80214792 | -21.2037783 | 231.4176 | 54142.8248032407 | 2007-02-11 19:47:43 | 54143.2167824074 | 2007-02-12 05:12:10 | 701028030 | 15.0878 | 13 | 15.0878 | 15.0878 | 0 | 15.0878 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.7164 | 15.7164 | 33.8379 | 1 | PROCESSED | 57537.3535069444 | 2016-05-29 08:29:03 | 54695 | 2008-08-17 00:00:00 | 54153.1806828704 | 2007-02-22 04:20:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ALBERT KONG | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701028030/ | Quick Look | ![]() |
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115 | NGC 3783 | 174.7611 | -37.7364 | 174.141196 | -37.45925 | 192.677729 | -36.170962 | 287.45850943 | 22.95048745 | 293.6402 | 53910.7726388889 | 2006-06-24 18:32:36 | 53912.8571412037 | 2006-06-26 20:34:17 | 701033010 | 75.7193 | 75 | 75.7193 | 75.7193 | 75.7193 | 75.7193 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.2993 | 68.2993 | 180.0237 | 0 | PROCESSED | 57534.7899652778 | 2016-05-26 18:57:33 | 54401 | 2007-10-28 00:00:00 | 53926.8847453704 | 2006-07-10 21:14:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011325 | We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ALEX MARKOWITZ | USA | 1 | AO1 | PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701033010/ | Quick Look | ![]() |
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116 | MRK 273 | 206.1319 | 55.8192 | 205.671114 | 56.069559 | 168.560084 | 59.024421 | 108.09580624 | 59.75355315 | 290.8776 | 53923.3108333333 | 2006-07-07 07:27:36 | 53925.3356481482 | 2006-07-09 08:03:20 | 701050010 | 79.9046 | 80 | 79.9126 | 79.9046 | 79.9206 | 79.9206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 82.8076 | 82.8076 | 174.9059 | 3 | PROCESSED | 57534.931400463 | 2016-05-26 22:21:13 | 54401 | 2007-10-28 00:00:00 | 53930.7076851852 | 2006-07-14 16:59:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011341 | We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SYLVAIN VEILLEUX | USA | 1 | AO1 | THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701050010/ | Quick Look | ![]() |
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117 | APM 08279+5255 | 127.9265 | 52.7635 | 126.994318 | 52.932793 | 116.239859 | 32.72128 | 165.74397918 | 36.24189551 | 118.0523 | 54020.1580902778 | 2006-10-12 03:47:39 | 54022.3134143518 | 2006-10-14 07:31:19 | 701057010 | 102.3328 | 100 | 102.3408 | 102.3408 | 102.3328 | 102.3408 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96.0187 | 96.0187 | 186.1858 | 3 | PROCESSED | 57535.8953125 | 2016-05-27 21:29:15 | 54702 | 2008-08-24 00:00:00 | 54053.9467013889 | 2006-11-14 22:43:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057010/ | Quick Look | ![]() |
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118 | 1ES 1101-232 | 165.8976 | -23.5471 | 165.286971 | -23.277424 | 177.035323 | -27.087344 | 273.21266184 | 33.02701002 | 279.8544 | 53880.6859606482 | 2006-05-25 16:27:47 | 53882.2161921296 | 2006-05-27 05:11:19 | 701071010 | 62.4327 | 55 | 62.4407 | 62.4407 | 62.4407 | 62.4327 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50.1033 | 50.1033 | 132.1939 | 0 | PROCESSED | 57534.4584027778 | 2016-05-26 11:00:06 | 54401 | 2007-10-28 00:00:00 | 53927.4165393518 | 2006-07-11 09:59:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANITA REIMER | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701071010/ | Quick Look | ![]() |
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119 | NGC 4992 | 197.2442 | 11.5776 | 196.620329 | 11.84391 | 191.275652 | 17.435393 | 318.61367169 | 73.91298788 | 297.9177 | 53904.2287615741 | 2006-06-18 05:29:25 | 53905.2112615741 | 2006-06-19 05:04:13 | 701080010 | 38.7886 | 40 | 38.7886 | 38.7886 | 38.7886 | 38.7886 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.6179 | 33.6179 | 84.8819 | 1 | PROCESSED | 57534.7313657407 | 2016-05-26 17:33:10 | 54422 | 2007-11-18 00:00:00 | 53926.1865856482 | 2006-07-10 04:28:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREA COMASTRI | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701080010/ | Quick Look | ![]() |
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120 | MKN 841 | 226.022 | 10.498 | 225.418561 | 10.69235 | 220.178743 | 26.653826 | 11.31218444 | 54.65057921 | 105.7688 | 54122.3650925926 | 2007-01-22 08:45:44 | 54123.6063541667 | 2007-01-23 14:33:09 | 701084010 | 51.7528 | 50 | 51.7928 | 51.7528 | 0 | 51.7928 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7077 | 43.7077 | 107.2379 | 1 | PROCESSED | 57536.9356481482 | 2016-05-28 22:27:20 | 54777 | 2008-11-07 00:00:00 | 54139.3030208333 | 2007-02-08 07:16:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PIERRE-OLIVIER PETRUCCI | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084010/ | Quick Look | ![]() |
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121 | GB1428+4217 | 217.5879 | 42.0673 | 217.100189 | 42.288572 | 194.201902 | 52.635769 | 75.8575282 | 64.90635728 | 315.7011 | 53898.716400463 | 2006-06-12 17:11:37 | 53899.8336111111 | 2006-06-13 20:00:24 | 701092010 | 48.6956 | 50 | 48.6956 | 48.6956 | 48.6956 | 48.6956 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.4943 | 43.4943 | 96.5159 | 1 | PROCESSED | 57534.6334259259 | 2016-05-26 15:12:08 | 54394 | 2007-10-21 00:00:00 | 53926.3635069444 | 2006-07-10 08:43:27 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012043 | We propose to observe GB1428+4217 at z=4.72 for 50ks with Suzaku in order to determine its spectrum up to 45 keV, corresponding to a rest-frame energy of ~250 keV. This will allow to robustly model the spectrum in terms of a hard power-law and a Comptonization component from the scattering of `cold' electrons in the jet onto the soft nuclear photon field, as qualitatively hinted by XMM-Newton available data. This would be the first detection of such a feature in blazars and would directly and uniquely give information on the power of the relativistic jets in this source. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREW FABIAN | EUR | 1 | AO1 | JET POWER OF THE DISTANT EXTREME LUMINOSITY BLAZAR GB1428+4217 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701092010/ | Quick Look | ![]() |
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122 | F05189-2524 | 80.2383 | -25.4117 | 79.728122 | -25.460147 | 76.667297 | -48.403351 | 227.93752087 | -30.32292957 | 290.8212 | 53835.6784259259 | 2006-04-10 16:16:56 | 53837.6467708333 | 2006-04-12 15:31:21 | 701097010 | 78.1555 | 80 | 78.1555 | 78.1635 | 78.1555 | 78.1555 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 51.7402 | 51.7402 | 169.9899 | 2 | PROCESSED | 57533.4937268518 | 2016-05-25 11:50:58 | 54401 | 2007-10-28 00:00:00 | 53906.8811689815 | 2006-06-20 21:08:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014341 | We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SYLVAIN VEILLEUX | NAOHISA ANABUKI | USJ | 1 | AO1 | THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701097010/ | Quick Look | ![]() |
123 | A2104W | 234.9146 | -3.2969 | 234.261116 | -3.135581 | 233.381893 | 15.795133 | 2.73337641 | 39.30878407 | 117.9077 | 54121.3401388889 | 2007-01-21 08:09:48 | 54121.8960532407 | 2007-01-21 21:30:19 | 801001010 | 19.9269 | 20 | 19.9269 | 19.9269 | 0 | 19.9269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.2001 | 17.2001 | 48.0079 | 2 | PROCESSED | 57536.8971875 | 2016-05-28 21:31:57 | 54735 | 2008-09-26 00:00:00 | 54137.0936805556 | 2007-02-06 02:14:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801001010/ | Quick Look | ![]() |
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124 | RX J1347.5-1145 | 206.8558 | -11.8095 | 206.189394 | -11.560383 | 209.147012 | -0.679812 | 323.97878779 | 48.76095676 | 291.7151 | 53931.2858333333 | 2006-07-15 06:51:36 | 53933.2551388889 | 2006-07-17 06:07:24 | 801013020 | 79.1105 | 75 | 79.1265 | 79.1105 | 79.1265 | 79.1345 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 69.567 | 69.567 | 170.1098 | 2 | PROCESSED | 57534.9865393518 | 2016-05-26 23:40:37 | 54394 | 2007-10-21 00:00:00 | 53942.463587963 | 2006-07-26 11:07:34 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010014 | We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013020/ | Quick Look | ![]() |
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125 | OPHIUCHUS CLUSTER 0 | 258.0174 | -23.3865 | 257.259196 | -23.326891 | 259.005066 | -0.401441 | 0.50702706 | 9.33401192 | 88.8366 | 54183.0313078704 | 2007-03-24 00:45:05 | 54183.5648726852 | 2007-03-24 13:33:25 | 801021010 | 16.6411 | 15 | 16.6411 | 16.6411 | 0 | 16.6411 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.5209 | 13.5209 | 46.0959 | 0 | PROCESSED | 57537.9746643518 | 2016-05-29 23:23:31 | 54736 | 2008-09-27 00:00:00 | 54209.5175462963 | 2007-04-19 12:25:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801021010/ | Quick Look | ![]() |
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126 | OPHIUCHUS CLUSTER 8 | 258.0175 | -23.6665 | 257.257716 | -23.606887 | 259.028283 | -0.680466 | 0.2749393 | 9.17298979 | 88.8988 | 54182.4897337963 | 2007-03-23 11:45:13 | 54183.0308333333 | 2007-03-24 00:44:24 | 801029010 | 23.7389 | 15 | 23.7469 | 23.7389 | 0 | 23.7469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.678 | 21.678 | 46.746 | 0 | PROCESSED | 57537.9753240741 | 2016-05-29 23:24:28 | 54736 | 2008-09-27 00:00:00 | 54209.5725231482 | 2007-04-19 13:44:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801029010/ | Quick Look | ![]() |
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127 | M87 50' SE | 188.2678 | 11.8367 | 187.635305 | 12.112401 | 182.806232 | 14.132107 | 286.30035277 | 74.11241529 | 119.899 | 54071.127650463 | 2006-12-02 03:03:49 | 54072.312037037 | 2006-12-03 07:29:20 | 801039010 | 53.6374 | 50 | 53.6374 | 53.6581 | 0 | 53.6454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1394 | 46.1394 | 102.309 | 1 | PROCESSED | 57536.2354861111 | 2016-05-28 05:39:06 | 54735 | 2008-09-26 00:00:00 | 54088.5776736111 | 2006-12-19 13:51:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010084 | The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIRONORI MATSUMOTO | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801039010/ | Quick Look | ![]() |
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128 | PERSEUS CL OFFSET | 49.2788 | 41.3719 | 48.454118 | 41.188803 | 58.04223 | 22.344257 | 150.2212005 | -13.65398882 | 65.9966 | 53980.7676273148 | 2006-09-02 18:25:23 | 53981.4543287037 | 2006-09-03 10:54:14 | 801049020 | 32.4646 | 30 | 32.4806 | 32.4646 | 32.4966 | 32.4886 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 28.2912 | 28.2912 | 59.3199 | 1 | PROCESSED | 57535.422025463 | 2016-05-27 10:07:43 | 54526 | 2008-03-01 00:00:00 | 54021.2712731482 | 2006-10-13 06:30:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049020/ | Quick Look | ![]() |
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129 | ABELL 2199 OFFSET 4 | 247.0296 | 39.3161 | 246.598828 | 39.425672 | 233.044127 | 59.841273 | 62.60481799 | 43.78660639 | 250.4756 | 54012.6800462963 | 2006-10-04 16:19:16 | 54013.3044444444 | 2006-10-05 07:18:24 | 801060010 | 24.4546 | 25 | 24.4706 | 24.4626 | 24.4546 | 24.4775 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.811 | 25.811 | 53.9399 | 0 | PROCESSED | 57535.7612615741 | 2016-05-27 18:16:13 | 54735 | 2008-09-26 00:00:00 | 54024.6738888889 | 2006-10-16 16:10:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801060010/ | Quick Look | ![]() |
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130 | Z8276 | 266.0474 | 32.9693 | 265.586798 | 32.989586 | 263.998981 | 56.326696 | 57.88393681 | 27.65216461 | 308.1365 | 53961.1406134259 | 2006-08-14 03:22:29 | 53961.4723958333 | 2006-08-14 11:20:15 | 801079010 | 14.9374 | 14 | 14.9374 | 14.9374 | 14.9374 | 14.9374 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15.462 | 15.462 | 28.658 | 0 | PROCESSED | 57535.267962963 | 2016-05-27 06:25:52 | 54391 | 2007-10-18 00:00:00 | 54018.6023842593 | 2006-10-10 14:27:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801079010/ | Quick Look | ![]() |
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131 | A3667_CENTER | 303.141 | -56.7974 | 302.14092 | -56.947599 | 291.656641 | -35.82366 | 340.90266514 | -33.39955413 | 74.263 | 53861.7363078704 | 2006-05-06 17:40:17 | 53862.3843055556 | 2006-05-07 09:13:24 | 801096010 | 20.8805 | 20 | 20.8885 | 20.8885 | 20.8965 | 20.8805 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.425 | 8.425 | 55.9439 | 1 | PROCESSED | 57533.6497337963 | 2016-05-25 15:35:37 | 54394 | 2007-10-21 00:00:00 | 53913.7840509259 | 2006-06-27 18:49:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801096010/ | Quick Look | ![]() |
132 | SGR1806-20 | 272.1595 | -20.349 | 271.415501 | -20.357687 | 272.017973 | 3.076639 | 10.0481975 | -0.20823053 | 88.7483 | 54189.6305555556 | 2007-03-30 15:08:00 | 54190.0627199074 | 2007-03-31 01:30:19 | 401021010 | 19.2889 | 20 | 19.2889 | 19.595 | 0 | 19.3563 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.5071 | 16.5071 | 37.3279 | 1 | PROCESSED | 57538.0253587963 | 2016-05-30 00:36:31 | 54561 | 2008-04-05 00:00:00 | 54209.5169212963 | 2007-04-19 12:24:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010124 | We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. | GALACTIC POINT SOURCES | 4 | A | YUJIN NAKAGAWA | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401021010/ | Quick Look | ![]() |
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133 | T CRB | 239.8773 | 25.9106 | 239.353591 | 26.051383 | 230.095833 | 45.264151 | 42.36027985 | 48.16117824 | 268.9321 | 53984.9474652778 | 2006-09-06 22:44:21 | 53986.0911921296 | 2006-09-08 02:11:19 | 401043010 | 46.3033 | 50 | 46.3113 | 46.3113 | 46.3193 | 46.3033 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.4314 | 45.4314 | 98.8159 | 1 | PROCESSED | 57535.5107175926 | 2016-05-27 12:15:26 | 54526 | 2008-03-01 00:00:00 | 54053.4340856482 | 2006-11-14 10:25:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011106 | Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism. | GALACTIC POINT SOURCES | 4 | A | JENNIFER SOKOLOSKI | USA | 1 | AO1 | THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401043010/ | Quick Look | ![]() |
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134 | GC_SGR_B_NORTH | 266.6958 | -28.383 | 265.90497 | -28.365031 | 267.072823 | -4.975469 | 0.60519276 | 0.06967717 | 271.4415 | 53999.7284837963 | 2006-09-21 17:29:01 | 54001.2863425926 | 2006-09-23 06:52:20 | 501040010 | 61.3753 | 62 | 61.3913 | 61.3753 | 61.3833 | 61.3913 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.867 | 53.867 | 134.5818 | 2 | PROCESSED | 57535.7042361111 | 2016-05-27 16:54:06 | 54735 | 2008-09-26 00:00:00 | 54021.2828472222 | 2006-10-13 06:47:18 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501040010/ | Quick Look | ![]() |
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135 | IGRJ16465-4507 | 251.6303 | -45.1738 | 250.724808 | -45.083948 | 256.064043 | -22.616175 | 340.00343338 | 0.10772124 | 284.9562 | 53987.3839814815 | 2006-09-09 09:12:56 | 53987.9203009259 | 2006-09-09 22:05:14 | 401052010 | 22.5279 | 20 | 22.5359 | 22.5279 | 22.5359 | 22.5359 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.6454 | 24.6454 | 46.332 | 0 | PROCESSED | 57535.4975925926 | 2016-05-27 11:56:32 | 54526 | 2008-03-01 00:00:00 | 54021.113287037 | 2006-10-13 02:43:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401052010/ | Quick Look | ![]() |
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136 | FORNAX A WEST LOBE | 50.4184 | -37.1645 | 49.940428 | -37.342839 | 32.47574 | -52.998531 | 240.1258488 | -56.89722719 | 219.7525 | 54092.8700462963 | 2006-12-23 20:52:52 | 54095.6113888889 | 2006-12-26 14:40:24 | 801014010 | 93.3093 | 100 | 93.3093 | 93.3093 | 0 | 93.3093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.3716 | 96.3716 | 236.8358 | 5 | PROCESSED | 57536.4597569444 | 2016-05-28 11:02:03 | 54735 | 2008-09-26 00:00:00 | 54111.6821875 | 2007-01-11 16:22:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010029 | We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO TASHIRO | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801014010/ | Quick Look | ![]() |
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137 | IGR J17497-2821 | 267.404 | -28.4152 | 266.612848 | -28.400666 | 267.698677 | -4.994865 | 0.89934627 | -0.48041902 | 271.4056 | 54003.2926967593 | 2006-09-25 07:01:29 | 54004.593275463 | 2006-09-26 14:14:19 | 901003010 | 53.3178 | 60 | 53.3338 | 53.3338 | 53.3338 | 53.3178 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 47.9476 | 47.9476 | 112.3599 | 1 | PROCESSED | 57535.7125925926 | 2016-05-27 17:06:08 | 54004 | 2006-09-26 00:00:00 | 54026.5016898148 | 2006-10-18 12:02:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017003 | N/A | GALACTIC COMPACT OBJECT | 9 | A | SWG | JAP | 1 | TOO | OBSERVATION OF IGR J17497-2821 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901003010/ | Quick Look | ![]() |
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138 | OPHIUCHUS CLUSTER 1 | 258.2981 | -23.3868 | 257.539766 | -23.328523 | 259.261866 | -0.380707 | 0.65649186 | 9.12279372 | 88.7031 | 54180.6159953704 | 2007-03-21 14:47:02 | 54181.1398611111 | 2007-03-22 03:21:24 | 801022010 | 24.067 | 15 | 24.075 | 24.067 | 0 | 24.075 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.8213 | 21.8213 | 45.254 | 1 | PROCESSED | 57537.7417476852 | 2016-05-29 17:48:07 | 54736 | 2008-09-27 00:00:00 | 54186.192650463 | 2007-03-27 04:37:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801022010/ | Quick Look | ![]() |
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139 | AWM7 | 43.631 | 41.5933 | 42.82175 | 41.390486 | 53.723626 | 23.815753 | 146.34082925 | -15.61629549 | 90.4997 | 53954.2348842593 | 2006-08-07 05:38:14 | 53954.71625 | 2006-08-07 17:11:24 | 801035010 | 18.9858 | 20 | 18.9858 | 18.9858 | 18.9858 | 18.9858 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.5542 | 17.5542 | 41.588 | 0 | PROCESSED | 57535.2434953704 | 2016-05-27 05:50:38 | 54422 | 2007-11-18 00:00:00 | 54020.7471759259 | 2006-10-12 17:55:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801035010/ | Quick Look | ![]() |
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140 | NGC 4631 | 190.5387 | 32.5478 | 189.929771 | 32.821718 | 174.99352 | 33.703009 | 142.74124336 | 84.2191655 | 139.0678 | 54067.1412615741 | 2006-11-28 03:23:25 | 54068.9133217593 | 2006-11-29 21:55:11 | 801019010 | 81.0761 | 80 | 81.0841 | 81.0761 | 0 | 81.0841 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.4358 | 74.4358 | 153.07 | 0 | PROCESSED | 57536.2568865741 | 2016-05-28 06:09:55 | 54735 | 2008-09-26 00:00:00 | 54088.6914699074 | 2006-12-19 16:35:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010062 | We propose to observe a edge-on nearby starburst galaxy, NGC 4631 for an exposure time of 80 ksec. This observation will give us a ``template'' of ejecta from type II SNe with less than 30% accuracy of abandance of alpha elemements. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORIKO YAMASAKI | JAP | 1 | AO1 | OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801019010/ | Quick Look | ![]() |
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141 | MARKARIAN 509 | 311.0428 | -10.7274 | 310.361715 | -10.908973 | 310.545221 | 7.124071 | 35.9681072 | -29.85888698 | 254.2043 | 54054.375150463 | 2006-11-15 09:00:13 | 54055.0113541667 | 2006-11-16 00:16:21 | 701093030 | 24.4466 | 25 | 24.4466 | 24.4466 | 0 | 24.4466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.327 | 18.327 | 54.9679 | 1 | PROCESSED | 57536.1015162037 | 2016-05-28 02:26:11 | 54456 | 2007-12-22 00:00:00 | 54088.6171875 | 2006-12-19 14:48:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093030/ | Quick Look | ![]() |
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142 | RXJ1713-3946 | 257.7765 | -39.428 | 256.912609 | -39.366986 | 260.174712 | -16.402181 | 347.32530765 | 0.10490445 | 268.0003 | 53990.7111689815 | 2006-09-12 17:04:05 | 53991.0488888889 | 2006-09-13 01:10:24 | 501067010 | 21.1796 | 20 | 21.1876 | 21.1796 | 21.1931 | 21.1956 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21.9861 | 21.9861 | 29.1679 | 0 | PROCESSED | 57535.5530902778 | 2016-05-27 13:16:27 | 54526 | 2008-03-01 00:00:00 | 54020.8250925926 | 2006-10-12 19:48:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501067010/ | Quick Look | ![]() |
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143 | JUPITER | 226.6157 | -16.1957 | 225.916913 | -16.003222 | 228.709072 | 1.245307 | 344.00356707 | 35.68981432 | 118.4907 | 53792.7940856482 | 2006-02-26 19:03:29 | 53793.8599421296 | 2006-02-27 20:38:19 | 401001030 | 40.7912 | 36 | 40.7992 | 40.7912 | 40.7992 | 40.7992 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.5363 | 35.5363 | 92.0739 | 0 | PROCESSED | 57533.1063078704 | 2016-05-25 02:33:05 | 54401 | 2007-10-28 00:00:00 | 53905.5868055556 | 2006-06-19 14:05:00 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001030/ | Quick Look | ![]() |
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144 | BETA LYR | 282.5094 | 33.3738 | 282.047614 | 33.314587 | 288.857821 | 55.998718 | 63.19462876 | 14.79594569 | 59.4704 | 53862.545474537 | 2006-05-07 13:05:29 | 53862.9952083333 | 2006-05-07 23:53:06 | 401036010 | 20.2515 | 20 | 20.2675 | 20.2515 | 20.2675 | 20.2675 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.8947 | 9.8947 | 38.8519 | 1 | PROCESSED | 57533.7394212963 | 2016-05-25 17:44:46 | 54401 | 2007-10-28 00:00:00 | 53913.8191550926 | 2006-06-27 19:39:35 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036010/ | Quick Look | ![]() |
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145 | BETA LYR | 282.5093 | 33.3719 | 282.047501 | 33.312687 | 288.85715 | 55.996853 | 63.19278609 | 14.79528012 | 53.4973 | 53871.4311226852 | 2006-05-16 10:20:49 | 53871.8571875 | 2006-05-16 20:34:21 | 401036030 | 18.1954 | 20 | 18.1954 | 18.1954 | 18.1954 | 18.1954 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.8421 | 19.8421 | 36.8079 | 0 | PROCESSED | 57534.3160532407 | 2016-05-26 07:35:07 | 54401 | 2007-10-28 00:00:00 | 53920.4164351852 | 2006-07-04 09:59:40 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | RICHARD IGNACE | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401036030/ | Quick Look | ![]() |
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146 | SKY_50.0_-62.4 | 50.0507 | -62.4328 | 49.819854 | -62.612067 | 354.772614 | -72.643934 | 278.67600391 | -47.08169247 | 281.591 | 53795.7055671296 | 2006-03-01 16:56:01 | 53796.9369675926 | 2006-03-02 22:29:14 | 501001010 | 80.145 | 80 | 80.153 | 80.145 | 80.153 | 80.145 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74.0122 | 74.0122 | 106.376 | 0 | PROCESSED | 57533.1282638889 | 2016-05-25 03:04:42 | 54401 | 2007-10-28 00:00:00 | 53905.6164930556 | 2006-06-19 14:47:45 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | ROBIN SHELTON | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501001010/ | Quick Look | ![]() |
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147 | 4U 1636-536 | 250.2272 | -53.754 | 249.230789 | -53.657507 | 256.461332 | -31.236669 | 332.91133194 | -4.81789372 | 91.2454 | 54160.0424421296 | 2007-03-01 01:01:07 | 54160.8931597222 | 2007-03-01 21:26:09 | 401050030 | 38.7193 | 38 | 38.7274 | 38.7193 | 0 | 38.7194 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 48.1459 | 48.1459 | 73.498 | 1 | PROCESSED | 57537.5161111111 | 2016-05-29 12:23:12 | 54695 | 2008-08-17 00:00:00 | 54167.6400462963 | 2007-03-08 15:21:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050030/ | Quick Look | ![]() |
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148 | GC SOUTH | 266.5016 | -29.1694 | 265.705845 | -29.150477 | 266.920624 | -5.765664 | 359.84485124 | -0.1935349 | 265.0006 | 54004.5960185185 | 2006-09-26 14:18:16 | 54007.8925231482 | 2006-09-29 21:25:14 | 501008010 | 129.5773 | 130 | 129.5773 | 129.5773 | 129.5773 | 129.5773 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111.2591 | 111.2591 | 284.8038 | 5 | PROCESSED | 57535.7712731482 | 2016-05-27 18:30:38 | 54744 | 2008-10-05 00:00:00 | 54021.0929050926 | 2006-10-13 02:13:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010044 | Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501008010/ | Quick Look | ![]() |
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149 | HESS J1745-303 | 266.2629 | -30.3722 | 265.459457 | -30.352101 | 266.742769 | -6.973282 | 358.71029443 | -0.64354718 | 263.6011 | 54015.0950462963 | 2006-10-07 02:16:52 | 54016.4300810185 | 2006-10-08 10:19:19 | 501010010 | 50.6707 | 50 | 50.6707 | 50.6707 | 50.6707 | 50.6707 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 45.6897 | 45.6897 | 115.3119 | 1 | PROCESSED | 57535.8009837963 | 2016-05-27 19:13:25 | 54526 | 2008-03-01 00:00:00 | 54021.698587963 | 2006-10-13 16:45:58 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010046 | So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons. | GALACTIC DIFFUSE EMISSION | 5 | A | RYO YAMAZAKI | JAP | 1 | AO1 | X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501010010/ | Quick Look | ![]() |
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150 | SWIFTJ2000.6+3210 | 300.1137 | 32.1218 | 299.624092 | 31.983158 | 312.678705 | 51.196511 | 68.93835501 | 1.08211502 | 255.6072 | 54039.0205671296 | 2006-10-31 00:29:37 | 54039.3029976852 | 2006-10-31 07:16:19 | 401053020 | 12.7484 | 10 | 12.7564 | 12.7484 | 12.7564 | 12.7564 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11.727 | 11.727 | 24.3939 | 0 | PROCESSED | 57535.9859490741 | 2016-05-27 23:39:46 | 54775 | 2008-11-05 00:00:00 | 54056.1959953704 | 2006-11-17 04:42:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053020/ | Quick Look | ![]() |
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151 | IGR J16318-4848 | 247.9691 | -48.8061 | 247.034981 | -48.699533 | 253.953463 | -26.583352 | 335.63186461 | -0.44896472 | 266.5948 | 53961.4825 | 2006-08-14 11:34:48 | 53964.3488310185 | 2006-08-17 08:22:19 | 401094010 | 97.2538 | 100 | 97.2698 | 97.2538 | 97.2698 | 97.2698 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 87.1128 | 87.1128 | 247.6059 | 5 | PROCESSED | 57535.3483564815 | 2016-05-27 08:21:38 | 54526 | 2008-03-01 00:00:00 | 54020.9181597222 | 2006-10-12 22:02:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012034 | We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848. | GALACTIC POINT SOURCES | 4 | B | JOERN WILMS | EUR | 1 | AO1 | OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401094010/ | Quick Look | ![]() |
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152 | CYGNUS_LOOP_P7 | 312.0838 | 30.7678 | 311.566097 | 30.58216 | 326.462182 | 46.307536 | 73.70103145 | -8.0534172 | 239.9966 | 54416.1673032407 | 2007-11-12 04:00:55 | 54416.7223263889 | 2007-11-12 17:20:09 | 501018010 | 24.1545 | 22 | 24.1545 | 24.1545 | 0 | 24.1545 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.861 | 18.861 | 47.92 | 0 | PROCESSED | 57540.4878587963 | 2016-06-01 11:42:31 | 54798 | 2008-11-28 00:00:00 | 54430.1343287037 | 2007-11-26 03:13:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501018010/ | Quick Look | ![]() |
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153 | HESS J1825-137 | 276.5031 | -13.6997 | 275.794781 | -13.729527 | 276.397624 | 9.596588 | 17.87105596 | -0.70261201 | 269.3213 | 54025.8175462963 | 2006-10-17 19:37:16 | 54027.1682291667 | 2006-10-19 04:02:15 | 501044010 | 50.293 | 50 | 50.293 | 50.293 | 50.293 | 50.293 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.9557 | 42.9557 | 116.694 | 1 | PROCESSED | 57535.8789351852 | 2016-05-27 21:05:40 | 54526 | 2008-03-01 00:00:00 | 54055.4418634259 | 2006-11-16 10:36:17 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501044010/ | Quick Look | ![]() |
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154 | RXJ1713-3946 | 257.7744 | -39.7271 | 256.908127 | -39.666071 | 260.20044 | -16.700257 | 347.08325974 | -0.07081205 | 268.0001 | 53990.3113310185 | 2006-09-12 07:28:19 | 53990.7106944444 | 2006-09-12 17:03:24 | 501066010 | 20.9207 | 20 | 20.9407 | 20.9207 | 20.926 | 20.9447 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.699 | 20.699 | 34.504 | 1 | PROCESSED | 57535.5600347222 | 2016-05-27 13:26:27 | 54526 | 2008-03-01 00:00:00 | 54020.8077546296 | 2006-10-12 19:23:10 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501066010/ | Quick Look | ![]() |
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155 | GALACTIC CENTER | 265.5037 | -30.2156 | 264.701457 | -30.191826 | 266.078204 | -6.8356 | 358.49956421 | -0.00336241 | 269.0005 | 54018.2813541667 | 2006-10-10 06:45:09 | 54018.887662037 | 2006-10-10 21:18:14 | 501052010 | 19.2451 | 20 | 19.2611 | 19.2611 | 19.2531 | 19.2451 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.0462 | 16.0462 | 52.3799 | 1 | PROCESSED | 57535.818275463 | 2016-05-27 19:38:19 | 54735 | 2008-09-26 00:00:00 | 54053.5074537037 | 2006-11-14 12:10:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501052010/ | Quick Look | ![]() |
156 | SNR G93.3+6.9 S2 | 312.6887 | 55.4958 | 312.345372 | 55.307685 | 351.959804 | 67.182569 | 93.24230604 | 7.18061007 | 40.0056 | 53905.9701736111 | 2006-06-19 23:17:03 | 53906.4293865741 | 2006-06-20 10:18:19 | 501081010 | 16.0092 | 15 | 16.0352 | 16.0272 | 16.0092 | 16.0352 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18.3757 | 18.3757 | 39.6679 | 1 | PROCESSED | 57534.7256134259 | 2016-05-26 17:24:53 | 54401 | 2007-10-28 00:00:00 | 53927.314537037 | 2006-07-11 07:32:56 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501081010/ | Quick Look | ![]() |
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157 | SWIFT J0601.9-8636 | 91.1523 | -86.6779 | 95.292028 | -86.662252 | 269.78546 | -69.879444 | 299.2555588 | -27.75439578 | 292.1727 | 53838.6834259259 | 2006-04-13 16:24:08 | 53839.0779976852 | 2006-04-14 01:52:19 | 701018010 | 19.7657 | 20 | 19.7817 | 19.7817 | 19.7657 | 19.7737 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.6614 | 16.6614 | 34.0599 | 0 | PROCESSED | 57533.4511226852 | 2016-05-25 10:49:37 | 54397 | 2007-10-24 00:00:00 | 53905.4682060185 | 2006-06-19 11:14:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701018010/ | Quick Look | ![]() |
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158 | PUP A : SE | 126.0128 | -43.1802 | 125.58355 | -43.01733 | 147.904142 | -59.590498 | 260.74447692 | -3.25911558 | 277.1832 | 53843.3098842593 | 2006-04-18 07:26:14 | 53843.8328009259 | 2006-04-18 19:59:14 | 501089010 | 29.7493 | 30 | 29.7493 | 29.8172 | 29.7652 | 29.7612 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 22.8867 | 22.8867 | 45.174 | 0 | PROCESSED | 57533.5119675926 | 2016-05-25 12:17:14 | 54401 | 2007-10-28 00:00:00 | 53907.001412037 | 2006-06-21 00:02:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501089010/ | Quick Look | ![]() |
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159 | NGC 5506 | 213.3121 | -3.2119 | 212.6632 | -2.97838 | 212.190756 | 9.596557 | 339.14659218 | 53.80640928 | 287.3747 | 53958.1015972222 | 2006-08-11 02:26:18 | 53959.4488425926 | 2006-08-12 10:46:20 | 701030020 | 53.2962 | 63 | 53.3042 | 53.2962 | 53.3042 | 53.3042 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.9832 | 47.9832 | 116.386 | 1 | PROCESSED | 57535.2817476852 | 2016-05-27 06:45:43 | 54695 | 2008-08-17 00:00:00 | 54116.3307291667 | 2007-01-16 07:56:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030020/ | Quick Look | ![]() |
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160 | MBM12 OFF-CLOUD | 41.3205 | 18.3346 | 40.61976 | 18.124407 | 44.482795 | 2.251416 | 157.33933963 | -36.81758445 | 247.4802 | 53772.648599537 | 2006-02-06 15:33:59 | 53774.618275463 | 2006-02-08 14:50:19 | 501104010 | 75.3292 | 70 | 75.3372 | 75.3292 | 75.3372 | 75.3372 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67.769 | 67.769 | 170.1159 | 1 | PROCESSED | 57532.9691550926 | 2016-05-24 23:15:35 | 54401 | 2007-10-28 00:00:00 | 53905.9757523148 | 2006-06-19 23:25:05 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011262 | Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | RANDALL SMITH | USA | 1 | AO1 | THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501104010/ | Quick Look | ![]() |
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161 | MRK 766 | 184.6147 | 29.8197 | 183.986078 | 30.097268 | 171.204802 | 28.944359 | 190.62410896 | 82.27145087 | 134.9989 | 54421.893287037 | 2007-11-17 21:26:20 | 54423.2363310185 | 2007-11-19 05:40:19 | 701035020 | 59.3635 | 50 | 59.3635 | 59.3635 | 0 | 59.3635 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51.1517 | 51.1517 | 116.0238 | 1 | PROCESSED | 57540.5762384259 | 2016-06-01 13:49:47 | 54800 | 2008-11-30 00:00:00 | 54433.2716666667 | 2007-11-29 06:31:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TRACEY TURNER | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701035020/ | Quick Look | ![]() |
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162 | E0102.2-7219 | 16.0175 | -72.0405 | 15.612819 | -72.30846 | 314.602108 | -65.044333 | 301.55408267 | -45.05394165 | 60.6353 | 53912.8662731482 | 2006-06-26 20:47:26 | 53913.4245833333 | 2006-06-27 10:11:24 | 101005030 | 21.6758 | 20 | 21.7158 | 21.6838 | 21.7158 | 21.6758 | 2 | 4 | 2 | 4 | 1 | 0 | 0 | 35.0626 | 35.0626 | 48.2039 | 0 | PROCESSED | 57534.7584837963 | 2016-05-26 18:12:13 | 53826 | 2006-04-01 00:00:00 | 53928.4586458333 | 2006-07-12 11:00:27 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101005030/ | Quick Look | ![]() |
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163 | RBS 315 | 36.2519 | 18.8398 | 35.555924 | 18.614311 | 40.065414 | 4.223463 | 151.73247281 | -38.74296898 | 76.7825 | 53941.8167013889 | 2006-07-25 19:36:03 | 53943.0404976852 | 2006-07-27 00:58:19 | 701077010 | 47.8309 | 50 | 47.8309 | 47.8309 | 47.8309 | 47.8309 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.425 | 43.425 | 105.7299 | 1 | PROCESSED | 57535.0495023148 | 2016-05-27 01:11:17 | 54400 | 2007-10-27 00:00:00 | 53955.7322106482 | 2006-08-08 17:34:23 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012008 | We propose to observe with Suzaku the X-ray bright blazar RBS 315, showing a very hard spectrum (Gamma<1.2) in the 2-10 keV range as determined by XMM. The requested observation will allow us to measure the continuum in the full Suzaku range (0.3-200 keV), fully exploiting the unique capabilities of the satellite. With its wide energy coverage and good response at soft energies, Suzaku will allow to determine with precision the spectral properties of the source in the hard medium and soft X-ray ranges, providing important clues on the physics and the environment of relativistic jets. A good measurement of the continuum will allow us to determine the luminosity emitted via the IC mechanism which usually dominates the radiative output and the total kinetic power carried by the outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FABRIZIO TAVECCHIO | EUR | 1 | AO1 | SUZAKU OBSERVATION OF THE HARD BROAD BAND CONTINUUM OF THE POWERFUL BLAZAR RBS 315 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701077010/ | Quick Look | ![]() |
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164 | GALACTIC CENTER | 266.0341 | -30.1068 | 265.232432 | -30.085596 | 266.53657 | -6.713302 | 358.83318764 | -0.33628911 | 269.0002 | 54019.4218402778 | 2006-10-11 10:07:27 | 54020.1446064815 | 2006-10-12 03:28:14 | 501057010 | 20.4884 | 20 | 20.4884 | 20.4964 | 20.4964 | 20.4964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.086 | 19.086 | 62.4379 | 0 | PROCESSED | 57535.8262037037 | 2016-05-27 19:49:44 | 54735 | 2008-09-26 00:00:00 | 54053.6059837963 | 2006-11-14 14:32:37 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501057010/ | Quick Look | ![]() |
165 | THE CRAB OFFSETS | 83.6229 | 22.105 | 82.870128 | 22.072264 | 84.093748 | -1.205217 | 184.47554642 | -5.74387633 | 85.7146 | 53983.889212963 | 2006-09-05 21:20:28 | 53983.9516087963 | 2006-09-05 22:50:19 | 101011020 | 3.35 | 2 | 3.35 | 3.35 | 3.35 | 3.35 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.004 | 3.004 | 5.3839 | 0 | PROCESSED | 57535.4600694444 | 2016-05-27 11:02:30 | 53826 | 2006-04-01 00:00:00 | 54104.4374189815 | 2007-01-04 10:29:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011020/ | Quick Look | ![]() |
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166 | SKY_53.3_-63.4 | 53.24 | -63.4549 | 53.047022 | -63.62196 | 354.144887 | -74.40934 | 278.62179386 | -45.30780651 | 286.1724 | 53797.8694444444 | 2006-03-03 20:52:00 | 53800.3342476852 | 2006-03-06 08:01:19 | 501002010 | 101.4752 | 100 | 101.4752 | 101.4752 | 101.4752 | 101.4752 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 145.4318 | 145.4318 | 212.8539 | 4 | PROCESSED | 57533.1863425926 | 2016-05-25 04:28:20 | 54401 | 2007-10-28 00:00:00 | 53906.7729282407 | 2006-06-20 18:33:01 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | ROBIN SHELTON | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501002010/ | Quick Look | ![]() |
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167 | GC SOUTH BGD | 266.1893 | -28.9082 | 265.395265 | -28.887768 | 266.639666 | -5.511508 | 359.92534776 | 0.17564926 | 265.0003 | 54007.8931365741 | 2006-09-29 21:26:07 | 54009.2884143518 | 2006-10-01 06:55:19 | 501009010 | 51.19 | 50 | 51.198 | 51.206 | 51.19 | 51.198 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47.7157 | 47.7157 | 120.5479 | 0 | PROCESSED | 57535.7087847222 | 2016-05-27 17:00:39 | 54735 | 2008-09-26 00:00:00 | 54020.9371064815 | 2006-10-12 22:29:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010044 | Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501009010/ | Quick Look | ![]() |
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168 | G344.7-0.1 | 255.9588 | -41.7032 | 255.078113 | -41.633558 | 258.959028 | -18.797881 | 344.67682908 | -0.15577285 | 89.2821 | 54152.1890393518 | 2007-02-21 04:32:13 | 54153.2919097222 | 2007-02-22 07:00:21 | 501011010 | 42.1336 | 40 | 42.1336 | 42.1336 | 0 | 42.1336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.2016 | 34.2016 | 95.28 | 1 | PROCESSED | 57537.4329050926 | 2016-05-29 10:23:23 | 54777 | 2008-11-07 00:00:00 | 54158.2352662037 | 2007-02-27 05:38:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010050 | We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | C | SHIGEO YAMAUCHI | JAP | 1 | AO1 | SUZAKU OBSERVATION OF G344.7-0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501011010/ | Quick Look | ![]() |
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169 | CYGNUS_LOOP_P13 | 313.4901 | 31.0708 | 312.971102 | 30.880128 | 328.238327 | 46.115492 | 74.70349314 | -8.80441033 | 68.2467 | 53865.1416666667 | 2006-05-10 03:24:00 | 53865.5321643518 | 2006-05-10 12:46:19 | 501030010 | 17.073 | 17 | 17.073 | 17.081 | 17.089 | 17.089 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14.269 | 14.269 | 33.7279 | 0 | PROCESSED | 57534.2605092593 | 2016-05-26 06:15:08 | 54394 | 2007-10-21 00:00:00 | 53914.0847569444 | 2006-06-28 02:02:03 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501030010/ | Quick Look | ![]() |
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170 | G156.2+5.7E | 75.8128 | 51.6405 | 74.832405 | 51.569986 | 80.017374 | 28.69124 | 156.70319129 | 6.10796494 | 274.6638 | 54149.9177893518 | 2007-02-18 22:01:37 | 54151.1750231482 | 2007-02-20 04:12:02 | 501074010 | 53.3331 | 50 | 53.3494 | 53.3491 | 0 | 53.3331 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.8218 | 50.8218 | 108.6199 | 2 | PROCESSED | 57537.4302893518 | 2016-05-29 10:19:37 | 54773 | 2008-11-03 00:00:00 | 54158.2839583333 | 2007-02-27 06:48:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBERT PETRE | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501074010/ | Quick Look | ![]() |
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171 | SNR G93.3+6.9 S3 | 313.171 | 55.2801 | 312.823004 | 55.090273 | 352.082126 | 66.837166 | 93.24775568 | 6.83197363 | 40.0152 | 53906.4300462963 | 2006-06-20 10:19:16 | 53906.7266087963 | 2006-06-20 17:26:19 | 501082010 | 16.3347 | 15 | 16.3347 | 16.3587 | 16.3507 | 16.3427 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13.9186 | 13.9186 | 25.6159 | 0 | PROCESSED | 57534.7339814815 | 2016-05-26 17:36:56 | 54401 | 2007-10-28 00:00:00 | 53926.2481365741 | 2006-07-10 05:57:19 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | Q. DANIEL WANG | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501082010/ | Quick Look | ![]() |
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172 | PUP A : NE | 125.7583 | -42.7117 | 125.326284 | -42.549841 | 147.156331 | -59.259606 | 260.25284038 | -3.14403225 | 277.1213 | 53842.913287037 | 2006-04-17 21:55:08 | 53843.3091319445 | 2006-04-18 07:25:09 | 501087010 | 20.7109 | 20 | 20.7336 | 20.7349 | 20.7189 | 20.7109 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19.7443 | 19.7443 | 34.1899 | 1 | PROCESSED | 57533.5127083333 | 2016-05-25 12:18:18 | 54401 | 2007-10-28 00:00:00 | 53906.9450231482 | 2006-06-20 22:40:50 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501087010/ | Quick Look | ![]() |
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173 | N11 SB | 74.1823 | -66.412 | 74.156384 | -66.487992 | 354.048784 | -83.709745 | 277.1886014 | -36.07081942 | 146.432 | 54046.4407291667 | 2006-11-07 10:34:39 | 54047.232037037 | 2006-11-08 05:34:08 | 501091010 | 30.452 | 30 | 30.452 | 30.452 | 30.452 | 30.452 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26.405 | 26.405 | 68.3659 | 0 | PROCESSED | 57536.0384953704 | 2016-05-28 00:55:26 | 54455 | 2007-12-21 00:00:00 | 54088.5643287037 | 2006-12-19 13:32:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011251 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | GALACTIC DIFFUSE EMISSION | 5 | C | ROSA WILLIAMS | USA | 1 | AO1 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501091010/ | Quick Look | ![]() |
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174 | VELA PULSAR/PWN 3 | 128.6368 | -45.8007 | 128.219858 | -45.627635 | 153.778024 | -60.967724 | 263.96966687 | -3.27226783 | 344.1164 | 53925.347974537 | 2006-07-09 08:21:05 | 53926.0467476852 | 2006-07-10 01:07:19 | 501110010 | 17.5886 | 20 | 17.6046 | 17.5886 | 17.5886 | 17.6046 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.2252 | 17.2252 | 60.3519 | 0 | PROCESSED | 57534.8715509259 | 2016-05-26 20:55:02 | 54401 | 2007-10-28 00:00:00 | 53930.634224537 | 2006-07-14 15:13:17 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | OLEG KARGALTSEV | KOJI MORI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501110010/ | Quick Look | ![]() |
175 | THE CRAB OFFSETS | 83.6323 | 21.9916 | 82.880162 | 21.958911 | 84.097445 | -1.318894 | 184.57650041 | -5.79723168 | 85.7244 | 53984.1531944445 | 2006-09-06 03:40:36 | 53984.2224421296 | 2006-09-06 05:20:19 | 101011050 | 3.355 | 2 | 3.355 | 3.355 | 3.355 | 3.355 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.187 | 2.187 | 5.9759 | 0 | PROCESSED | 57535.4744907407 | 2016-05-27 11:23:16 | 53826 | 2006-04-01 00:00:00 | 54104.4478587963 | 2007-01-04 10:44:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011050/ | Quick Look | ![]() |
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176 | RXJ1713-3946 | 258.1633 | -39.7281 | 257.296672 | -39.668915 | 260.511599 | -16.675371 | 347.25895477 | -0.31287235 | 268.0002 | 53989.5311574074 | 2006-09-11 12:44:52 | 53989.9216898148 | 2006-09-11 22:07:14 | 501064010 | 21.322 | 20 | 21.322 | 21.322 | 21.322 | 21.322 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23.0306 | 23.0306 | 33.7279 | 0 | PROCESSED | 57535.5353356482 | 2016-05-27 12:50:53 | 54526 | 2008-03-01 00:00:00 | 54020.8109027778 | 2006-10-12 19:27:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501064010/ | Quick Look | ![]() |
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177 | CYGNUS_LOOP_P2 | 313.2729 | 31.7708 | 312.75774 | 31.580892 | 328.394465 | 46.831624 | 75.13379207 | -8.21853117 | 240.0005 | 54418.0909722222 | 2007-11-14 02:11:00 | 54418.4168865741 | 2007-11-14 10:00:19 | 501013010 | 16.3799 | 10 | 16.3879 | 16.3879 | 0 | 16.3799 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.9786 | 10.9786 | 28.1519 | 0 | PROCESSED | 57540.5114351852 | 2016-06-01 12:16:28 | 54798 | 2008-11-28 00:00:00 | 54430.1915972222 | 2007-11-26 04:35:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501013010/ | Quick Look | ![]() |
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178 | CYGNUS_LOOP_P14 | 313.2365 | 30.8681 | 312.717032 | 30.678328 | 327.835222 | 46.014729 | 74.40554659 | -8.76356285 | 62.362 | 53867.6311111111 | 2006-05-12 15:08:48 | 53868.0050462963 | 2006-05-13 00:07:16 | 501031010 | 18.5809 | 18 | 18.5809 | 18.5809 | 18.5809 | 18.5809 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12.7378 | 12.7378 | 32.2979 | 0 | PROCESSED | 57534.275775463 | 2016-05-26 06:37:07 | 54394 | 2007-10-21 00:00:00 | 53914.3142476852 | 2006-06-28 07:32:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501031010/ | Quick Look | ![]() |
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179 | CYGNUS_LOOP_P18 | 312.0547 | 29.7111 | 311.531939 | 29.525574 | 325.8489 | 45.340722 | 72.84665082 | -8.68804998 | 237.4994 | 54087.0528819444 | 2006-12-18 01:16:09 | 54087.3405208333 | 2006-12-18 08:10:21 | 501035010 | 12.011 | 13 | 12.915 | 12.011 | 0 | 12.907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.4394 | 11.4394 | 24.8359 | 3 | PROCESSED | 57536.3543981482 | 2016-05-28 08:30:20 | 54750 | 2008-10-11 00:00:00 | 54096.4390972222 | 2006-12-27 10:32:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501035010/ | Quick Look | ![]() |
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180 | HESS J1825-137 BG | 276.9022 | -13.2649 | 276.196149 | -13.29666 | 276.811822 | 10.012623 | 18.4366217 | -0.84356166 | 269.33 | 54027.1689351852 | 2006-10-19 04:03:16 | 54028.5072337963 | 2006-10-20 12:10:25 | 501045010 | 52.1444 | 50 | 52.1524 | 52.1444 | 52.1524 | 52.1444 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.1974 | 42.1974 | 115.6079 | 2 | PROCESSED | 57535.8869907407 | 2016-05-27 21:17:16 | 54526 | 2008-03-01 00:00:00 | 54055.6591550926 | 2006-11-16 15:49:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501045010/ | Quick Look | ![]() |
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181 | PUP A : S | 125.6829 | -43.1445 | 125.254263 | -42.982932 | 147.449231 | -59.669734 | 260.57740663 | -3.43620983 | 277.8865 | 53843.8334606482 | 2006-04-18 20:00:11 | 53844.4397569444 | 2006-04-19 10:33:15 | 501090010 | 31.1445 | 30 | 31.1605 | 31.1525 | 31.1445 | 31.1685 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26.5856 | 26.5856 | 52.3719 | 1 | PROCESSED | 57533.5191550926 | 2016-05-25 12:27:35 | 54401 | 2007-10-28 00:00:00 | 53907.0902199074 | 2006-06-21 02:09:55 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501090010/ | Quick Look | ![]() |
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182 | VELA FRAGMENT B | 135.5139 | -43.4767 | 135.058427 | -43.278826 | 159.573758 | -56.461444 | 265.2464603 | 1.98991007 | 89.0012 | 54044.6051388889 | 2006-11-05 14:31:24 | 54046.4341898148 | 2006-11-07 10:25:14 | 501085010 | 57.8804 | 60 | 57.8964 | 57.8804 | 57.8964 | 57.8964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56.9652 | 56.9652 | 158.0219 | 2 | PROCESSED | 57536.0751157407 | 2016-05-28 01:48:10 | 54695 | 2008-08-17 00:00:00 | 54091.4107175926 | 2006-12-22 09:51:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011245 | Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | C | TERRANCE GAETZ | USA | 1 | AO1 | SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501085010/ | Quick Look | ![]() |
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183 | VELA PULSAR/PWN 1 | 128.7701 | -45.1981 | 128.348103 | -45.024538 | 153.316878 | -60.401286 | 263.5414959 | -2.83747227 | 337.9628 | 53926.0492592593 | 2006-07-10 01:10:56 | 53927.7841782407 | 2006-07-11 18:49:13 | 501109010 | 60.2913 | 60 | 60.3446 | 60.2913 | 60.3313 | 60.3233 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 52.6899 | 52.6899 | 149.8659 | 1 | PROCESSED | 57534.9239699074 | 2016-05-26 22:10:31 | 54401 | 2007-10-28 00:00:00 | 53942.4588078704 | 2006-07-26 11:00:41 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | OLEG KARGALTSEV | KOJI MORI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501109010/ | Quick Look | ![]() |
184 | THE CRAB OFFSETS | 83.5675 | 22.0116 | 82.815266 | 21.978598 | 84.038293 | -1.296249 | 184.5271819 | -5.8372614 | 85.7131 | 53984.7573263889 | 2006-09-06 18:10:33 | 53984.8197222222 | 2006-09-06 19:40:24 | 101011140 | 3.369 | 2 | 3.369 | 3.369 | 3.369 | 3.369 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.632 | 3.632 | 5.3839 | 0 | PROCESSED | 57535.4802546296 | 2016-05-27 11:31:34 | 53826 | 2006-04-01 00:00:00 | 54104.4270601852 | 2007-01-04 10:14:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011140/ | Quick Look | ![]() |
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185 | IRASF11223-1244 | 171.2239 | -12.9662 | 170.593283 | -12.69128 | 177.194404 | -15.365769 | 272.54538498 | 44.73919633 | 107.3062 | 54064.7275347222 | 2006-11-25 17:27:39 | 54065.5709953704 | 2006-11-26 13:42:14 | 701008010 | 40.9415 | 40 | 41.1015 | 40.9415 | 0 | 41.1095 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37.6804 | 37.6804 | 72.8639 | 1 | PROCESSED | 57536.1775925926 | 2016-05-28 04:15:44 | 54735 | 2008-09-26 00:00:00 | 54088.8556828704 | 2006-12-19 20:32:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010038 | The source of huge energy output from ultraluminous infrared galaxies (ULIRGs) is still under debate. We propose to search for a hidden QSO as the energy source by observing ULIRGs with high luminosity optical emission lines classified as a Seyfert 2. The data will be used to constrain the power of the central AGN and to study the nature of infrared selected type 2 QSOs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YUICHI TERASHIMA | JAP | 1 | AO1 | A SEARCH FOR HIDDEN QSO IN ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701008010/ | Quick Look | ![]() |
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186 | MRK 0359 | 21.8893 | 19.1757 | 21.213343 | 18.916781 | 27.368924 | 9.282102 | 134.6025573 | -42.87605962 | 244.6178 | 54137.9789699074 | 2007-02-06 23:29:43 | 54140.3738078704 | 2007-02-09 08:58:17 | 701082010 | 107.507 | 100 | 107.507 | 107.507 | 0 | 107.507 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.5761 | 102.5761 | 206.8678 | 2 | PROCESSED | 57537.3689930556 | 2016-05-29 08:51:21 | 54735 | 2008-09-26 00:00:00 | 54151.5150925926 | 2007-02-20 12:21:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012023 | Markarian 359 was the first source to be identified as a Narrow Line Seyfert 1 (NLS1) AGN, and its importance as an unusual source has been recognised for a long time. In the optical, it has unusually narrow lines for a NLS1. X-ray observations of the source are rare, but based on an XMM-Newton observation a strong reflection 'hump' is predicted. The source is therefore a critical one in the investigation of relativistically blurred photoionized disc reflection models. A detailed Suzaku observation will provide improved data quality in the XIS waveband, allow investigation of spectral variability in this waveband, and constrain the amount of reflection independently by using the HXD. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JAMIE CRUMMY | EUR | 1 | AO1 | NVESTIGATING REFLECTION IN MARKARIAN 359 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701082010/ | Quick Look | ![]() |
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187 | M31 | 10.6944 | 41.2627 | 10.010045 | 40.988882 | 27.852586 | 33.34214 | 121.18191229 | -21.57961988 | 231.6592 | 54115.6775578704 | 2007-01-15 16:15:41 | 54117.4572222222 | 2007-01-17 10:58:24 | 801043010 | 99.8723 | 100 | 99.8723 | 99.8723 | 0 | 99.8723 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.9124 | 103.9124 | 153.7238 | 1 | PROCESSED | 57536.8902777778 | 2016-05-28 21:22:00 | 54744 | 2008-10-05 00:00:00 | 54132.9457291667 | 2007-02-01 22:41:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010089 | We propose the 100 ks Suzaku observation of the central region of Andromeda Nebula (M31). Our gaol is to detect 3 components (cool, hot and hard) of galactic diffuse X-ray emission (GDXE) with the XIS and HXD. This detection shows the existance of the GDXE hot and hard component in the extragalactic normal spiral galaxy, for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROMITSU TAKAHASHI | JAP | 1 | AO1 | DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801043010/ | Quick Look | ![]() |
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188 | CRAB | 83.6368 | 22.0131 | 82.88454 | 21.980432 | 84.102563 | -1.297599 | 184.56049184 | -5.78219867 | 250.943 | 53829.1296643518 | 2006-04-04 03:06:43 | 53829.5974305556 | 2006-04-04 14:20:18 | 101004020 | 19.1389 | 20 | 19.1389 | 19.1458 | 19.1389 | 19.1389 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13.2831 | 13.2831 | 40.4119 | 1 | PROCESSED | 57533.3778009259 | 2016-05-25 09:04:02 | 53826 | 2006-04-01 00:00:00 | 53906.6409375 | 2006-06-20 15:22:57 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101004020/ | Quick Look | ![]() |
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189 | PKS 0558-504 | 89.9324 | -50.4401 | 89.628897 | -50.441186 | 89.861567 | -73.881962 | 257.95192858 | -28.57760064 | 211.3321 | 54120.8400925926 | 2007-01-20 20:09:44 | 54121.3279976852 | 2007-01-21 07:52:19 | 701011040 | 19.7381 | 20 | 19.7541 | 19.7381 | 0 | 19.7541 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.175 | 17.175 | 42.1359 | 0 | PROCESSED | 57536.8909953704 | 2016-05-28 21:23:02 | 54735 | 2008-09-26 00:00:00 | 54137.1036921296 | 2007-02-06 02:29:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011040/ | Quick Look | ![]() |
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190 | SWIFT J0255.2-0011 | 43.8161 | -0.2397 | 43.176621 | -0.441669 | 41.282729 | -16.217011 | 175.95402612 | -49.91735431 | 256.3177 | 54123.6209490741 | 2007-01-23 14:54:10 | 54126.2294560185 | 2007-01-26 05:30:25 | 701013010 | 101.6321 | 100 | 101.6321 | 101.6321 | 0 | 101.6321 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.2824 | 86.2824 | 225.3379 | 3 | PROCESSED | 57536.9811342593 | 2016-05-28 23:32:50 | 54735 | 2008-09-26 00:00:00 | 54137.3009027778 | 2007-02-06 07:13:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010122 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701013010/ | Quick Look | ![]() |
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191 | SWIFT J0505.7-2348 | 76.4285 | -23.9055 | 75.907939 | -23.972083 | 71.84647 | -46.496539 | 225.00444872 | -33.15769393 | 284.9903 | 53826.9254166667 | 2006-04-01 22:12:36 | 53829.1216898148 | 2006-04-04 02:55:14 | 701014010 | 78.5544 | 80 | 78.5544 | 78.5544 | 78.5544 | 78.5544 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.4937 | 53.4937 | 189.6979 | 1 | PROCESSED | 57533.4023726852 | 2016-05-25 09:39:25 | 54439 | 2007-12-05 00:00:00 | 53945.2822569444 | 2006-07-29 06:46:27 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010122 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701014010/ | Quick Look | ![]() |
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192 | SWIFT J0138.6-4001 | 24.6022 | -39.9757 | 24.058156 | -40.229446 | 3.045259 | -45.758208 | 268.75310615 | -73.8819888 | 44.7851 | 53890.7590740741 | 2006-06-04 18:13:04 | 53891.2085532407 | 2006-06-05 05:00:19 | 701015010 | 21.1979 | 20 | 21.2139 | 21.1979 | 21.2139 | 21.2139 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.4771 | 17.4771 | 38.8319 | 1 | PROCESSED | 57534.4839814815 | 2016-05-26 11:36:56 | 54394 | 2007-10-21 00:00:00 | 53926.7722337963 | 2006-07-10 18:32:01 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701015010/ | Quick Look | ![]() |
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193 | SWIFT J0350.1-5019 | 57.5863 | -50.3518 | 57.229549 | -50.501821 | 28.784936 | -67.035424 | 259.75531799 | -48.98660415 | 277.9348 | 54162.2927777778 | 2007-03-03 07:01:36 | 54162.5036921296 | 2007-03-03 12:05:19 | 701017030 | 8.1487 | 10 | 8.1567 | 8.1487 | 0 | 8.1567 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.0597 | 7.0597 | 18.2159 | 0 | PROCESSED | 57537.5866898148 | 2016-05-29 14:04:50 | 54750 | 2008-10-11 00:00:00 | 54167.6235763889 | 2007-03-08 14:57:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017030/ | Quick Look | ![]() |
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194 | TON S180 | 14.333 | -22.3803 | 13.720307 | -22.650448 | 3.73482 | -26.131336 | 138.98529016 | -85.06726133 | 237.1425 | 54078.5680671296 | 2006-12-09 13:38:01 | 54081.3584953704 | 2006-12-12 08:36:14 | 701021010 | 120.6609 | 120 | 120.6849 | 120.6609 | 0 | 120.6769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.3128 | 109.3128 | 241.052 | 3 | PROCESSED | 57536.3458680556 | 2016-05-28 08:18:03 | 54735 | 2008-09-26 00:00:00 | 54094.4773958333 | 2006-12-25 11:27:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010141 | TON S180 is a luminous Narrow Line Seyfert 1 galaxy, chracterizing enhanced Soft X-ray emission component without complex absorption/emission structures. The source is considered to be at super Eddington accretion rate. We aim to track change (or no change) in soft X-ray spectrum of this source according to factor of two ,rapid flux variation this source show. We partciularly focus on the slim disk model propsed for super Eddington accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | SOFT X-RAY EMISSION FROM SUPER-EDDINGTON ACCRETION DISK IN TON S180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701021010/ | Quick Look | ![]() |
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195 | MARKARIAN 335 | 1.5539 | 20.2624 | 0.911019 | 19.984083 | 9.744165 | 17.917566 | 108.74842011 | -41.36053721 | 68.4831 | 53907.0624537037 | 2006-06-21 01:29:56 | 53910.7585532407 | 2006-06-24 18:12:19 | 701031010 | 151.2884 | 150 | 151.2964 | 151.2884 | 151.2964 | 151.2964 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 140.9812 | 140.9812 | 319.3028 | 4 | PROCESSED | 57534.8340046296 | 2016-05-26 20:00:58 | 54401 | 2007-10-28 00:00:00 | 53928.5392361111 | 2006-07-12 12:56:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011323 | We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JON MILLER | USA | 1 | AO1 | REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701031010/ | Quick Look | ![]() |
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196 | NGC 1068 | 40.6928 | -0.0667 | 40.052721 | -0.278811 | 38.248989 | -15.097296 | 172.18986515 | -51.95763403 | 248.588 | 54141.0038078704 | 2007-02-10 00:05:29 | 54141.9168287037 | 2007-02-10 22:00:14 | 701039010 | 41.6229 | 35 | 41.6309 | 41.6309 | 0 | 41.6229 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8024 | 41.8024 | 78.8839 | 0 | PROCESSED | 57537.346875 | 2016-05-29 08:19:30 | 54525 | 2008-02-29 00:00:00 | 54151.5012962963 | 2007-02-20 12:01:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AARON STEFFEN | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701039010/ | Quick Look | ![]() |
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197 | MARKARIAN 509 | 311.0427 | -10.7271 | 310.361616 | -10.908673 | 310.545205 | 7.124386 | 35.96837179 | -29.85867019 | 254.3019 | 54022.3263888889 | 2006-10-14 07:50:00 | 54023.0856365741 | 2006-10-15 02:03:19 | 701093020 | 25.9298 | 25 | 25.9618 | 25.9298 | 25.9538 | 25.9618 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23.4497 | 23.4497 | 65.5899 | 1 | PROCESSED | 57535.8399305556 | 2016-05-27 20:09:30 | 54526 | 2008-03-01 00:00:00 | 54053.6032638889 | 2006-11-14 14:28:42 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093020/ | Quick Look | ![]() |
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198 | MARKARIAN 509 | 311.0451 | -10.7278 | 310.364015 | -10.909382 | 310.547312 | 7.12309 | 35.96880101 | -29.86110163 | 254.2048 | 54066.1625810185 | 2006-11-27 03:54:07 | 54067.12875 | 2006-11-28 03:05:24 | 701093040 | 33.0944 | 32 | 33.0944 | 33.0944 | 0 | 33.0944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.4544 | 29.4544 | 83.4659 | 1 | PROCESSED | 57536.2044212963 | 2016-05-28 04:54:22 | 54456 | 2007-12-22 00:00:00 | 54088.5895023148 | 2006-12-19 14:08:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093040/ | Quick Look | ![]() |
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199 | PKS 1510-089 | 228.2108 | -9.1043 | 227.537329 | -8.917552 | 228.287746 | 8.492539 | 351.2856545 | 40.1353659 | 286.8003 | 53949.3968634259 | 2006-08-02 09:31:29 | 53952.2544444445 | 2006-08-05 06:06:24 | 701094010 | 119.1577 | 120 | 119.1577 | 119.1577 | 119.1657 | 119.1657 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 106.2588 | 106.2588 | 246.8638 | 5 | PROCESSED | 57535.1605208333 | 2016-05-27 03:51:09 | 54394 | 2007-10-21 00:00:00 | 54018.7363194444 | 2006-10-10 17:40:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013016 | It has been a long mystery (i) how the relativistic jets are formed, and (ii) what is the composition of a jet. In the theoretical view, strong magnetic field (u_B >> u_e) is necessary to produce such outflows with baryonic matters, but observations favor opposite scenario, namely particle dominated (u_e >> u_B), leptonic jet. Such discrepancies can be resolved if moderate numbers of protons (n_e/n_p > 50) are mixed in the non-tnermal pair populations. This can be easily tested if we can observe characteristic "soft X-ray bump" produced by the bulk-Comptonization of UV photons emitted from an accretion disk. We propose a deep observation (40ksec x3) of an EGRET quasar PKS 1510-089, which shows a clear sign of soft X-ray bump in BeppoSAX, ROSAT and ASCA observations. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JUN KATAOKA | GRZEGORZ MADEJSKI | JUS | 1 | AO1 | DIRECT TESTING THE JET COMPOSITION IN A POWERFUL EGRET QUASAR PKS 1510-089 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701094010/ | Quick Look | ![]() |
200 | Z8852 | 347.6318 | 7.5789 | 346.999079 | 7.307292 | 351.631711 | 11.858062 | 84.17423864 | -47.55525942 | 260.3346 | 54065.5867013889 | 2006-11-26 14:04:51 | 54066.1543287037 | 2006-11-27 03:42:14 | 801074010 | 14.8526 | 15 | 14.8526 | 14.8526 | 0 | 14.8526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.9834 | 13.9834 | 49.0379 | 0 | PROCESSED | 57536.1918402778 | 2016-05-28 04:36:15 | 54695 | 2008-08-17 00:00:00 | 54088.6000694444 | 2006-12-19 14:24:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801074010/ | Quick Look | ![]() |
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201 | A2495 | 342.5662 | 10.9218 | 341.941655 | 10.656649 | 348.262816 | 16.910805 | 81.19678392 | -41.92445268 | 65.1354 | 54260.5857523148 | 2007-06-09 14:03:29 | 54261.1668287037 | 2007-06-10 04:00:14 | 801080020 | 25.7806 | 18 | 25.7806 | 25.7806 | 0 | 25.7806 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.9762 | 20.9762 | 50.1959 | 2 | PROCESSED | 57538.8757291667 | 2016-05-30 21:01:03 | 54695 | 2008-08-17 00:00:00 | 54270.430625 | 2007-06-19 10:20:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080020/ | Quick Look | ![]() |
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202 | NGC 1667 | 72.1445 | -6.2644 | 71.533156 | -6.35119 | 69.717897 | -28.457954 | 203.99435404 | -30.10712566 | 81.9813 | 53964.3614814815 | 2006-08-17 08:40:32 | 53965.2536805556 | 2006-08-18 06:05:18 | 701006010 | 39.253 | 40 | 39.253 | 39.261 | 39.261 | 39.261 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.7281 | 35.7281 | 77.0759 | 0 | PROCESSED | 57535.2875578704 | 2016-05-27 06:54:05 | 54526 | 2008-03-01 00:00:00 | 54020.7803009259 | 2006-10-12 18:43:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701006010/ | Quick Look | ![]() |
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203 | NGC4418 | 186.7074 | -0.9383 | 186.066307 | -0.661629 | 186.526079 | 1.80107 | 290.03230216 | 61.31559989 | 292.8039 | 53929.4791898148 | 2006-07-13 11:30:02 | 53931.280775463 | 2006-07-15 06:44:19 | 701001010 | 68.3485 | 70 | 68.3485 | 68.3485 | 68.3485 | 68.3485 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57.1103 | 57.1103 | 155.634 | 1 | PROCESSED | 57534.9858564815 | 2016-05-26 23:39:38 | 54408 | 2007-11-04 00:00:00 | 53942.4601388889 | 2006-07-26 11:02:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701001010/ | Quick Look | ![]() |
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204 | PKS 0558-504 | 89.9338 | -50.4417 | 89.630316 | -50.442779 | 89.864771 | -73.883563 | 257.95388656 | -28.57696937 | 207.8266 | 54117.4686226852 | 2007-01-17 11:14:49 | 54118.1127777778 | 2007-01-18 02:42:24 | 701011010 | 20.6207 | 20 | 20.6207 | 20.6207 | 0 | 20.6207 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.914 | 18.914 | 55.6479 | 0 | PROCESSED | 57536.8527777778 | 2016-05-28 20:28:00 | 54735 | 2008-09-26 00:00:00 | 54133.0355787037 | 2007-02-02 00:51:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011010/ | Quick Look | ![]() |
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205 | PKS 0558-504 | 89.9338 | -50.4409 | 89.630307 | -50.441979 | 89.864775 | -73.882763 | 257.95298672 | -28.57684464 | 209.1054 | 54118.6998032407 | 2007-01-18 16:47:43 | 54119.2654976852 | 2007-01-19 06:22:19 | 701011020 | 18.8753 | 20 | 18.8753 | 18.8753 | 0 | 18.8753 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.0497 | 18.0497 | 48.87 | 1 | PROCESSED | 57536.8739814815 | 2016-05-28 20:58:32 | 54735 | 2008-09-26 00:00:00 | 54133.3967361111 | 2007-02-02 09:31:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011020/ | Quick Look | ![]() |
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206 | KAZ 102 | 270.6661 | 67.6374 | 270.701804 | 67.634057 | 77.059679 | 88.893324 | 97.62313354 | 29.55178422 | 2.066 | 53895.6833101852 | 2006-06-09 16:23:58 | 53896.5343055556 | 2006-06-10 12:49:24 | 701012010 | 41.454 | 40 | 41.454 | 41.462 | 41.47 | 41.47 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40.9507 | 40.9507 | 73.5199 | 2 | PROCESSED | 57534.6269328704 | 2016-05-26 15:02:47 | 54394 | 2007-10-21 00:00:00 | 53928.2501157407 | 2006-07-12 06:00:10 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010112 | We propose to make a detailed broad-band X-ray spectroscopic study of the radio quiet QSO (RQQ) Kaz 102. This RQQ had a power-law spectrum with a photon index ~ 1 with our ASCA observation. We also found a spectral variability over the time scale of years, from ~ 2.2 during the ROSAT All Sky Survey to ~ 1 during the Einstein / ASCA observations. From our ASCA spectra, we couldn't discriminate whether the apparently unusual hard spectrum was caused by warm absorber, Compton reflection, or a simple featureless power-law continuum. High quality and wide-band spectroscopy with Suzaku is essential to unveil the physical nature of the enigmatic hardness and spectral variability of Kaz 102. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YOSHITAKA ISHISAKI | JAP | 1 | AO1 | WHAT IS THE PHYSICAL NATURE OF KAZ 102: AN ENIGMATIC X-RAY HARD RADIO QUIET QSO? | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701012010/ | Quick Look | ![]() |
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207 | 1ES1218+304 | 185.3064 | 30.1169 | 184.679878 | 30.394195 | 171.661841 | 29.481192 | 186.88913956 | 82.72978014 | 298.9428 | 53874.8006365741 | 2006-05-19 19:12:55 | 53876.706412037 | 2006-05-21 16:57:14 | 701025010 | 79.8692 | 80 | 79.8852 | 79.8692 | 79.8852 | 79.8772 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.5118 | 70.5118 | 164.6379 | 2 | PROCESSED | 57534.4292013889 | 2016-05-26 10:18:03 | 54398 | 2007-10-25 00:00:00 | 53927.8564930556 | 2006-07-11 20:33:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701025010/ | Quick Look | ![]() |
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208 | 1ES1426+428 | 217.0716 | 42.6249 | 216.585066 | 42.847682 | 193.182318 | 52.911489 | 77.44668506 | 64.96380656 | 316.1862 | 53902.7388310185 | 2006-06-16 17:43:55 | 53904.2225 | 2006-06-18 05:20:24 | 701026010 | 60.9149 | 60 | 60.9149 | 60.9149 | 60.9149 | 60.9149 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.0911 | 54.0911 | 128.16 | 1 | PROCESSED | 57534.6747800926 | 2016-05-26 16:11:41 | 54400 | 2007-10-27 00:00:00 | 53928.3009143518 | 2006-07-12 07:13:19 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701026010/ | Quick Look | ![]() |
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209 | MRK 501 | 253.4 | 39.7089 | 252.98087 | 39.789378 | 242.4893 | 61.571247 | 63.52834502 | 38.90621529 | 316.9908 | 53934.7872569444 | 2006-07-18 18:53:39 | 53935.7272916667 | 2006-07-19 17:27:18 | 701027010 | 42.4271 | 40 | 42.4389 | 42.4389 | 42.4271 | 42.4351 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.9711 | 39.9711 | 81.2099 | 0 | PROCESSED | 57534.9978587963 | 2016-05-26 23:56:55 | 54408 | 2007-11-04 00:00:00 | 53971.6784259259 | 2006-08-24 16:16:56 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701027010/ | Quick Look | ![]() |
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210 | NGC 4552 | 188.9456 | 12.612 | 188.314388 | 12.887225 | 183.105993 | 15.109639 | 287.9907408 | 75.02773792 | 120.0696 | 54072.312974537 | 2006-12-03 07:30:41 | 54072.8405092593 | 2006-12-03 20:10:20 | 701037010 | 20.4398 | 20 | 20.4398 | 20.4398 | 0 | 20.4398 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.553 | 16.553 | 45.5439 | 0 | PROCESSED | 57536.226875 | 2016-05-28 05:26:42 | 54455 | 2007-12-21 00:00:00 | 54088.5410069444 | 2006-12-19 12:59:03 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AARON STEFFEN | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701037010/ | Quick Look | ![]() |
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211 | PDS 456 | 262.0807 | -14.2604 | 261.370018 | -14.220332 | 262.221238 | 8.96686 | 10.39565911 | 11.16772638 | 98.239 | 54155.7486574074 | 2007-02-24 17:58:04 | 54160.0355787037 | 2007-03-01 00:51:14 | 701056010 | 190.6002 | 188 | 190.6082 | 190.6002 | 0 | 190.6142 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 176.4708 | 176.4708 | 370.3428 | 4 | PROCESSED | 57537.5850578704 | 2016-05-29 14:02:29 | 54757 | 2008-10-18 00:00:00 | 54168.6244560185 | 2007-03-09 14:59:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011351 | A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | JAMES REEVES | USA | 1 | AO1 | SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701056010/ | Quick Look | ![]() |
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212 | BL LACERTAE | 330.6466 | 42.3471 | 330.130697 | 42.105096 | 354.282545 | 49.658149 | 92.61224541 | -10.37092111 | 71.9797 | 53882.2303703704 | 2006-05-27 05:31:44 | 53883.305775463 | 2006-05-28 07:20:19 | 701073010 | 48.5294 | 50 | 48.5454 | 48.5454 | 48.5294 | 48.5374 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.5443 | 35.5443 | 92.902 | 1 | PROCESSED | 57534.4514236111 | 2016-05-26 10:50:03 | 54401 | 2007-10-28 00:00:00 | 53926.2373032407 | 2006-07-10 05:41:43 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011377 | We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRZEGORZ MADEJSKI | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701073010/ | Quick Look | ![]() |
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213 | MARKARIAN 509 | 311.0194 | -10.6637 | 310.338544 | -10.845188 | 310.53976 | 7.19158 | 36.02321332 | -29.81091499 | 73.1708 | 53850.7831481482 | 2006-04-25 18:47:44 | 53851.5252199074 | 2006-04-26 12:36:19 | 701093010 | 24.5756 | 25 | 24.5756 | 24.5756 | 24.5916 | 24.5916 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15.407 | 15.407 | 64.0979 | 1 | PROCESSED | 57533.5586342593 | 2016-05-25 13:24:26 | 54394 | 2007-10-21 00:00:00 | 53907.6894560185 | 2006-06-21 16:32:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GABRIELE PONTI | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701093010/ | Quick Look | ![]() |
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214 | A2104N | 235.0318 | -3.1802 | 234.37876 | -3.019346 | 233.471257 | 15.936264 | 2.94593816 | 39.29281704 | 117.689 | 54119.2779166667 | 2007-01-19 06:40:12 | 54119.7522337963 | 2007-01-19 18:03:13 | 801002010 | 18.8424 | 20 | 18.8424 | 18.8424 | 0 | 18.8424 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.6448 | 13.6448 | 40.9779 | 1 | PROCESSED | 57536.8705439815 | 2016-05-28 20:53:35 | 54735 | 2008-09-26 00:00:00 | 54133.3893518518 | 2007-02-02 09:20:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801002010/ | Quick Look | ![]() |
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215 | NGC 507 | 20.9105 | 33.2598 | 20.206045 | 32.999169 | 32.202982 | 22.611804 | 130.6367604 | -29.12969375 | 54.0771 | 53944.6189351852 | 2006-07-28 14:51:16 | 53946.5544444444 | 2006-07-30 13:18:24 | 801017010 | 79.5013 | 80 | 79.5253 | 79.5013 | 79.5253 | 79.5253 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 80.2867 | 80.2867 | 167.17 | 2 | PROCESSED | 57535.1047222222 | 2016-05-27 02:30:48 | 54394 | 2007-10-21 00:00:00 | 53955.7736689815 | 2006-08-08 18:34:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010061 | We propose to observe luminous elliptical galaxies NGC 507 and NGC 499 for 80 and 100 ksec, respectively, to study abundance distribution of Fe and O. The good energy resolution and low background of the XIS instrument is crucial for this study, and we can perform the first reliable measurement of O distribution around elliptical galaxies. Comparison of O and Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. Comparison of NGC 507 and NGC 499 will show us how much metal production process differ with galaxy size. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 1 | AO1 | CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801017010/ | Quick Look | ![]() |
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216 | OPHIUCHUS CLUSTER 2 | 257.7375 | -23.3864 | 256.979428 | -23.325463 | 258.749053 | -0.422802 | 0.3572282 | 9.54416529 | 94.9391 | 54181.1423726852 | 2007-03-22 03:25:01 | 54181.825162037 | 2007-03-22 19:48:14 | 801023010 | 24.6782 | 15 | 24.7022 | 24.6942 | 0 | 24.6782 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.2781 | 21.2781 | 58.9879 | 1 | PROCESSED | 57537.9744097222 | 2016-05-29 23:23:09 | 54736 | 2008-09-27 00:00:00 | 54209.5433217593 | 2007-04-19 13:02:23 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801023010/ | Quick Look | ![]() |
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217 | A2319CENTER | 290.3341 | 43.878 | 289.944223 | 43.782148 | 306.012819 | 64.798086 | 75.63759851 | 13.45022652 | 251.6652 | 54035.9326041667 | 2006-10-27 22:22:57 | 54038.1466898148 | 2006-10-30 03:31:14 | 801040010 | 99.5332 | 100 | 99.5492 | 99.5412 | 99.5332 | 99.5492 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.9548 | 93.9548 | 191.268 | 2 | PROCESSED | 57535.9905555556 | 2016-05-27 23:46:24 | 54735 | 2008-09-26 00:00:00 | 54063.5741666667 | 2006-11-24 13:46:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010085 | We propose the observations of the A2319 cluster with the Suzaku HXD and XIS to investigate particle acceleration processes in the intracluster medium(ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will detect non-thermal hard X-ray with HXD, and determine the velocity difference between the two subclusters with XIS. With these results, we will determine dynamical status of the ICM and get implications on the particle acceleration processes. We will compare the results with theoretical models, numerical simulations, and radio and optical observations to get an overall picture of particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MOTOKAZU TAKIZAWA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE A2319 CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801040010/ | Quick Look | ![]() |
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218 | PERSEUS CL OFFSET | 50.5735 | 41.8053 | 49.742345 | 41.626976 | 59.178685 | 22.492416 | 150.80595618 | -12.75877318 | 65.9956 | 53982.1426736111 | 2006-09-04 03:25:27 | 53982.4377893518 | 2006-09-04 10:30:25 | 801049040 | 10.4206 | 30 | 10.4206 | 10.4206 | 10.4206 | 10.4206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7.5402 | 7.5402 | 25.4679 | 1 | PROCESSED | 57535.4390856482 | 2016-05-27 10:32:17 | 54526 | 2008-03-01 00:00:00 | 54021.0033680556 | 2006-10-13 00:04:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049040/ | Quick Look | ![]() |
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219 | NGC3923 | 177.7599 | -28.8047 | 177.126048 | -28.526534 | 190.367331 | -27.106442 | 287.27787622 | 32.22445477 | 293.1988 | 53899.8430671296 | 2006-06-13 20:14:01 | 53902.7293287037 | 2006-06-16 17:30:14 | 801054010 | 115.82 | 120 | 115.828 | 115.82 | 115.828 | 115.828 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 107.7313 | 107.7313 | 249.3528 | 3 | PROCESSED | 57534.7187731482 | 2016-05-26 17:15:02 | 54394 | 2007-10-21 00:00:00 | 53927.2880902778 | 2006-07-11 06:54:51 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010100 | We propose to observe an isolated elliptical galaxy NGC3923, to meaasure a dark matter distribution. The large effective area and stable low background of XIS enable us to measure a faint extended X-ray emission such as the periphery of elliptical galaxies more accurately than ever. Since X-ray bright elliptical galaxies have been found to be surrounded by group-scale emission, X-ray faint elliptical galaxies are the best to investigate the dark matter associated with the galaxy itself. The dark matter around galaxies is a key to resolve the problem of why X-ray bright and faint elliptical galaxies exist. The oxygen abundance distribution is also useful to probe the above issue. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YASUSHI FUKAZAWA | JAP | 1 | AO1 | ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801054010/ | Quick Look | ![]() |
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220 | NGC 4472 | 187.4441 | 8.005 | 186.80838 | 8.281234 | 183.627851 | 10.299036 | 286.9163593 | 70.20028227 | 117.8054 | 54072.8427893518 | 2006-12-03 20:13:37 | 54075.7014699074 | 2006-12-06 16:50:07 | 801064010 | 121.0358 | 120 | 121.0358 | 121.0358 | 0 | 121.0358 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.4464 | 103.4464 | 246.9548 | 6 | PROCESSED | 57536.3089467593 | 2016-05-28 07:24:53 | 54702 | 2008-08-24 00:00:00 | 54089.1857523148 | 2006-12-20 04:27:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801064010/ | Quick Look | ![]() |
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221 | NGC 4649 | 190.9148 | 11.557 | 190.284732 | 11.830628 | 185.371113 | 14.926523 | 295.86493189 | 74.32191724 | 113.3108 | 54098.4203703704 | 2006-12-29 10:05:20 | 54104.1473263889 | 2007-01-04 03:32:09 | 801065010 | 224.0304 | 120 | 224.0304 | 224.0304 | 0 | 224.0304 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3042 | 26.3042 | 69.2898 | 1 | PROCESSED | 57536.4300578704 | 2016-05-28 10:19:17 | 54743 | 2008-10-04 00:00:00 | 54132.9809027778 | 2007-02-01 23:32:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801065010/ | Quick Look | ![]() |
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222 | UGC03957 | 115.2433 | 55.429 | 114.235063 | 55.545488 | 106.863653 | 33.455815 | 162.22286538 | 28.93195726 | 271.243 | 53841.9927314815 | 2006-04-16 23:49:32 | 53842.2828587963 | 2006-04-17 06:47:19 | 801072010 | 10.7714 | 12 | 10.7794 | 10.7794 | 10.7874 | 10.7714 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.642 | 9.642 | 25.0079 | 0 | PROCESSED | 57533.4729166667 | 2016-05-25 11:21:00 | 54401 | 2007-10-28 00:00:00 | 53906.7753240741 | 2006-06-20 18:36:28 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801072010/ | Quick Look | ![]() |
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223 | A272 | 28.7603 | 33.9026 | 28.031098 | 33.657734 | 38.955118 | 20.665911 | 137.73606223 | -27.1341127 | 64.9465 | 53943.0449537037 | 2006-07-27 01:04:44 | 53943.6842476852 | 2006-07-27 16:25:19 | 801084010 | 22.2455 | 21 | 22.2535 | 22.2535 | 22.2455 | 22.2535 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.6035 | 24.6035 | 55.2319 | 0 | PROCESSED | 57535.0602430556 | 2016-05-27 01:26:45 | 54401 | 2007-10-28 00:00:00 | 53955.6516782407 | 2006-08-08 15:38:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801084010/ | Quick Look | ![]() |
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224 | A566 | 106.0915 | 63.2647 | 104.91759 | 63.339113 | 99.420321 | 40.34898 | 152.76309519 | 25.45548296 | 285.637 | 54178.3128587963 | 2007-03-19 07:30:31 | 54178.8029976852 | 2007-03-19 19:16:19 | 801085010 | 22.2711 | 20 | 22.2711 | 22.2711 | 0 | 22.2711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.1523 | 22.1523 | 42.3399 | 0 | PROCESSED | 57537.7151157407 | 2016-05-29 17:09:46 | 54695 | 2008-08-17 00:00:00 | 54185.9799305556 | 2007-03-26 23:31:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801085010/ | Quick Look | ![]() |
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225 | RXJ 0658 | 104.704 | -55.933 | 104.461428 | -55.862903 | 130.333928 | -77.302143 | 266.02429497 | -21.20357002 | 164.9362 | 54095.6181597222 | 2006-12-26 14:50:09 | 54098.4099421296 | 2006-12-29 09:50:19 | 801089010 | 101.3845 | 100 | 101.3845 | 101.3845 | 0 | 101.3845 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.3679 | 84.3679 | 241.1547 | 2 | PROCESSED | 57637.5971180556 | 2016-09-06 14:19:51 | 54702 | 2008-08-24 00:00:00 | 54111.5842013889 | 2007-01-11 14:01:15 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011448 | We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | VAHE PETROSIAN | USA | 1 | AO1 | HARD X-RAY EMISSION FROM CLUSTER RXJ0658 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801089010/ | Quick Look | ![]() |
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226 | RXJ1713-3946 | 258.5527 | -40.0289 | 257.68331 | -39.971559 | 260.849002 | -16.950052 | 347.19063141 | -0.73133412 | 268.0015 | 53997.9147569444 | 2006-09-19 21:57:15 | 53998.4425925926 | 2006-09-20 10:37:20 | 501070010 | 20.7442 | 20 | 20.7442 | 20.7522 | 20.7522 | 20.7522 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 22.0266 | 22.0266 | 45.5959 | 1 | PROCESSED | 57535.6347685185 | 2016-05-27 15:14:04 | 54526 | 2008-03-01 00:00:00 | 54021.1763541667 | 2006-10-13 04:13:57 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501070010/ | Quick Look | ![]() |
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227 | COMA RADIO HALO | 194.9267 | 27.9061 | 194.323466 | 28.175433 | 181.517491 | 31.325949 | 56.39742233 | 88.00849705 | 295.2687 | 53886.8435300926 | 2006-05-31 20:14:41 | 53890.7439699074 | 2006-06-04 17:51:19 | 801097010 | 178.6572 | 180 | 178.6892 | 178.6572 | 178.7132 | 178.6892 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 167.4506 | 167.4506 | 336.9758 | 7 | PROCESSED | 57534.5953472222 | 2016-05-26 14:17:18 | 54401 | 2007-10-28 00:00:00 | 53926.6760416667 | 2006-07-10 16:13:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014446 | We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | CRAIG SARAZIN | KYOKO MATSUSHITA | USJ | 1 | AO1 | NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801097010/ | Quick Look | ![]() |
228 | OPHIUCHUS CLUSTER BG | 257.0147 | -25.0612 | 256.247464 | -24.996818 | 258.237934 | -2.148508 | 358.58755189 | 9.10838139 | 89.7146 | 54183.5662268518 | 2007-03-24 13:35:22 | 54183.9169444444 | 2007-03-24 22:00:24 | 801030010 | 15.2983 | 15 | 15.3063 | 15.3063 | 0 | 15.2983 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6351 | 14.6351 | 30.296 | 0 | PROCESSED | 57537.9841898148 | 2016-05-29 23:37:14 | 54736 | 2008-09-27 00:00:00 | 54209.5187384259 | 2007-04-19 12:26:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801030010/ | Quick Look | ![]() |
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229 | AWM7 WEST OFFSET | 43.2295 | 41.594 | 42.421509 | 41.389857 | 53.412323 | 23.911285 | 146.06522235 | -15.7568529 | 90.4999 | 53953.2407060185 | 2006-08-06 05:46:37 | 53954.2343171296 | 2006-08-07 05:37:25 | 801037010 | 39.8177 | 40 | 39.8497 | 39.8177 | 39.8497 | 39.8497 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.1089 | 38.1089 | 85.8359 | 1 | PROCESSED | 57535.2509375 | 2016-05-27 06:01:21 | 54394 | 2007-10-21 00:00:00 | 54020.7562384259 | 2006-10-12 18:08:59 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801037010/ | Quick Look | ![]() |
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230 | A2256 | 256.0138 | 78.7112 | 256.73222 | 78.776756 | 102.386288 | 77.234603 | 111.08264828 | 31.72462704 | 207.9671 | 54049.8560069445 | 2006-11-10 20:32:39 | 54052.0834722222 | 2006-11-13 02:00:12 | 801061010 | 95.5111 | 100 | 95.5111 | 95.5111 | 0 | 95.5111 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.5789 | 103.5789 | 192.4418 | 4 | PROCESSED | 57536.1203009259 | 2016-05-28 02:53:14 | 54456 | 2007-12-22 00:00:00 | 54089.4338425926 | 2006-12-20 10:24:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010139 | A2256 is a nearby (z=0.058) rich cluster with strong X-ray emission. The cluster has variety of indications of a on-going merger; two peaks separated by 3.5 arcmin are clearly visible near the center of X-ray emission, gas temperature map show sub structure and a cold front etc. The velocity distribution of member galaxies also exhibits two or three sub groups in this cluster. We measure the bulk motion of the hot gas using Suzaku XIS, in particular, about 2000km/s velocity difference between the main-cluster and the sub-cluster is the target. We also aim to search for hard X-ray emission claimed by previous missions with Suzaku HXD. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801061010/ | Quick Look | ![]() |
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231 | SERSIC 159-03 | 348.4959 | -42.7314 | 347.802109 | -43.003937 | 330.666566 | -34.355163 | 348.33340728 | -64.81387916 | 47.3295 | 53851.5323611111 | 2006-04-26 12:46:36 | 53853.2668055556 | 2006-04-28 06:24:12 | 801093010 | 67.7843 | 70 | 67.8003 | 67.8003 | 67.7843 | 67.7923 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41.5833 | 41.5833 | 149.8278 | 2 | PROCESSED | 57533.6210532407 | 2016-05-25 14:54:19 | 54400 | 2007-10-27 00:00:00 | 53907.8625231482 | 2006-06-21 20:42:02 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012045 | We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JELLE KAASTRA | EUR | 1 | AO1 | O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN? | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801093010/ | Quick Look | ![]() |
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232 | GALACTIC CENTER GC10 | 266.4308 | -29.5343 | 265.632731 | -29.515028 | 266.867639 | -6.131965 | 359.50116476 | -0.33080245 | 109.7996 | 54171.9994097222 | 2007-03-12 23:59:09 | 54172.6529976852 | 2007-03-13 15:40:19 | 501055010 | 27.2257 | 25 | 27.2257 | 27.2497 | 0 | 27.2337 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1819 | 21.1819 | 56.4539 | 0 | PROCESSED | 57537.6665740741 | 2016-05-29 15:59:52 | 54736 | 2008-09-27 00:00:00 | 54182.3161342593 | 2007-03-23 07:35:14 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501055010/ | Quick Look | ![]() |
233 | A2061 | 230.3095 | 30.6453 | 229.795666 | 30.824015 | 216.361499 | 46.967712 | 48.13899774 | 57.1713197 | 293.2901 | 53943.6955092593 | 2006-07-27 16:41:32 | 53943.9946643518 | 2006-07-27 23:52:19 | 801081010 | 13.8887 | 14 | 13.9047 | 13.9047 | 13.8887 | 13.8967 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 11.8443 | 11.8443 | 25.8399 | 0 | PROCESSED | 57535.0552083333 | 2016-05-27 01:19:30 | 54401 | 2007-10-28 00:00:00 | 53955.6442939815 | 2006-08-08 15:27:47 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801081010/ | Quick Look | ![]() |
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234 | A2249 | 257.46 | 34.4851 | 257.00595 | 34.546595 | 250.753931 | 57.089244 | 57.64541352 | 34.94797305 | 129.9858 | 54114.5939467593 | 2007-01-14 14:15:17 | 54115.1252777778 | 2007-01-15 03:00:24 | 801082010 | 22.8156 | 15 | 22.8156 | 22.8236 | 0 | 22.8236 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.7637 | 19.7637 | 45.9039 | 1 | PROCESSED | 57536.8308333333 | 2016-05-28 19:56:24 | 54695 | 2008-08-17 00:00:00 | 54133.0295833333 | 2007-02-02 00:42:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801082010/ | Quick Look | ![]() |
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235 | GALACTIC CENTER GC9 | 266.6299 | -29.2499 | 265.833607 | -29.231598 | 267.035089 | -5.843458 | 359.83430056 | -0.33104727 | 109.8001 | 54171.3410532407 | 2007-03-12 08:11:07 | 54171.9988888889 | 2007-03-12 23:58:24 | 501054010 | 26.1044 | 25 | 26.1044 | 26.1044 | 0 | 26.1044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.5424 | 23.5424 | 56.8299 | 0 | PROCESSED | 57537.6542013889 | 2016-05-29 15:42:03 | 54736 | 2008-09-27 00:00:00 | 54182.2954166667 | 2007-03-23 07:05:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501054010/ | Quick Look | ![]() |
236 | JUPITER | 226.6349 | -16.1983 | 225.936085 | -16.00589 | 228.727521 | 1.247844 | 344.01962259 | 35.67652355 | 118.4908 | 53793.86 | 2006-02-27 20:38:24 | 53794.9585532407 | 2006-02-28 23:00:19 | 401001040 | 42.2558 | 36 | 42.2638 | 42.2638 | 42.2638 | 42.2558 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.7067 | 35.7067 | 94.9059 | 2 | PROCESSED | 57533.1103819444 | 2016-05-25 02:38:57 | 54401 | 2007-10-28 00:00:00 | 53906.5712615741 | 2006-06-20 13:42:37 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | RONALD ELSNER | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401001040/ | Quick Look | ![]() |
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237 | NGC 5044 | 198.8504 | -16.3899 | 198.183934 | -16.125889 | 203.593771 | -7.791309 | 311.2339251 | 46.09520433 | 290.0016 | 53918.7631712963 | 2006-07-02 18:18:58 | 53919.3600115741 | 2006-07-03 08:38:25 | 801046010 | 19.7466 | 20 | 19.7466 | 19.7466 | 19.7466 | 19.7466 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.9716 | 17.9716 | 51.562 | 1 | PROCESSED | 57534.8255208333 | 2016-05-26 19:48:45 | 54394 | 2007-10-21 00:00:00 | 53930.6133217593 | 2006-07-14 14:43:11 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801046010/ | Quick Look | ![]() |
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238 | XTE J1856+053 | 284.159 | 5.396 | 283.54361 | 5.329341 | 286.008229 | 28.053142 | 38.32644604 | 1.30563349 | 89.2928 | 54178.8141666667 | 2007-03-19 19:32:24 | 54179.4321643518 | 2007-03-20 10:22:19 | 901004010 | 24.476 | 25 | 24.476 | 24.476 | 0 | 24.476 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.1108 | 20.1108 | 53.3919 | 0 | PROCESSED | 57537.7386805556 | 2016-05-29 17:43:42 | 54171 | 2007-03-12 00:00:00 | 54185.38 | 2007-03-26 09:07:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017020 | Observation for a outburst of XTE J1856+053 (ATEL #1024) | GALACTIC POINT SOURCES | 9 | A | SWG | JAP | 1 | TOO | TOO OBSERVATION OF XTE J1856+053 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901004010/ | Quick Look | ![]() |
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239 | 4U 1705-44 | 257.2313 | -44.1028 | 256.328133 | -44.039108 | 260.196098 | -21.094402 | 343.32206131 | -2.34487049 | 297.0793 | 54014.4242708333 | 2006-10-06 10:10:57 | 54015.0891087963 | 2006-10-07 02:08:19 | 401046030 | 20.065 | 20 | 20.065 | 20.065 | 20.065 | 20.065 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.9196 | 17.9196 | 57.4239 | 2 | PROCESSED | 57535.7945138889 | 2016-05-27 19:04:06 | 54526 | 2008-03-01 00:00:00 | 54021.6765162037 | 2006-10-13 16:14:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046030/ | Quick Look | ![]() |
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240 | PERSEUS CLUSTER | 49.9436 | 41.5175 | 49.116107 | 41.336843 | 58.603575 | 22.345195 | 150.56798595 | -13.25929387 | 66.0393 | 53976.788275463 | 2006-08-29 18:55:07 | 53980.0793865741 | 2006-09-02 01:54:19 | 101012010 | 150.9051 | 150 | 150.9051 | 150.9211 | 150.9371 | 150.9211 | 6 | 6 | 6 | 6 | 1 | 0 | 0 | 142.5334 | 142.5334 | 284.336 | 3 | PROCESSED | 57535.5159375 | 2016-05-27 12:22:57 | 53826 | 2006-04-01 00:00:00 | 54024.8648726852 | 2006-10-16 20:45:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015016 | We propose the observation of Perseus cluster for 150ks. To recover the energy resolution of the XIS, we will try the periodic charge injection method. However, the charge injection will change calibrations such as gain, QE and so on dramatically. To study the change of the clibrations, Perseus cluster is one of the best targets, because it is extended over the whole XIS FOV and the iron K line from the cluster is extremely strong. For the first 50ks, the observation will be done with the normal mode without the charge injection. For the second and third 50ks, we will do the charge injections with every 54 and 108 rows, repectively. | CALIBRATION | 1 | A | HIRONORI MATSUMOTO | JAP | 1 | AO1 | PERSEUS OBSERVATION FOR CALIBRATIONS ON THE PERIODIC CHARGE INJECTION METHOD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101012010/ | Quick Look | ![]() |
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241 | M17 | 275.2076 | -16.1829 | 274.486266 | -16.206429 | 275.030512 | 7.16685 | 15.0906551 | -0.7606192 | 110.1996 | 53805.8263425926 | 2006-03-11 19:49:56 | 53808.5349421296 | 2006-03-14 12:50:19 | 501003010 | 102.7021 | 100 | 102.7101 | 102.7101 | 102.7021 | 102.7101 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 92.5661 | 92.5661 | 233.9678 | 4 | PROCESSED | 57533.2492939815 | 2016-05-25 05:58:59 | 54394 | 2007-10-21 00:00:00 | 53905.822662037 | 2006-06-19 19:44:38 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010066 | Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAHIRO TSUJIMOTO | JAP | 1 | AO1 | XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501003010/ | Quick Look | ![]() |
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242 | CTB 37B | 258.4918 | -38.2006 | 257.636889 | -38.143005 | 260.643359 | -15.13191 | 348.64561092 | 0.37683278 | 270.1267 | 53974.0604976852 | 2006-08-27 01:27:07 | 53976.2398032407 | 2006-08-29 05:45:19 | 501007010 | 82.8151 | 80 | 82.8711 | 82.8151 | 82.8791 | 82.8631 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.8603 | 68.8603 | 188.2779 | 2 | PROCESSED | 57535.4428703704 | 2016-05-27 10:37:44 | 54526 | 2008-03-01 00:00:00 | 54053.4840162037 | 2006-11-14 11:36:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010042 | The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the extended sample with radio SNR counterpart, CTB 37B, which is marginally detected on the edge of ASCA GIS. ASCA spectrum shows rather soft power-law feature, indicating that there are both thermal and non-thermal X-ray emission. With the low background of XISs and HXD, parameters of both components are determined with 80 ks exposure. The non-thermal component suggests the new sample of accelerators, and the thermal compopent reveals the condition of the proton acceleration site, for the first time. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 1 | AO1 | UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501007010/ | Quick Look | ![]() |
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243 | GX 339-4 | 255.7025 | -48.7916 | 254.754666 | -48.72059 | 259.573177 | -25.865576 | 338.93635594 | -4.32587966 | 86.7489 | 54143.2316087963 | 2007-02-12 05:33:31 | 54146.2003009259 | 2007-02-15 04:48:26 | 401068010 | 77.2053 | 100 | 83.8935 | 77.2053 | 0 | 82.1138 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.026 | 94.026 | 256.484 | 4 | PROCESSED | 57537.4905208333 | 2016-05-29 11:46:21 | 54535 | 2008-03-10 00:00:00 | 54167.7751851852 | 2007-03-08 18:36:16 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011146 | Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme. | GALACTIC POINT SOURCES | 4 | A | JON MILLER | USA | 1 | AO1-TOO | SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401068010/ | Quick Look | ![]() |
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244 | UGC5101 | 144.0189 | 61.4178 | 143.073331 | 61.641673 | 122.524313 | 43.933823 | 152.38145034 | 42.89433298 | 112.6892 | 54039.7635300926 | 2006-10-31 18:19:29 | 54040.396087963 | 2006-11-01 09:30:22 | 701002020 | 42.166 | 35 | 42.166 | 42.174 | 42.182 | 42.182 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.5589 | 33.5589 | 54.6519 | 0 | PROCESSED | 57536.0043518518 | 2016-05-28 00:06:16 | 54735 | 2008-09-26 00:00:00 | 54063.3945949074 | 2006-11-24 09:28:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002020/ | Quick Look | ![]() |
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245 | PKS 0558-504 | 89.9334 | -50.4402 | 89.629898 | -50.441281 | 89.86386 | -73.882062 | 257.95215413 | -28.57698713 | 210.2147 | 54119.7661805556 | 2007-01-19 18:23:18 | 54120.3203009259 | 2007-01-20 07:41:14 | 701011030 | 21.2563 | 20 | 21.2563 | 21.2563 | 0 | 21.2563 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.1145 | 19.1145 | 47.87 | 0 | PROCESSED | 57536.8847916667 | 2016-05-28 21:14:06 | 54735 | 2008-09-26 00:00:00 | 54133.3934259259 | 2007-02-02 09:26:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YOSHITO HABA | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701011030/ | Quick Look | ![]() |
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246 | SWIFT J1628.1+5145 | 246.9541 | 51.8388 | 246.639575 | 51.948443 | 220.797096 | 71.358115 | 79.81767806 | 42.92326404 | 60.2479 | 53840.7843518518 | 2006-04-15 18:49:28 | 53841.3904976852 | 2006-04-16 09:22:19 | 701016010 | 23.589 | 20 | 23.605 | 23.597 | 23.589 | 23.597 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.6261 | 20.6261 | 52.3599 | 2 | PROCESSED | 57533.4625231482 | 2016-05-25 11:06:02 | 54394 | 2007-10-21 00:00:00 | 53905.7494444444 | 2006-06-19 17:59:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701016010/ | Quick Look | ![]() |
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247 | SS 433 | 287.9531 | 4.9906 | 287.335307 | 4.906206 | 290.183209 | 27.182001 | 39.69950989 | -2.2379409 | 78.6445 | 53829.6109606482 | 2006-04-04 14:39:47 | 53830.5327662037 | 2006-04-05 12:47:11 | 401003010 | 38.6767 | 40 | 38.6767 | 38.6767 | 38.6767 | 38.6767 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.2411 | 28.2411 | 79.634 | 1 | PROCESSED | 57533.395162037 | 2016-05-25 09:29:02 | 54394 | 2007-10-21 00:00:00 | 53906.1478125 | 2006-06-20 03:32:51 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010031 | SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. | GALACTIC POINT SOURCES | 4 | A | NOBUYUKI KAWAI | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401003010/ | Quick Look | ![]() |
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248 | NGC 4151 | 182.6375 | 39.4139 | 182.006166 | 39.692011 | 164.091601 | 36.628069 | 155.05374688 | 75.05753801 | 112.1087 | 54087.8369097222 | 2006-12-18 20:05:09 | 54090.3848726852 | 2006-12-21 09:14:13 | 701034010 | 124.9796 | 125 | 124.9796 | 124.9796 | 0 | 124.9796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131.2741 | 131.2741 | 220.1059 | 3 | PROCESSED | 57536.4582060185 | 2016-05-28 10:59:49 | 54702 | 2008-08-24 00:00:00 | 54132.849537037 | 2007-02-01 20:23:20 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011327 | We propose a 100 ks Suzaku observation of the brightest Seyfert Galaxy in the sky. Given the broad band-pass, and high sensitivity, the proposed observations will provide a high-quality spectrum which will allow us to search for variability in the high-ionized absorber (compared to previous observations). We will be able to obtain stringent constraints on the "Reflection Hump" and compare it to the strength of the Fe Kalpha emission line - thus providing a direct test of Reflection models. The proposed program will also complement observations of fainter and more exotic Seyferts likely to be observed during AO-1. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IAN GEORGE | USA | 1 | AO1 | DECOUPLING THE COMPONENTS IN THE BRIGHTEST SEYFERT: NGC 4151 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701034010/ | Quick Look | ![]() |
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249 | HESS J1837-069 | 279.4395 | -6.8651 | 278.765532 | -6.909152 | 279.755327 | 16.256333 | 25.2664546 | -0.10276403 | 102.6144 | 54164.5341898148 | 2007-03-05 12:49:14 | 54165.4286342593 | 2007-03-06 10:17:14 | 401026010 | 42.1911 | 40 | 42.1911 | 42.1991 | 0 | 42.2071 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7021 | 37.7021 | 77.2599 | 1 | PROCESSED | 57537.6010185185 | 2016-05-29 14:25:28 | 54750 | 2008-10-11 00:00:00 | 54171.2613425926 | 2007-03-12 06:16:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010131 | The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis. | GALACTIC POINT SOURCES | 4 | B | KEN EBISAWA | JAP | 1 | AO1 | INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401026010/ | Quick Look | ![]() |
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250 | APM 08279+5255 | 127.9229 | 52.7639 | 126.990699 | 52.933179 | 116.237243 | 32.72103 | 165.74356471 | 36.23970609 | 100.0676 | 54040.3996643518 | 2006-11-01 09:35:31 | 54041.9690277778 | 2006-11-02 23:15:24 | 701057020 | 102.295 | 100 | 102.303 | 102.311 | 102.311 | 102.295 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 95.624 | 95.624 | 135.5778 | 1 | PROCESSED | 57536.0492592593 | 2016-05-28 01:10:56 | 54695 | 2008-08-17 00:00:00 | 54088.5241782407 | 2006-12-19 12:34:49 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057020/ | Quick Look | ![]() |
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251 | NGC 5728 | 220.5794 | -17.3095 | 219.88301 | -17.096936 | 223.49481 | -1.485509 | 337.26599487 | 38.0606459 | 290.4081 | 53935.7359143518 | 2006-07-19 17:39:43 | 53936.6264930556 | 2006-07-20 15:02:09 | 701079010 | 41.3077 | 40 | 41.3077 | 41.3077 | 41.3077 | 41.3077 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.569 | 39.569 | 76.9419 | 0 | PROCESSED | 57535.0121064815 | 2016-05-27 00:17:26 | 54400 | 2007-10-27 00:00:00 | 53943.5061111111 | 2006-07-27 12:08:48 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANDREA COMASTRI | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701079010/ | Quick Look | ![]() |
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252 | 1RX J154814.5-452845 | 237.0511 | -45.4226 | 236.175049 | -45.269354 | 245.126412 | -24.783918 | 332.46961393 | 7.07040697 | 85.7358 | 54132.6368518518 | 2007-02-01 15:17:04 | 54135.3543865741 | 2007-02-04 08:30:19 | 401037010 | 99.4541 | 100 | 99.4541 | 99.4621 | 0 | 99.4701 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.8552 | 86.8552 | 234.7838 | 3 | PROCESSED | 57537.0252777778 | 2016-05-29 00:36:24 | 54702 | 2008-08-24 00:00:00 | 54139.4767939815 | 2007-02-08 11:26:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401037010/ | Quick Look | ![]() |
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253 | 4U 1705-44 | 257.2281 | -44.1019 | 256.324944 | -44.038193 | 260.193555 | -21.093723 | 343.32141433 | -2.34248879 | 264.0666 | 53996.5173611111 | 2006-09-18 12:25:00 | 53996.8619675926 | 2006-09-18 20:41:14 | 401046020 | 17.134 | 20 | 17.342 | 17.134 | 17.334 | 17.334 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15.4477 | 15.4477 | 29.7679 | 0 | PROCESSED | 57535.6082175926 | 2016-05-27 14:35:50 | 54526 | 2008-03-01 00:00:00 | 54020.9055555556 | 2006-10-12 21:44:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | ANDREW YOUNG | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401046020/ | Quick Look | ![]() |
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254 | GALACTIC CENTER GC11 | 266.231 | -29.8182 | 265.431151 | -29.797955 | 266.700372 | -6.420209 | 359.16839231 | -0.33075371 | 109.7993 | 54172.6536111111 | 2007-03-13 15:41:12 | 54173.2086111111 | 2007-03-14 05:00:24 | 501056010 | 26.5374 | 25 | 26.5454 | 26.5454 | 0 | 26.5374 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2789 | 25.2789 | 47.946 | 0 | PROCESSED | 57537.6702199074 | 2016-05-29 16:05:07 | 54736 | 2008-09-27 00:00:00 | 54182.3328125 | 2007-03-23 07:59:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501056010/ | Quick Look | ![]() |
255 | SWIFTJ2000.6+3210 | 300.0869 | 32.2033 | 299.597811 | 32.064769 | 312.685822 | 51.280995 | 68.99570836 | 1.1443147 | 87.4233 | 53837.6619212963 | 2006-04-12 15:53:10 | 53837.9139351852 | 2006-04-12 21:56:04 | 401053010 | 12.4384 | 20 | 12.444 | 12.4512 | 12.4512 | 12.4384 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.8767 | 9.8767 | 21.7679 | 0 | PROCESSED | 57533.4456134259 | 2016-05-25 10:41:41 | 54775 | 2008-11-05 00:00:00 | 53927.3549189815 | 2006-07-11 08:31:05 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401053010/ | Quick Look | ![]() |
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256 | ABELL 2199 CENTER | 247.1922 | 39.484 | 246.76294 | 39.592842 | 233.179095 | 60.039777 | 62.84241749 | 43.66620611 | 252.3681 | 54009.2972222222 | 2006-10-01 07:08:00 | 54009.8967361111 | 2006-10-01 21:31:18 | 801056010 | 24.9282 | 25 | 25.4799 | 24.9282 | 25.4799 | 25.4799 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.519 | 20.519 | 51.7939 | 1 | PROCESSED | 57535.7247453704 | 2016-05-27 17:23:38 | 54735 | 2008-09-26 00:00:00 | 54021.2246990741 | 2006-10-13 05:23:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801056010/ | Quick Look | ![]() |
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257 | GC SGR D NORTH | 266.9758 | -27.7178 | 266.189062 | -27.7012 | 267.305981 | -4.305004 | 1.30220378 | 0.20283685 | 108.7992 | 54173.2100578704 | 2007-03-14 05:02:29 | 54174.7883564815 | 2007-03-15 18:55:14 | 501058010 | 63.2422 | 63 | 63.2502 | 63.2422 | 0 | 63.2582 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.1479 | 51.1479 | 136.3519 | 0 | PROCESSED | 57537.7302546296 | 2016-05-29 17:31:34 | 54735 | 2008-09-26 00:00:00 | 54182.440462963 | 2007-03-23 10:34:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501058010/ | Quick Look | ![]() |
258 | A3667_NW_17OFF | 302.8177 | -56.56 | 301.819585 | -56.708877 | 291.523842 | -35.547493 | 341.18808838 | -33.22347241 | 74.1682 | 53861.293912037 | 2006-05-06 07:03:14 | 53861.7356944444 | 2006-05-06 17:39:24 | 801095010 | 17.2586 | 20 | 17.2826 | 17.2746 | 17.2666 | 17.2586 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14.2555 | 14.2555 | 38.1519 | 1 | PROCESSED | 57533.636099537 | 2016-05-25 15:15:59 | 54735 | 2008-09-26 00:00:00 | 53913.7593518518 | 2006-06-27 18:13:28 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095010/ | Quick Look | ![]() |
259 | RXJ1713-3946 | 257.9704 | -39.5791 | 257.105134 | -39.519003 | 260.343852 | -16.539668 | 347.29183097 | -0.10508063 | 267.9995 | 53989.172025463 | 2006-09-11 04:07:43 | 53989.5306365741 | 2006-09-11 12:44:07 | 501063010 | 18.422 | 20 | 18.422 | 18.422 | 18.422 | 18.422 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.7597 | 17.7597 | 30.9719 | 1 | PROCESSED | 57535.5249537037 | 2016-05-27 12:35:56 | 54526 | 2008-03-01 00:00:00 | 54021.1086458333 | 2006-10-13 02:36:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501063010/ | Quick Look | ![]() |
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260 | CYGNUS_LOOP_P12 | 313.7421 | 31.2725 | 313.223564 | 31.080937 | 328.639569 | 46.215284 | 74.99964096 | -8.84356964 | 62.1405 | 53864.7943055556 | 2006-05-09 19:03:48 | 53865.1391087963 | 2006-05-10 03:20:19 | 501029010 | 13.5426 | 10 | 13.5426 | 13.5426 | 13.5426 | 13.5426 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2.1567 | 2.1567 | 29.78 | 1 | PROCESSED | 57534.2604166667 | 2016-05-26 06:15:00 | 54394 | 2007-10-21 00:00:00 | 53914.0447916667 | 2006-06-28 01:04:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501029010/ | Quick Look | ![]() |
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261 | 3EGJ1234 1318_1 | 188.0173 | -13.3363 | 187.367898 | -13.060386 | 192.646727 | -9.069223 | 295.70141073 | 49.26333697 | 109.7313 | 54081.3723032407 | 2006-12-12 08:56:07 | 54081.9273032407 | 2006-12-12 22:15:19 | 801031010 | 19.4098 | 20 | 19.4178 | 19.4178 | 0 | 19.4098 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.7228 | 18.7228 | 47.9499 | 1 | PROCESSED | 57536.3099768518 | 2016-05-28 07:26:22 | 54735 | 2008-09-26 00:00:00 | 54094.2359722222 | 2006-12-25 05:39:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010068 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOMONORI TOTANI | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801031010/ | Quick Look | ![]() |
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262 | 3EGJ1234 1318_2 | 188.017 | -13.0869 | 187.367769 | -12.810986 | 192.545784 | -8.84065 | 295.65674578 | 49.51103665 | 109.9322 | 54081.9277777778 | 2006-12-12 22:16:00 | 54082.7766087963 | 2006-12-13 18:38:19 | 801032010 | 30.9427 | 30 | 30.9667 | 30.9587 | 0 | 30.9427 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.083 | 26.083 | 73.3339 | 1 | PROCESSED | 57536.3393055556 | 2016-05-28 08:08:36 | 54735 | 2008-09-26 00:00:00 | 54094.2665740741 | 2006-12-25 06:23:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010068 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOMONORI TOTANI | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801032010/ | Quick Look | ![]() |
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263 | A3667_NW_17OFF | 302.869 | -56.6666 | 301.869632 | -56.815685 | 291.522519 | -35.657764 | 341.06051648 | -33.2513141 | 258.9342 | 54038.8325578704 | 2006-10-30 19:58:53 | 54039.0106944444 | 2006-10-31 00:15:24 | 801095020 | 11.9634 | 10 | 11.9794 | 11.9794 | 11.9634 | 11.9714 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.724 | 8.724 | 15.3839 | 0 | PROCESSED | 57535.9848032407 | 2016-05-27 23:38:07 | 54735 | 2008-09-26 00:00:00 | 54056.1858796296 | 2006-11-17 04:27:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095020/ | Quick Look | ![]() |
264 | SNR 0509-67.5 | 77.3855 | -67.5341 | 77.403087 | -67.594899 | 342.98809 | -84.999306 | 278.15788525 | -34.58671131 | 68.6442 | 53965.2623032407 | 2006-08-18 06:17:43 | 53966.1640509259 | 2006-08-19 03:56:14 | 501041010 | 51.2762 | 50 | 51.2762 | 51.2762 | 51.2762 | 51.2762 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50.8294 | 50.8294 | 77.89 | 1 | PROCESSED | 57535.3081365741 | 2016-05-27 07:23:43 | 54526 | 2008-03-01 00:00:00 | 54020.7617592593 | 2006-10-12 18:16:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010072 | Hot plasma in young supernova remnants (SNRs) are generally in the state of non-equilibrium ionization (NEI), hence strong L-shell lines of Si, Fe and other elements appear in soft energy band (<1keV). With the observations with Chandra and XMM, quite large ambiguity of ionization age for each element remains because of the limited energy resolution in the soft energy band. Utilizing the supreme energy resolution and background property of Suzaku/XIS, we propose the observation of the youngest type Ia SNR in the LMC, 0509-67.5. We correctly diagnose the NEI plasma of this SNR by determining the ionization age and electron temperature for each element component and constrain the ejecta structure of Type Ia SNR. | GALACTIC DIFFUSE EMISSION | 5 | C | HIROSHI NAKAJIMA | JAP | 1 | AO1 | NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501041010/ | Quick Look | ![]() |
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265 | GALACTIC CENTER | 265.9791 | -28.902 | 265.18515 | -28.880549 | 266.454701 | -5.510331 | 359.8343278 | 0.33569605 | 108.8002 | 54169.6271990741 | 2007-03-10 15:03:10 | 54170.1633564815 | 2007-03-11 03:55:14 | 501046010 | 25.211 | 25 | 25.227 | 25.211 | 0 | 25.243 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0087 | 25.0087 | 46.2919 | 0 | PROCESSED | 57537.6350925926 | 2016-05-29 15:14:32 | 54736 | 2008-09-27 00:00:00 | 54179.4773842593 | 2007-03-20 11:27:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501046010/ | Quick Look | ![]() |
266 | GALACTIC CENTER | 265.7083 | -29.9322 | 264.907837 | -29.909421 | 266.247634 | -6.546909 | 358.83372455 | -0.00453222 | 269.0002 | 54017.5695486111 | 2006-10-09 13:40:09 | 54018.2808333333 | 2006-10-10 06:44:24 | 501051010 | 21.869 | 20 | 21.877 | 21.877 | 21.869 | 21.877 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.1322 | 21.1322 | 61.4459 | 0 | PROCESSED | 57535.8166435185 | 2016-05-27 19:35:58 | 54735 | 2008-09-26 00:00:00 | 54053.5109953704 | 2006-11-14 12:15:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501051010/ | Quick Look | ![]() |
267 | RXJ1713-3946 | 258.5534 | -39.7289 | 257.686429 | -39.671569 | 260.823727 | -16.651038 | 347.43430559 | -0.55631777 | 267.9997 | 53991.0497337963 | 2006-09-13 01:11:37 | 53991.4460300926 | 2006-09-13 10:42:17 | 501068010 | 21.0015 | 20 | 21.0175 | 21.0095 | 21.0015 | 21.0255 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.2093 | 21.2093 | 34.2339 | 1 | PROCESSED | 57535.5599537037 | 2016-05-27 13:26:20 | 54526 | 2008-03-01 00:00:00 | 54021.2424537037 | 2006-10-13 05:49:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501068010/ | Quick Look | ![]() |
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268 | A3667_NW_RELIC | 302.5617 | -56.3599 | 301.565299 | -56.507728 | 291.421165 | -35.317169 | 341.42703548 | -33.08195751 | 74.7123 | 53858.7409837963 | 2006-05-03 17:47:01 | 53861.2933449074 | 2006-05-06 07:02:25 | 801094010 | 94.3946 | 95 | 94.4026 | 94.3946 | 94.3946 | 94.4026 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 56.2506 | 56.2506 | 220.489 | 4 | PROCESSED | 57533.7274074074 | 2016-05-25 17:27:28 | 54394 | 2007-10-21 00:00:00 | 53913.7574189815 | 2006-06-27 18:10:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801094010/ | Quick Look | ![]() |
269 | LMC X-3 OFF FIELD 1 | 85.5783 | -64.5441 | 85.521216 | -64.565729 | 45.792643 | -87.283954 | 274.09377866 | -31.6918405 | 324.0002 | 53847.1442361111 | 2006-04-22 03:27:42 | 53848.0099421296 | 2006-04-23 00:14:19 | 501097010 | 43.6067 | 50 | 43.6067 | 43.6067 | 43.6067 | 43.6067 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.0261 | 42.0261 | 74.7459 | 0 | PROCESSED | 57533.5339583333 | 2016-05-25 12:48:54 | 54526 | 2008-03-01 00:00:00 | 53907.3335763889 | 2006-06-21 08:00:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | Q. DANIEL WANG | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097010/ | Quick Look | ![]() |
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270 | MRK 1073 | 48.7401 | 42.0969 | 47.912237 | 41.911835 | 57.846592 | 23.153427 | 149.47083071 | -13.26071681 | 81.0781 | 53949.235162037 | 2006-08-02 05:38:38 | 53949.3834722222 | 2006-08-02 09:12:12 | 701007010 | 3.4746 | 40 | 3.4746 | 3.4806 | 3.4786 | 3.4766 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4.1358 | 4.1358 | 12.806 | 0 | PROCESSED | 57535.0684375 | 2016-05-27 01:38:33 | 54735 | 2008-09-26 00:00:00 | 54132.9684490741 | 2007-02-01 23:14:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701007010/ | Quick Look | ![]() |
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271 | AWM7 EAST OFFSET | 44.0318 | 41.5949 | 43.221288 | 41.393422 | 54.035202 | 23.723269 | 146.61375919 | -15.47239178 | 90.4995 | 53952.2676967593 | 2006-08-05 06:25:29 | 53953.2398611111 | 2006-08-06 05:45:24 | 801036010 | 38.5361 | 40 | 38.5361 | 38.5361 | 38.5361 | 38.5361 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37.541 | 37.541 | 83.9599 | 0 | PROCESSED | 57535.0870138889 | 2016-05-27 02:05:18 | 54394 | 2007-10-21 00:00:00 | 54020.7498726852 | 2006-10-12 17:59:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801036010/ | Quick Look | ![]() |
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272 | MRK421 | 166.0521 | 38.1644 | 165.357194 | 38.434126 | 151.189395 | 29.439264 | 179.96763761 | 64.99940635 | 318.3733 | 53853.2821412037 | 2006-04-28 06:46:17 | 53854.2711226852 | 2006-04-29 06:30:25 | 701024010 | 41.4709 | 40 | 41.4789 | 41.4709 | 41.4789 | 41.4789 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.7033 | 34.7033 | 85.4301 | 1 | PROCESSED | 57533.6140162037 | 2016-05-25 14:44:11 | 54394 | 2007-10-21 00:00:00 | 53908.0343055556 | 2006-06-22 00:49:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701024010/ | Quick Look | ![]() |
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273 | NGC 5506 | 213.312 | -3.2124 | 212.663098 | -2.97888 | 212.190832 | 9.596053 | 339.14600253 | 53.80603682 | 287.3743 | 53955.6875578704 | 2006-08-08 16:30:05 | 53957.003900463 | 2006-08-10 00:05:37 | 701030010 | 47.7531 | 150 | 47.7531 | 47.7531 | 47.7531 | 47.7531 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41.0973 | 41.0973 | 113.7259 | 2 | PROCESSED | 57535.2578587963 | 2016-05-27 06:11:19 | 54695 | 2008-08-17 00:00:00 | 54116.2715740741 | 2007-01-16 06:31:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030010/ | Quick Look | ![]() |
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274 | IRAS08572+3915 | 135.0664 | 39.0091 | 134.264876 | 39.204772 | 126.11779 | 21.048672 | 183.47368885 | 40.96543811 | 300.022 | 53839.0903240741 | 2006-04-14 02:10:04 | 53840.7752199074 | 2006-04-15 18:36:19 | 701053010 | 77.1974 | 75 | 77.2214 | 77.1974 | 77.2134 | 77.2214 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62.3339 | 62.3339 | 145.4999 | 9 | PROCESSED | 57533.486875 | 2016-05-25 11:41:06 | 54401 | 2007-10-28 00:00:00 | 53906.2114699074 | 2006-06-20 05:04:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011344 | Ultraluminous infrared galaxies (ULIRGs) produce the energy outputs of quasars with nearly all the power emerging in the far-IR via reprocessing of optical, UV, and X-ray radiation by dust. The ultimate nuclear power source, be it AGN or compact starburst, of ULIRGs has been the focus of much debate since their discovery with the IRAS mission. While observations with Spitzer are unlocking the secrets of many nearby ULIRGs, some have nuclei that are apparently so obscured as to be optically thick even in the mid-IR. We have chosen three local ULIRGs, IRAS 08572+3915, IRAS15250+3609, and IRAS20551-4250 that are IR-bright, yet highly obscured for deep Suzaku observations to search for the tell-tale signs of a buried AGN: hard X-ray emission behind significant column densities of HI gas. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SARAH GALLAGHER | USA | 1 | AO1 | ULTRAHARD X-RAY CASE STUDIES OF ULIRGS WITH DEEP SILICATE ABSORPTION | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701053010/ | Quick Look | ![]() |
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275 | MKN 841 | 225.9811 | 10.3761 | 225.377197 | 10.570593 | 220.178092 | 26.525473 | 11.09749436 | 54.61837916 | 292.433 | 54304.6970949074 | 2007-07-23 16:43:49 | 54306.218912037 | 2007-07-25 05:15:14 | 701084020 | 50.9253 | 50 | 50.9253 | 50.9333 | 0 | 50.9333 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6556 | 47.6556 | 131.4738 | 2 | PROCESSED | 57539.3432060185 | 2016-05-31 08:14:13 | 54800 | 2008-11-30 00:00:00 | 54339.5240277778 | 2007-08-27 12:34:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PIERRE-OLIVIER PETRUCCI | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701084020/ | Quick Look | ![]() |
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276 | A2104E | 235.1486 | -3.297 | 234.495076 | -3.136609 | 233.617797 | 15.850396 | 2.9252225 | 39.1285511 | 117.6908 | 54118.1261226852 | 2007-01-18 03:01:37 | 54118.6850231482 | 2007-01-18 16:26:26 | 801003010 | 22.7847 | 20 | 22.7847 | 22.7847 | 0 | 22.7847 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.7352 | 17.7352 | 48.2879 | 1 | PROCESSED | 57536.8549189815 | 2016-05-28 20:31:05 | 54735 | 2008-09-26 00:00:00 | 54132.8631365741 | 2007-02-01 20:42:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801003010/ | Quick Look | ![]() |
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277 | A399/401 FILAMENT | 44.7475 | 13.2485 | 44.061375 | 13.049612 | 46.15841 | -3.573964 | 164.45015039 | -39.12843885 | 74.1756 | 53966.1736921296 | 2006-08-19 04:10:07 | 53969.4641666667 | 2006-08-22 11:08:24 | 801020010 | 151.0601 | 150 | 151.0601 | 151.0681 | 151.0681 | 151.0681 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 142.2036 | 142.2036 | 284.2738 | 5 | PROCESSED | 57535.3984837963 | 2016-05-27 09:33:49 | 54526 | 2008-03-01 00:00:00 | 54021.1056944444 | 2006-10-13 02:32:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010063 | Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YUTAKA FUJITA | JAP | 1 | AO1 | THE DETECTION OF WHIM IN THE A399/401 FILAMENT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801020010/ | Quick Look | ![]() |
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278 | ABELL 2204 | 248.0963 | 5.6404 | 247.481247 | 5.74563 | 245.314616 | 27.222606 | 21.10023438 | 33.35451369 | 261.3606 | 53995.3098958333 | 2006-09-17 07:26:15 | 53996.5098958333 | 2006-09-18 12:14:15 | 801091010 | 49.1113 | 55 | 49.1113 | 49.1113 | 49.1113 | 49.1113 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 51.9372 | 51.9372 | 103.6439 | 1 | PROCESSED | 57535.6038194444 | 2016-05-27 14:29:30 | 54526 | 2008-03-01 00:00:00 | 54020.8840277778 | 2006-10-12 21:13:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012018 | Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | THOMAS REIPRICH | EUR | 1 | AO1 | A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801091010/ | Quick Look | ![]() |
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279 | THE CRAB OFFSETS | 83.6331 | 21.9589 | 82.881145 | 21.926215 | 84.096743 | -1.351596 | 184.60466298 | -5.81410844 | 87.5062 | 53996.8758680556 | 2006-09-18 21:01:15 | 53996.9515509259 | 2006-09-18 22:50:14 | 101011060 | 3.368 | 2 | 3.368 | 3.368 | 3.368 | 3.368 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.716 | 2.716 | 6.5279 | 0 | PROCESSED | 57535.6113888889 | 2016-05-27 14:40:24 | 53826 | 2006-04-01 00:00:00 | 54104.4231481482 | 2007-01-04 10:09:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | YOSHITOMO MAEDA | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/101011060/ | Quick Look | ![]() |
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280 | SGR1900+14 | 286.803 | 9.3875 | 286.206177 | 9.3084 | 289.573902 | 31.693472 | 43.07594962 | 0.80149907 | 86.5533 | 53826.3631597222 | 2006-04-01 08:42:57 | 53826.9113310185 | 2006-04-01 21:52:19 | 401022010 | 17.0562 | 20 | 17.7046 | 21.7074 | 21.6555 | 17.0562 | 1 | 2 | 1 | 1 | 1 | 0 | 0 | 14.3604 | 14.3604 | 47.336 | 1 | PROCESSED | 57533.34875 | 2016-05-25 08:22:12 | 54394 | 2007-10-21 00:00:00 | 53906.0977893518 | 2006-06-20 02:20:49 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010124 | We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. | GALACTIC POINT SOURCES | 4 | A | YUJIN NAKAGAWA | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401022010/ | Quick Look | ![]() |
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281 | CYGNUS X-2 | 326.1653 | 38.3323 | 325.647427 | 38.10178 | 346.69525 | 47.972917 | 87.3318132 | -11.3049847 | 76.3142 | 53871.8636805556 | 2006-05-16 20:43:42 | 53872.7293171296 | 2006-05-17 17:30:13 | 401049010 | 39.3903 | 37 | 39.3903 | 39.4063 | 39.3903 | 39.3903 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 36.8804 | 36.8804 | 74.786 | 1 | PROCESSED | 57534.3858217593 | 2016-05-26 09:15:35 | 54401 | 2007-10-28 00:00:00 | 53927.6429166667 | 2006-07-11 15:25:48 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | JON MILLER | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401049010/ | Quick Look | ![]() |
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282 | 1E 1841-045 | 280.3141 | -4.8735 | 279.649841 | -4.921767 | 280.812771 | 18.180712 | 27.4352849 | 0.03686802 | 77.3227 | 53844.4525462963 | 2006-04-19 10:51:40 | 53847.1328009259 | 2006-04-22 03:11:14 | 401100010 | 97.9622 | 100 | 97.9622 | 97.9702 | 97.9709 | 97.9709 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63.474 | 63.474 | 231.5399 | 2 | PROCESSED | 57533.5748032407 | 2016-05-25 13:47:43 | 54401 | 2007-10-28 00:00:00 | 53907.2806597222 | 2006-06-21 06:44:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014204 | Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data. | GALACTIC POINT SOURCES | 4 | A | ILANA HARRUS | MIKIO NORII | USJ | 1 | AO1 | SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401100010/ | Quick Look | ![]() |
283 | SDSSJ084234.9+362503 | 130.6534 | 36.3531 | 129.855939 | 36.532969 | 123.380084 | 17.503637 | 186.36195466 | 37.19411123 | 266.2333 | 53868.6856018518 | 2006-05-13 16:27:16 | 53871.41625 | 2006-05-16 09:59:24 | 701004010 | 109.9556 | 120 | 109.9716 | 109.9636 | 109.9556 | 109.9636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 127.2306 | 127.2306 | 235.8948 | 1 | PROCESSED | 57534.3648032407 | 2016-05-26 08:45:19 | 54400 | 2007-10-27 00:00:00 | 53920.287650463 | 2006-07-04 06:54:13 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010036 | Type 2 QSOs are one of the key class to understand the structure and evolution of AGN, origin of the Cosmic X-ray background, and the history of black hole growth. We propose to measure a hard X-ray spectrum of the most luminous and brightest type 2 QSO candidate in the Sloan Digital Sky Survey. The selection by optical narrow line spectra is not biased toward Compton-thin AGNs and enables us to investigate the true nature of type 2 QSOs. The data will be used to measure the absorption column density, intrinsic luminosity, and to constrain the structure of the absorber. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YUICHI TERASHIMA | JAP | 1 | AO1 | THE MOST LUMINOUS TYPE 2 QSO IN SDSS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701004010/ | Quick Look | ![]() |
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284 | RXJ1713-3946 | 258.942 | -39.4278 | 258.077115 | -39.372323 | 261.109643 | -16.326699 | 347.8535904 | -0.62405701 | 268.0013 | 53998.4433912037 | 2006-09-20 10:38:29 | 53998.8467476852 | 2006-09-20 20:19:19 | 501071010 | 21.1741 | 20 | 21.1741 | 21.1981 | 21.1901 | 21.1821 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18.3387 | 18.3387 | 34.8399 | 0 | PROCESSED | 57535.634537037 | 2016-05-27 15:13:44 | 54526 | 2008-03-01 00:00:00 | 54020.8878009259 | 2006-10-12 21:18:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TADAYUKI TAKAHASHI | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501071010/ | Quick Look | ![]() |
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285 | M81 | 148.8559 | 68.9951 | 147.832512 | 69.232018 | 119.540473 | 51.512284 | 142.17660014 | 40.93097712 | 281.1688 | 53863.0052083333 | 2006-05-08 00:07:30 | 53864.5209953704 | 2006-05-09 12:30:14 | 701022010 | 103.5186 | 100 | 103.5266 | 103.5266 | 103.5266 | 103.5186 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70.7369 | 70.7369 | 130.9421 | 0 | PROCESSED | 57534.2973726852 | 2016-05-26 07:08:13 | 54397 | 2007-10-24 00:00:00 | 53913.9816550926 | 2006-06-27 23:33:35 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010151 | We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKESHI ITOH | JAP | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701022010/ | Quick Look | ![]() |
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286 | SWIFT J0350.1-5019 | 57.5315 | -50.3337 | 57.174394 | -50.483946 | 28.735241 | -67.001155 | 259.74491819 | -49.02538792 | 320.5309 | 53838.5046875 | 2006-04-13 12:06:45 | 53838.6752199074 | 2006-04-13 16:12:19 | 701017010 | 2.6998 | 20 | 2.7158 | 2.7158 | 2.6998 | 2.7078 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1.1771 | 1.1771 | 9.165 | 0 | PROCESSED | 57533.4464930556 | 2016-05-25 10:42:57 | 54750 | 2008-10-11 00:00:00 | 53905.4679398148 | 2006-06-19 11:13:50 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOSHIHIRO UEDA | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701017010/ | Quick Look | ![]() |
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287 | GALACTIC CENTER GC2 | 265.779 | -29.1853 | 264.9833 | -29.162875 | 266.287161 | -5.798531 | 359.50136289 | 0.33591697 | 108.7998 | 54170.1638773148 | 2007-03-11 03:55:59 | 54170.7946064815 | 2007-03-11 19:04:14 | 501047010 | 25.599 | 25 | 25.607 | 25.599 | 0 | 25.623 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.0886 | 19.0886 | 54.4799 | 0 | PROCESSED | 57537.6398611111 | 2016-05-29 15:21:24 | 54736 | 2008-09-27 00:00:00 | 54182.2693865741 | 2007-03-23 06:27:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | MOTOHIDE KOKUBUN | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501047010/ | Quick Look | ![]() |
288 | LMC X-3 OFF FIELD 1 | 85.5246 | -64.555 | 85.467763 | -64.576889 | 45.273362 | -87.277293 | 274.10794908 | -31.71433471 | 145.4977 | 54039.3159722222 | 2006-10-31 07:35:00 | 54039.7509722222 | 2006-10-31 18:01:24 | 501097020 | 15.3749 | 10 | 15.3749 | 15.3829 | 15.3829 | 15.3829 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.9263 | 14.9263 | 37.58 | 0 | PROCESSED | 57536.0002314815 | 2016-05-28 00:00:20 | 54526 | 2008-03-01 00:00:00 | 54088.8072222222 | 2006-12-19 19:22:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | Q. DANIEL WANG | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501097020/ | Quick Look | ![]() |
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289 | Z348 | 16.7077 | 1.0407 | 16.065796 | 0.773597 | 15.79467 | -5.606239 | 131.03941429 | -61.58850223 | 247.9196 | 54110.9286689815 | 2007-01-10 22:17:17 | 54111.5259722222 | 2007-01-11 12:37:24 | 801050010 | 22.6477 | 23 | 22.6477 | 22.6477 | 0 | 22.6477 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.3403 | 21.3403 | 51.589 | 1 | PROCESSED | 57536.8362384259 | 2016-05-28 20:04:11 | 54735 | 2008-09-26 00:00:00 | 54133.0321643518 | 2007-02-02 00:46:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010098 | We propose to carry out the Suzaku/XIS observations of 4 massive clusters at low redshifts (z <0.3). Combining the X-ray data with the existing Subaru datasets that allow us to directly reconstruct the mass distribution from the gravitational lensing measurements, we will investigate the physical relations between the mass and gas distributions to understand the nature of cluster in a quantitative way. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOSHIFUMI FUTAMASE | JAP | 1 | AO1 | THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801050010/ | Quick Look | ![]() |
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290 | A2104S | 235.0317 | -3.4139 | 234.377731 | -3.253044 | 233.528717 | 15.709214 | 2.71321412 | 39.14413145 | 117.9978 | 54120.3324884259 | 2007-01-20 07:58:47 | 54120.8266087963 | 2007-01-20 19:50:19 | 801004010 | 17.3234 | 20 | 17.3234 | 17.3234 | 0 | 17.3234 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.8291 | 13.8291 | 42.6819 | 1 | PROCESSED | 57536.8854166667 | 2016-05-28 21:15:00 | 54750 | 2008-10-11 00:00:00 | 54137.3891898148 | 2007-02-06 09:20:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801004010/ | Quick Look | ![]() |
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291 | IIZW108 | 318.5228 | 2.5728 | 317.890055 | 2.365228 | 321.781705 | 17.722745 | 53.56011975 | -29.86052353 | 77.7227 | 53864.5319791667 | 2006-05-09 12:46:03 | 53864.7883680556 | 2006-05-09 18:55:15 | 801075010 | 11.6052 | 11 | 11.6052 | 11.6052 | 11.6052 | 11.6052 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.632 | 9.632 | 22.1499 | 1 | PROCESSED | 57534.2579398148 | 2016-05-26 06:11:26 | 54401 | 2007-10-28 00:00:00 | 53913.9958564815 | 2006-06-27 23:54:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801075010/ | Quick Look | ![]() |
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292 | 4U1700-37 | 255.9894 | -37.8441 | 255.139416 | -37.774677 | 258.577099 | -14.956185 | 347.75582102 | 2.17172645 | 269.6945 | 53991.447662037 | 2006-09-13 10:44:38 | 53992.918912037 | 2006-09-14 22:03:14 | 401058010 | 81.4425 | 80 | 81.4569 | 81.4704 | 81.4425 | 81.4544 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 82.1093 | 82.1093 | 127.109 | 1 | PROCESSED | 57535.6097916667 | 2016-05-27 14:38:06 | 54526 | 2008-03-01 00:00:00 | 54053.5428240741 | 2006-11-14 13:01:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011135 | The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse. | GALACTIC POINT SOURCES | 4 | A | TIMOTHY KALLMAN | USA | 1 | AO1 | IRON LINE VARIABILITY IN 4U1700-37 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401058010/ | Quick Look | ![]() |
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293 | ALGOL | 47.0831 | 40.8965 | 46.267674 | 40.705521 | 56.181748 | 22.363141 | 149.0355551 | -14.93487401 | 244.4771 | 54167.6197222222 | 2007-03-08 14:52:24 | 54169.6132986111 | 2007-03-10 14:43:09 | 401093010 | 102.1642 | 105 | 102.1642 | 102.1642 | 0 | 102.1642 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.4729 | 102.4729 | 172.1928 | 1 | PROCESSED | 57537.6825810185 | 2016-05-29 16:22:55 | 54736 | 2008-09-27 00:00:00 | 54186.3983564815 | 2007-03-27 09:33:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012024 | Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD. | GALACTIC POINT SOURCES | 4 | C | MANUEL GUEDEL | EUR | 1 | AO1 | A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401093010/ | Quick Look | ![]() |
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294 | SERPENS X-1 | 279.9934 | 5.0285 | 279.376671 | 4.981655 | 281.288405 | 28.078275 | 36.11311789 | 4.83561165 | 256.1423 | 54032.2853819444 | 2006-10-24 06:50:57 | 54033.2259143518 | 2006-10-25 05:25:19 | 401048010 | 37.1578 | 37 | 37.1578 | 37.2698 | 37.2058 | 37.1658 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31.0695 | 31.0695 | 81.2399 | 2 | PROCESSED | 57535.9734722222 | 2016-05-27 23:21:48 | 54526 | 2008-03-01 00:00:00 | 54056.4719328704 | 2006-11-17 11:19:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | JON MILLER | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401048010/ | Quick Look | ![]() |
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295 | 4U 1636-536 | 250.2273 | -53.7542 | 249.230886 | -53.657708 | 256.461437 | -31.236858 | 332.91122007 | -4.81806999 | 91.2447 | 54153.2955787037 | 2007-02-22 07:05:38 | 54154.3544560185 | 2007-02-23 08:30:25 | 401050020 | 40.096 | 38 | 40.096 | 40.104 | 0 | 40.096 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 35.55 | 35.55 | 91.4779 | 0 | PROCESSED | 57537.4821990741 | 2016-05-29 11:34:22 | 54525 | 2008-02-29 00:00:00 | 54158.392037037 | 2007-02-27 09:24:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050020/ | Quick Look | ![]() |
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296 | IGRJ16493-4348 | 252.3173 | -43.8652 | 251.422595 | -43.77854 | 256.400238 | -21.254215 | 341.31911758 | 0.57823277 | 287.444 | 54013.8822916667 | 2006-10-05 21:10:30 | 54014.4204166667 | 2006-10-06 10:05:24 | 401054010 | 21.1998 | 20 | 21.2158 | 21.2158 | 21.1998 | 21.2078 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20.2197 | 20.2197 | 46.4639 | 1 | PROCESSED | 57535.7818634259 | 2016-05-27 18:45:53 | 54695 | 2008-08-17 00:00:00 | 54025.4796412037 | 2006-10-17 11:30:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | RANDALL SMITH | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401054010/ | Quick Look | ![]() |
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297 | SGR 1806-20 | 272.166 | -20.4729 | 271.421316 | -20.481616 | 272.022208 | 2.952663 | 9.94279657 | -0.27364584 | 269.9473 | 53987.9261921296 | 2006-09-09 22:13:43 | 53989.1668287037 | 2006-09-11 04:00:14 | 401092010 | 48.9155 | 50 | 48.9155 | 48.9235 | 48.9315 | 48.9315 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 55.4085 | 55.4085 | 107.1759 | 1 | PROCESSED | 57535.5272453704 | 2016-05-27 12:39:14 | 54526 | 2008-03-01 00:00:00 | 54021.1112615741 | 2006-10-13 02:40:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012017 | The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters. | GALACTIC POINT SOURCES | 4 | B | SANDRO MEREGHETTI | EUR | 1 | AO1 | COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401092010/ | Quick Look | ![]() |
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298 | RX J1347.5-1145 | 206.856 | -11.8093 | 206.189594 | -11.560184 | 209.147124 | -0.679556 | 323.97916756 | 48.76108187 | 292.056 | 53916.7756597222 | 2006-06-30 18:36:57 | 53918.7600115741 | 2006-07-02 18:14:25 | 801013010 | 69.6611 | 75 | 69.6611 | 69.6611 | 69.6611 | 69.6611 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.982 | 60.982 | 171.3759 | 0 | PROCESSED | 57534.8555671296 | 2016-05-26 20:32:01 | 54394 | 2007-10-21 00:00:00 | 53926.4810300926 | 2006-07-10 11:32:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010014 | We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013010/ | Quick Look | ![]() |
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299 | OPHIUCHUS CLUSTER 5 | 258.0184 | -23.1077 | 257.261763 | -23.048099 | 258.982957 | -0.123527 | 0.73892155 | 9.49336651 | 88.7652 | 54181.8276736111 | 2007-03-22 19:51:51 | 54182.4890277778 | 2007-03-23 11:44:12 | 801026010 | 24.2557 | 15 | 24.2557 | 24.2557 | 0 | 24.2557 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2271 | 19.2271 | 57.1359 | 0 | PROCESSED | 57537.9767013889 | 2016-05-29 23:26:27 | 54736 | 2008-09-27 00:00:00 | 54186.2070949074 | 2007-03-27 04:58:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801026010/ | Quick Look | ![]() |
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300 | M87 CENTER | 187.7366 | 12.4456 | 187.103964 | 12.721646 | 182.061198 | 14.477269 | 283.82387862 | 74.55209055 | 120.529 | 54068.9187037037 | 2006-11-29 22:02:56 | 54071.1266666667 | 2006-12-02 03:02:24 | 801038010 | 98.1831 | 100 | 98.1831 | 98.1831 | 0 | 98.1831 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 88.2503 | 88.2503 | 190.7308 | 2 | PROCESSED | 57536.2829050926 | 2016-05-28 06:47:23 | 54735 | 2008-09-26 00:00:00 | 54090.4156134259 | 2006-12-21 09:58:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010084 | The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIRONORI MATSUMOTO | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801038010/ | Quick Look | ![]() |
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301 | PERSEUS CL OFFSET | 49.6445 | 42.068 | 48.814215 | 41.886236 | 58.537476 | 22.936041 | 150.06631202 | -12.92163855 | 65.996 | 53980.0800925926 | 2006-09-02 01:55:20 | 53980.7668287037 | 2006-09-02 18:24:14 | 801049010 | 29.2438 | 30 | 29.2559 | 29.2479 | 29.2518 | 29.2438 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.6729 | 25.6729 | 59.3299 | 1 | PROCESSED | 57535.4121296296 | 2016-05-27 09:53:28 | 54526 | 2008-03-01 00:00:00 | 54021.3135416667 | 2006-10-13 07:31:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049010/ | Quick Look | ![]() |
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302 | PERSEUS CL OFFSET | 50.2242 | 41.1004 | 49.398659 | 40.920786 | 58.698225 | 21.886134 | 150.98569591 | -13.49005998 | 65.9967 | 53981.4552662037 | 2006-09-03 10:55:35 | 53982.1418287037 | 2006-09-04 03:24:14 | 801049030 | 32.8396 | 30 | 32.8556 | 32.8476 | 32.8396 | 32.8636 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 31.0313 | 31.0313 | 59.288 | 0 | PROCESSED | 57535.4291087963 | 2016-05-27 10:17:55 | 54526 | 2008-03-01 00:00:00 | 54020.8372106482 | 2006-10-12 20:05:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049030/ | Quick Look | ![]() |
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303 | ABELL 2199 OFFSET 2 | 247.3619 | 39.6495 | 246.934152 | 39.757579 | 233.32636 | 60.237575 | 63.07626508 | 43.54039287 | 251.2564 | 54011.5284722222 | 2006-10-03 12:41:00 | 54012.1578587963 | 2006-10-04 03:47:19 | 801058010 | 22.7072 | 25 | 22.7232 | 22.7072 | 22.7232 | 22.7232 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.704 | 20.704 | 54.36 | 0 | PROCESSED | 57535.7442476852 | 2016-05-27 17:51:43 | 54735 | 2008-09-26 00:00:00 | 54024.6719907407 | 2006-10-16 16:07:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801058010/ | Quick Look | ![]() |
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304 | M101 | 210.8841 | 54.3679 | 210.442342 | 54.607302 | 174.405989 | 59.838606 | 101.97854462 | 59.72940376 | 150.2959 | 54062.5790625 | 2006-11-23 13:53:51 | 54064.7182175926 | 2006-11-25 17:14:14 | 801063010 | 98.8522 | 100 | 98.8762 | 98.8522 | 0 | 98.8762 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.6125 | 89.6125 | 184.802 | 2 | PROCESSED | 57536.2145486111 | 2016-05-28 05:08:57 | 54455 | 2007-12-21 00:00:00 | 54088.707650463 | 2006-12-19 16:59:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011402 | We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | K. KUNTZ | USA | 1 | AO1 | SOFT DIFFUSE X-RAY EMISSION FROM M101 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801063010/ | Quick Look | ![]() |
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305 | SN 1987A | 83.9013 | -69.2655 | 83.9928 | -69.294887 | 307.391677 | -86.458548 | 279.69660922 | -31.92548266 | 330.0004 | 53894.6930555556 | 2006-06-08 16:38:00 | 53895.6683449074 | 2006-06-09 16:02:25 | 801090010 | 39.6464 | 40 | 39.6464 | 39.6464 | 39.6464 | 39.6464 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.2519 | 39.2519 | 84.2399 | 0 | PROCESSED | 57534.6267592593 | 2016-05-26 15:02:32 | 54400 | 2007-10-27 00:00:00 | 53928.1346527778 | 2006-07-12 03:13:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012006 | In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | G NTHER HASINGER | EUR | 1 | AO1 | SN 1987A - A RUSTY REMNANT? | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801090010/ | Quick Look | ![]() |
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306 | CXOU J164710.2-455216 | 251.7964 | -45.87 | 250.884129 | -45.780896 | 256.291708 | -23.290157 | 339.54853507 | -0.43200811 | 286.2915 | 54001.2911689815 | 2006-09-23 06:59:17 | 54002.205775463 | 2006-09-24 04:56:19 | 901002010 | 38.6794 | 40 | 38.6874 | 38.6954 | 38.6961 | 38.6794 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 35.0799 | 35.0799 | 79.0159 | 1 | PROCESSED | 57535.6726851852 | 2016-05-27 16:08:40 | 54002 | 2006-09-24 00:00:00 | 54026.4631134259 | 2006-10-18 11:06:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017002 | N/A | GALACTIC COMPACT OBJECT | 9 | A | SWG | JAP | 1 | TOO | TOO OBSERVATION OF CXOU J164710.2-455216 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/901002010/ | Quick Look | ![]() |
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307 | NGC 5506 | 213.3095 | -3.2029 | 212.660624 | -2.969373 | 212.1852 | 9.604154 | 339.1508826 | 53.81542712 | 91.2728 | 54131.0918055556 | 2007-01-31 02:12:12 | 54132.6279513889 | 2007-02-01 15:04:15 | 701030030 | 57.4063 | 150 | 57.4143 | 57.4063 | 0 | 57.4143 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.7027 | 47.7027 | 132.6858 | 0 | PROCESSED | 57536.9491666667 | 2016-05-28 22:46:48 | 54695 | 2008-08-17 00:00:00 | 54139.3642361111 | 2007-02-08 08:44:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TRACEY TURNER | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701030030/ | Quick Look | ![]() |
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308 | CIRCINUS GALAXY | 213.2971 | -65.3336 | 212.329588 | -65.099539 | 238.600438 | -47.951762 | 311.32997737 | -3.80345965 | 276.4798 | 53937.5207986111 | 2006-07-21 12:29:57 | 53939.0475 | 2006-07-23 01:08:24 | 701036010 | 108.0217 | 100 | 108.0457 | 108.0217 | 108.0457 | 108.0297 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94.272 | 94.272 | 131.8879 | 1 | PROCESSED | 57535.0550578704 | 2016-05-27 01:19:17 | 54401 | 2007-10-28 00:00:00 | 53943.5986574074 | 2006-07-27 14:22:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011331 | The light of AGN dominates the hard cosmic X-ray background. However, the contribution of Compton thick objects is poorly constrained because they emit chiefly above the energy range where Chandra and XMM are sensitive. Here we propose to observe the Circinus galaxy, one of the two brightest AGN reflection sources below 10 keV and with a known high column density. Our observations below 10 keV will provide CCD spectra of the rich emission line and continuum spectra, allowing limited photoionization modelling and searches for variability, possibly seen in Circinus. In the range 10 - 60 keV, we shall obtain a spectrum of the directly viewed continuum with unprecedented S/N in the key band for the HCXB. Above 60 keV, we will detect Circinus and check whether the spectrum has a rollover. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ANDREW WILSON | USA | 1 | AO1 | THE HARD X-RAY BACKGROUND, COMPTON-THICK AGN AND WATER VAPOR MEGAMASERS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701036010/ | Quick Look | ![]() |
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309 | APM 08279+5255 | 127.9195 | 52.7471 | 126.987464 | 52.916366 | 116.240703 | 32.704357 | 165.76446097 | 36.2381521 | 299.485 | 54183.9301041667 | 2007-03-24 22:19:21 | 54186.4654513889 | 2007-03-27 11:10:15 | 701057030 | 117.1433 | 125 | 117.1433 | 117.1513 | 0 | 117.1433 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.9324 | 110.9324 | 219.0418 | 3 | PROCESSED | 57538.0464467593 | 2016-05-30 01:06:53 | 54702 | 2008-08-24 00:00:00 | 54209.5933680556 | 2007-04-19 14:14:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE CHARTAS | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701057030/ | Quick Look | ![]() |
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310 | 1ES 1553+113 | 238.8999 | 11.1305 | 238.306227 | 11.275519 | 233.852477 | 30.750337 | 21.81691499 | 43.96274027 | 296.7536 | 53940.6127777778 | 2006-07-24 14:42:24 | 53941.8036342593 | 2006-07-25 19:17:14 | 701070010 | 55.6355 | 55 | 55.6435 | 55.6515 | 55.6515 | 55.6355 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53.2015 | 53.2015 | 102.8819 | 0 | PROCESSED | 57535.0418171296 | 2016-05-27 01:00:13 | 54401 | 2007-10-28 00:00:00 | 53955.6133680556 | 2006-08-08 14:43:15 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ANITA REIMER | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701070010/ | Quick Look | ![]() |
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311 | 1ES 1959+650 | 299.9645 | 65.1588 | 299.84329 | 65.020024 | 7.34886 | 77.791428 | 98.00607393 | 17.68746705 | 45.1602 | 53878.0509606482 | 2006-05-23 01:13:23 | 53880.1718055556 | 2006-05-25 04:07:24 | 701075010 | 98.8622 | 100 | 98.8782 | 98.8622 | 98.8702 | 98.8782 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96.106 | 96.106 | 183.2028 | 2 | PROCESSED | 57534.4674305556 | 2016-05-26 11:13:06 | 54408 | 2007-11-04 00:00:00 | 53928.2478472222 | 2006-07-12 05:56:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012002 | We request to observe 1ES1959+650 and 1ES2344+514 for 100 ks each with SUZAKU simultaneously with the Whipple Cherenkov telescope. Whipple will extensively monitor these sources for months in 2006-2007. There are three well defined scientific cases that we would like to address. We want to study 1) the correlation between the soft and hard X-ray and TeV fluxes and spectra, extremely variable in these sources, sometimes showing extreme conditions; 2) the mystery of the ''orphan'' flares; i.e. events observed only in the TeV gamma rays without a counterpart in the X-rays: this is currently not understood in the framework of SSC models; 3) the origin of the lag observed between soft and hard X-ray variability in some blazars and the implications for the TeV emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GIANPIERO TAGLIAFERRI | EUR | 1 | AO1 | JETS ON TEST: SIMULTANEOUS X-RAY AND TEV OBSERVATIONS OF 1ES1959+650 AND 1ES2344+514 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701075010/ | Quick Look | ![]() |
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312 | ABELL 2199 OFFSET 1 | 247.0269 | 39.6504 | 246.598636 | 39.759978 | 232.832467 | 60.158374 | 63.06766091 | 43.79825488 | 251.7923 | 54009.8973958333 | 2006-10-01 21:32:15 | 54010.4467476852 | 2006-10-02 10:43:19 | 801057010 | 24.6315 | 25 | 24.6315 | 24.6315 | 24.6315 | 24.6315 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.5343 | 25.5343 | 47.454 | 0 | PROCESSED | 57535.7339814815 | 2016-05-27 17:36:56 | 54735 | 2008-09-26 00:00:00 | 54021.2449189815 | 2006-10-13 05:52:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801057010/ | Quick Look | ![]() |
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313 | ABELL 2199 OFFSET 3 | 247.3596 | 39.3165 | 246.92934 | 39.424595 | 233.528009 | 59.920137 | 62.61707687 | 43.53145251 | 252.4737 | 54012.1589351852 | 2006-10-04 03:48:52 | 54012.6786921296 | 2006-10-04 16:17:19 | 801059010 | 25.2467 | 25 | 25.2467 | 25.2467 | 25.2467 | 25.2467 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.505 | 20.505 | 44.8879 | 1 | PROCESSED | 57535.7507291667 | 2016-05-27 18:01:03 | 54735 | 2008-09-26 00:00:00 | 54025.4730092593 | 2006-10-17 11:21:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801059010/ | Quick Look | ![]() |
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314 | AB DOR | 82.2881 | -65.4658 | 82.252574 | -65.503277 | 15.679222 | -86.688003 | 275.31538375 | -33.00189818 | 204.2849 | 54108.0647569444 | 2007-01-08 01:33:15 | 54109.4724421296 | 2007-01-09 11:20:19 | 401031020 | 49.0965 | 45 | 49.0965 | 49.0965 | 0 | 49.0965 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.9611 | 44.9611 | 121.6199 | 2 | PROCESSED | 57536.5000578704 | 2016-05-28 12:00:05 | 54502 | 2008-02-06 00:00:00 | 54133.0127083333 | 2007-02-02 00:18:18 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | MARC AUDARD | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401031020/ | Quick Look | ![]() |
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315 | 1RXS J213344.1+51072 | 323.4354 | 51.1973 | 323.001109 | 50.974362 | 356.300054 | 59.716219 | 94.50909334 | -0.42447705 | 94.0452 | 53854.2853009259 | 2006-04-29 06:50:50 | 53856.2501736111 | 2006-05-01 06:00:15 | 401038010 | 81.9241 | 80 | 81.9241 | 81.9241 | 81.9241 | 81.9241 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62.8881 | 62.8881 | 169.7261 | 3 | PROCESSED | 57533.6330671296 | 2016-05-25 15:11:37 | 54391 | 2007-10-18 00:00:00 | 53908.1887962963 | 2006-06-22 04:31:52 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | KOJI MUKAI | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401038010/ | Quick Look | ![]() |
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316 | V893 SCO | 243.8144 | -28.6275 | 243.038085 | -28.502934 | 247.008203 | -7.251726 | 348.06577336 | 15.88028883 | 274.6746 | 53973.4024189815 | 2006-08-26 09:39:29 | 53974.056412037 | 2006-08-27 01:21:14 | 401041010 | 18.4978 | 20 | 18.4978 | 18.4978 | 18.4978 | 18.4978 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16.1403 | 16.1403 | 56.482 | 0 | PROCESSED | 57535.3695601852 | 2016-05-27 08:52:10 | 54526 | 2008-03-01 00:00:00 | 54053.4763888889 | 2006-11-14 11:26:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011103 | The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies. | GALACTIC POINT SOURCES | 4 | B | KOJI MUKAI | USA | 1 | AO1 | CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401041010/ | Quick Look | ![]() |
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317 | 4U 1636-536 | 250.2277 | -53.7538 | 249.23129 | -53.65731 | 256.461636 | -31.236425 | 332.91167841 | -4.81798429 | 93.2445 | 54186.4802777778 | 2007-03-27 11:31:36 | 54187.3043287037 | 2007-03-28 07:18:14 | 401050040 | 32.1304 | 38 | 32.1304 | 32.1384 | 0 | 32.1304 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 27.7842 | 27.7842 | 71.1779 | 1 | PROCESSED | 57538.0141782407 | 2016-05-30 00:20:25 | 54695 | 2008-08-17 00:00:00 | 54209.541412037 | 2007-04-19 12:59:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | JEROEN HOMAN | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401050040/ | Quick Look | ![]() |
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318 | 4U 1822-37 | 276.4461 | -37.1042 | 275.595774 | -37.133404 | 275.279951 | -13.781506 | 356.85149319 | -11.29112534 | 258.4537 | 54010.4563888889 | 2006-10-02 10:57:12 | 54011.5189699074 | 2006-10-03 12:27:19 | 401051010 | 37.7434 | 40 | 37.7682 | 37.7682 | 37.7434 | 37.7434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33.1785 | 33.1785 | 91.8059 | 0 | PROCESSED | 57535.7615393518 | 2016-05-27 18:16:37 | 54695 | 2008-08-17 00:00:00 | 54024.6539814815 | 2006-10-16 15:41:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011121 | We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe. | GALACTIC POINT SOURCES | 4 | B | JEAN COTTAM | USA | 1 | AO1 | ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401051010/ | Quick Look | ![]() |
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319 | HESSJ1813-178 | 273.3946 | -17.7704 | 272.66469 | -17.785118 | 273.238499 | 5.632147 | 12.87014503 | 0.01155473 | 90.9367 | 54160.8999768518 | 2007-03-01 21:35:58 | 54162.2814699074 | 2007-03-03 06:45:19 | 401101010 | 63.8391 | 65 | 63.8471 | 63.8391 | 0 | 63.8471 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.7561 | 57.7561 | 119.3519 | 1 | PROCESSED | 57537.5358449074 | 2016-05-29 12:51:37 | 54736 | 2008-09-27 00:00:00 | 54167.6346990741 | 2007-03-08 15:13:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014214 | Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies. | GALACTIC POINT SOURCES | 4 | B | OLAF REIMER | KEN EBISAWA | USJ | 1 | AO1 | IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401101010/ | Quick Look | ![]() |
320 | CYGNUS_LOOP_P3 | 313.0409 | 31.565 | 312.525205 | 31.375918 | 328.010479 | 46.721185 | 74.84662265 | -8.19493741 | 240.0003 | 54418.4174074074 | 2007-11-14 10:01:04 | 54418.9377083333 | 2007-11-14 22:30:18 | 501014010 | 16.7648 | 12 | 16.7812 | 16.7808 | 0 | 16.7648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6962 | 14.6962 | 44.9439 | 0 | PROCESSED | 57540.5210069445 | 2016-06-01 12:30:15 | 54798 | 2008-11-28 00:00:00 | 54430.2624884259 | 2007-11-26 06:17:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501014010/ | Quick Look | ![]() |
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321 | DRACO HVC REGION A | 243.9602 | 60.0594 | 243.754378 | 60.182015 | 196.928393 | 76.754112 | 91.20688798 | 42.38144862 | 79.8192 | 53814.6161111111 | 2006-03-20 14:47:12 | 53816.0050578704 | 2006-03-22 00:07:17 | 501004010 | 61.1798 | 60 | 61.1798 | 61.1798 | 61.1798 | 61.1798 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61.2301 | 61.2301 | 119.9879 | 2 | PROCESSED | 57533.2956481482 | 2016-05-25 07:05:44 | 54394 | 2007-10-21 00:00:00 | 53906.0459722222 | 2006-06-20 01:06:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010069 | High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501004010/ | Quick Look | ![]() |
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322 | CAR-D1 | 162.0244 | -59.5887 | 161.531362 | -59.324189 | 202.52434 | -58.576902 | 287.89332648 | -0.36746291 | 282.973 | 53891.5567361111 | 2006-06-05 13:21:42 | 53892.6343055556 | 2006-06-06 15:13:24 | 501099010 | 76.9074 | 75 | 76.924 | 76.932 | 76.9314 | 76.9074 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64.2576 | 64.2576 | 93.0899 | 0 | PROCESSED | 57534.5127430556 | 2016-05-26 12:18:21 | 54401 | 2007-10-28 00:00:00 | 53926.947974537 | 2006-07-10 22:45:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011257 | Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip. | GALACTIC DIFFUSE EMISSION | 5 | B | KENJI HAMAGUCHI | USA | 1 | AO1 | ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501099010/ | Quick Look | ![]() |
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323 | GALACTIC PLANE 111 | 347.9369 | 61.9538 | 347.407091 | 61.681886 | 29.574403 | 58.088255 | 111.50111702 | 1.31488521 | 81.8498 | 53892.6499652778 | 2006-06-06 15:35:57 | 53893.680775463 | 2006-06-07 16:20:19 | 501100010 | 72.1409 | 75 | 72.1649 | 72.1649 | 72.1649 | 72.1409 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61.025 | 61.025 | 89.0349 | 1 | PROCESSED | 57534.5221064815 | 2016-05-26 12:31:50 | 54401 | 2007-10-28 00:00:00 | 53927.3325115741 | 2006-07-11 07:58:49 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011258 | We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component. | GALACTIC DIFFUSE EMISSION | 5 | B | K. KUNTZ | USA | 1 | AO1 | BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501100010/ | Quick Look | ![]() |
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324 | DRACO ENHANCEMENT | 239.3128 | 61.2868 | 239.109888 | 61.42925 | 187.011559 | 75.692319 | 93.98685674 | 43.98646489 | 194.9053 | 54048.1213888889 | 2006-11-09 02:54:48 | 54049.8515509259 | 2006-11-10 20:26:14 | 501101010 | 43.8628 | 75 | 79.4274 | 79.4274 | 43.8628 | 79.4194 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.8741 | 75.8741 | 149.474 | 1 | PROCESSED | 57536.1016319444 | 2016-05-28 02:26:21 | 54455 | 2007-12-21 00:00:00 | 54088.7470486111 | 2006-12-19 17:55:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011259 | We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature. | GALACTIC DIFFUSE EMISSION | 5 | C | K. KUNTZ | USA | 1 | AO1 | THE SOFT COMPONENT OF THE GALACTIC HALO | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501101010/ | Quick Look | ![]() |
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325 | MONOGEM RING WEST | 118.3557 | 8.2507 | 117.679197 | 8.381467 | 118.769502 | -12.402687 | 212.50229712 | 17.5030797 | 287.8334 | 53865.545462963 | 2006-05-10 13:05:28 | 53867.1127199074 | 2006-05-12 02:42:19 | 501084010 | 54.2685 | 50 | 54.2685 | 54.2685 | 54.2685 | 54.2685 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.2312 | 43.2312 | 135.3899 | 2 | PROCESSED | 57534.3136689815 | 2016-05-26 07:31:41 | 54401 | 2007-10-28 00:00:00 | 53914.2479282407 | 2006-06-28 05:57:01 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011243 | We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium. | GALACTIC DIFFUSE EMISSION | 5 | B | PAUL PLUCINSKY | USA | 1 | AO1 | THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501084010/ | Quick Look | ![]() |
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326 | 3C 390.3 | 280.629 | 79.7686 | 281.497615 | 79.715169 | 81.957835 | 76.491681 | 111.4356997 | 27.05756334 | 197.286 | 54083.1426851852 | 2006-12-14 03:25:28 | 54085.1384722222 | 2006-12-16 03:19:24 | 701060010 | 0.024 | 100 | 99.3678 | 99.3678 | 0.024 | 99.3678 | 2 | 2 | 1 | 2 | 1 | 0 | 0 | 97.8813 | 97.8813 | 172.4199 | 3 | PROCESSED | 57536.3784722222 | 2016-05-28 09:05:00 | 54702 | 2008-08-24 00:00:00 | 54132.9968055556 | 2007-02-01 23:55:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011363 | We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxies 3C382 and 3C390.3 to study their complex broad-band X-ray spectra. The HXD will constrain the continuum above 10 keV, discriminating between competing physically-different models, while at the same time the XIS will determine the parameters of the FeKalpha line and the shape of the soft X-rays. The proposed observations will allow us to shed light on the origin of reflection features in radio-loud AGN, ultimately determining the structure and ionization state of the accretion flow in these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RITA SAMBRUNA | USA | 1 | AO1 | THE BROAD-BAND X-RAY SPECTRUM OF BROAD-LINE RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701060010/ | Quick Look | ![]() |
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327 | CYGNUS_LOOP_P15 | 312.9857 | 30.6621 | 312.465734 | 30.473222 | 327.433989 | 45.909388 | 74.106397 | -8.72540127 | 61.9987 | 53880.177974537 | 2006-05-25 04:16:17 | 53880.6716898148 | 2006-05-25 16:07:14 | 501032010 | 20.7289 | 21 | 20.7289 | 20.7289 | 20.7289 | 20.7289 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.476 | 17.476 | 42.6349 | 0 | PROCESSED | 57534.4101041667 | 2016-05-26 09:50:33 | 54394 | 2007-10-21 00:00:00 | 53926.2440046296 | 2006-07-10 05:51:22 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501032010/ | Quick Look | ![]() |
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328 | NGC 7213 | 332.316 | -47.1629 | 331.53332 | -47.408605 | 315.985734 | -33.170959 | 349.59497628 | -52.58020545 | 231.3714 | 54030.2323611111 | 2006-10-22 05:34:36 | 54032.2759722222 | 2006-10-24 06:37:24 | 701029010 | 90.736 | 100 | 90.76 | 90.744 | 90.736 | 90.752 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90.3418 | 90.3418 | 176.5358 | 0 | PROCESSED | 57535.9564814815 | 2016-05-27 22:57:20 | 54695 | 2008-08-17 00:00:00 | 54056.3665162037 | 2006-11-17 08:47:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011305 | We propose a 100ks Suzaku observation of the low luminosity AGN, NGC 7213. Previous observations show a complex iron line and weak or no Compton reflection. However the iron line and reflection hump are poorly constrained, so the line emitting matter could arise from a truncated disk, BLR or a Compton-thin torus. A high quality Suzaku observation will constrain the iron line profile, resolve the ionized emission and unambiguously determine its origin. Using the unique broad bandpass of Suzaku above 10 keV we will place tight constraints on any reflection hump, enabling us to determine if the iron line originates from a truncated disk. This could provide a direct test of the paradigm that the X-ray emission in low accretion rate AGN occurs in a truncated disk system such as an ADAF. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | JAMES REEVES | USA | 1 | AO1 | DOES THE LOW LUMINOSITY AGN NGC7213 CONTAIN A TRUNCATED ACCRETION DISK? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701029010/ | Quick Look | ![]() |
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329 | IRAS 19254-7245 | 292.8508 | -72.6492 | 291.381636 | -72.754038 | 280.373528 | -50.031737 | 322.5078751 | -28.76929596 | 279.8892 | 54041.9830208333 | 2006-11-02 23:35:33 | 54044.5967476852 | 2006-11-05 14:19:19 | 701052010 | 113.5123 | 120 | 113.5203 | 113.5203 | 113.5123 | 113.5203 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 151.9778 | 151.9778 | 225.8099 | 1 | PROCESSED | 57536.068125 | 2016-05-28 01:38:06 | 54455 | 2007-12-21 00:00:00 | 54088.8285185185 | 2006-12-19 19:53:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011342 | We propose a 120 ksec Suzaku exposure of the ULIRG IRAS19254-7245. A previous XMM-Newton observation revealed the presence of a strong iron emission line and a flat continuum, both suggesting that this source hosts a Compton-thick AGN. In this scenario, the 2-10 keV luminosity of IRAS19254-7245 could be greater than 10e44 erg/s. However since no direct continuum is visible in the XMM bandpass, a direct measure of the absorbing column density was not feasible, thus the intrinsic X-ray luminosity of this source was derived only through indirect arguments. The unique bandpass and sensititvity of Suzaku above 10 keV will allow us to confirm the Compton-thick nature of this source and to measure for the first time the intrinsic X-ray luminosity of the AGN hosted in IRAS 19254-7245. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | VALENTINA BRAITO | USA | 1 | AO1 | ASSESSING THE ENERGETIC BUDGET IN THE SUPERANTENNAE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701052010/ | Quick Look | ![]() |
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330 | A85 | 10.4739 | -9.4292 | 9.841504 | -9.703266 | 5.843917 | -12.80705 | 115.23010576 | -72.15810594 | 248.2856 | 54105.4020023148 | 2007-01-05 09:38:53 | 54108.0557175926 | 2007-01-08 01:20:14 | 801041010 | 99.2012 | 100 | 99.2012 | 99.2012 | 0 | 99.2012 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.8139 | 84.8139 | 229.2421 | 2 | PROCESSED | 57536.5180671296 | 2016-05-28 12:26:01 | 54735 | 2008-09-26 00:00:00 | 54132.9388773148 | 2007-02-01 22:31:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010088 | We propose observations of A2199 and A85 clusters of galaxies with an each exposure time of 100 ks, in order to search for excess hard X-ray emission, to constrain the spectral shape, and to discuss the origin of the hard X-ray emission. Both are listed as the clusters which are detected non-thermal emission signal with 2 sigma confidence level by Beppo SAX PDS detector. In addition, these two clusters only have features of brighter X-ray flux, good size, relatively cool ICM temperature, and including no bright member AGNs. Therefore they are suitable target samples for our observational purpose about estimation photon index and flux for the excess hard X-ray emission with high significance wherever possible. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RYO SHIBATA | JAP | 1 | AO1 | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801041010/ | Quick Look | ![]() |
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331 | UGC5101 | 143.841 | 61.3185 | 142.895417 | 61.541858 | 122.479903 | 43.806931 | 152.55229096 | 42.85621781 | 331.581 | 53825.1798148148 | 2006-03-31 04:18:56 | 53826.3509722222 | 2006-04-01 08:25:24 | 701002010 | 48.9902 | 70 | 48.9902 | 48.9902 | 48.9902 | 48.9902 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43.9748 | 43.9748 | 101.1779 | 0 | PROCESSED | 57533.3610763889 | 2016-05-25 08:39:57 | 54735 | 2008-09-26 00:00:00 | 53905.890625 | 2006-06-19 21:22:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MASATOSHI IMANISHI | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701002010/ | Quick Look | ![]() |
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332 | IRAS13224-3809 | 201.327 | -38.416 | 200.607672 | -38.155977 | 214.865009 | -27.173801 | 310.18598264 | 23.97820794 | 118.5234 | 54126.2420601852 | 2007-01-26 05:48:34 | 54131.0849421296 | 2007-01-31 02:02:19 | 701003010 | 197.9376 | 200 | 197.9536 | 197.9376 | 0 | 197.9516 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 169.6526 | 169.6526 | 418.3978 | 4 | PROCESSED | 57537.0458912037 | 2016-05-29 01:06:05 | 54777 | 2008-11-07 00:00:00 | 54139.7293287037 | 2007-02-08 17:30:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010028 | We propose a 200 ks continuous observation of the narrow-line Seyfert 1 galaxy IRAS13224-3809 in order to understand its remarkable and puzzling spectral and variability properties. Suzaku data will enable us to disentangle the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. If the latter then the appearance of the source is controlled by general relativistic effects. In addition, the ability for Suzaku to conduct long continuous observations will allow us to monitor IRAS13224-3809 for giant amplitude flaring (as seen with ROSAT); therefore enabling us to enhance our understanding of AGN variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | YASUO TANAKA | JAP | 1 | AO1 | THE REMARKABLE NARROW LINE SEYFERT 1 GALAXY IRAS13224-3809 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/701003010/ | Quick Look | ![]() |
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333 | SNR 0103-72.6 | 16.2944 | -72.389 | 15.898915 | -72.656584 | 313.931508 | -65.2662 | 301.47055063 | -44.70024477 | 13.8765 | 53848.0156018518 | 2006-04-23 00:22:28 | 53849.3773032407 | 2006-04-24 09:03:19 | 501077010 | 49.2715 | 50 | 49.2795 | 49.2875 | 49.2875 | 49.2715 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.1905 | 37.1905 | 117.6299 | 3 | PROCESSED | 57533.5571296296 | 2016-05-25 13:22:16 | 54401 | 2007-10-28 00:00:00 | 53907.4220023148 | 2006-06-21 10:07:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011241 | We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 1 | AO1 | BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501077010/ | Quick Look | ![]() |
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334 | PUP A : BEK | 125.942 | -42.9405 | 125.511174 | -42.777913 | 147.596211 | -59.401563 | 260.51799115 | -3.16426215 | 276.3687 | 53842.2933449074 | 2006-04-17 07:02:25 | 53842.5807407407 | 2006-04-17 13:56:16 | 501086010 | 16.0913 | 15 | 16.0913 | 16.0993 | 16.0913 | 16.0913 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.6985 | 9.6985 | 24.797 | 0 | PROCESSED | 57533.4850115741 | 2016-05-25 11:38:25 | 54401 | 2007-10-28 00:00:00 | 53906.8467708333 | 2006-06-20 20:19:21 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501086010/ | Quick Look | ![]() |
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335 | CYGNUS_LOOP_P19 | 311.8094 | 30.0818 | 311.288879 | 29.89716 | 325.768852 | 45.764417 | 73.00862935 | -8.2918477 | 237.4997 | 54087.3411805556 | 2006-12-18 08:11:18 | 54087.8245833333 | 2006-12-18 19:47:24 | 501036010 | 18.595 | 17 | 18.595 | 18.595 | 0 | 18.595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.355 | 18.355 | 41.7559 | 0 | PROCESSED | 57536.3627199074 | 2016-05-28 08:42:19 | 54744 | 2008-10-05 00:00:00 | 54096.1443171296 | 2006-12-27 03:27:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/501036010/ | Quick Look | ![]() |
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336 | XB 1916-053 | 289.7027 | -5.2415 | 289.037629 | -5.333849 | 290.520863 | 16.806325 | 31.35614078 | -8.46800846 | 250.2538 | 54047.242974537 | 2006-11-08 05:49:53 | 54048.1119791667 | 2006-11-09 02:41:15 | 401095010 | 38.4647 | 40 | 39.0967 | 39.0887 | 38.4647 | 39.0967 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.4857 | 37.4857 | 75.082 | 2 | PROCESSED | 57536.0684259259 | 2016-05-28 01:38:32 | 54735 | 2008-09-26 00:00:00 | 54088.866087963 | 2006-12-19 20:47:10 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012038 | We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV. | GALACTIC POINT SOURCES | 4 | A | MARIA DIAZ TRIGO | EUR | 1 | AO1 | BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/401095010/ | Quick Look | ![]() |
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337 | A2142 | 239.5312 | 27.2879 | 239.014287 | 27.430116 | 229.09968 | 46.49364 | 44.29837206 | 48.74478569 | 138.1624 | 54104.1546990741 | 2007-01-04 03:42:46 | 54105.3891666667 | 2007-01-05 09:20:24 | 801055010 | 51.4525 | 60 | 51.4605 | 51.4525 | 0 | 51.4605 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.2098 | 49.2098 | 106.632 | 1 | PROCESSED | 57536.4705555556 | 2016-05-28 11:17:36 | 54735 | 2008-09-26 00:00:00 | 54111.417037037 | 2007-01-11 10:00:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010106 | We propose to reveal the formation and evolution of dense core with cold fronts with SUZAKU/XIS. Our strategy of observation is based on the results of Chandra, ROSAT and weak lensing analysis. A2142 is a galaxy cluster which has contact discontinuities, "cold fronts", between cold-dense cores and hot-thin surrounding gas. We have carried out "weak lensing analysis" and derived mass map in A2142. We measure the bulk velocity via Fe-K line in the central region. We derive the merger velocity by observing the temperatures of the heating and non-heating which are expected by our observational results. It leads to understand the formation and evolution of dense core with cold fronts, since the merger and core velocities are closely related to the evolution of dense cores with cold fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO OKABE | JAP | 1 | AO1 | REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801055010/ | Quick Look | ![]() |
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