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 766
No. |
object_name
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center_ra
|
center_dec
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center_ra_b1950
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center_dec_b1950
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center_ecliptic_lon
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center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
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observation_start_time_mjd
|
observation_start_time
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observation_end_time_mjd
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observation_end_time
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observation_id
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exposure
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awarded_exposure
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xis0_exposure
|
xis1_exposure
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xis2_exposure
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xis3_exposure
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xis0_observation_mode
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xis1_observation_mode
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xis2_observation_mode
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xis3_observation_mode
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hxd_observation_mode
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hxd_coarse_clock_rate_exposure
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hxd_first_clock_rate_exposure
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hxd_normal_clock_rate_exposure
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hxd_all_clock_rate_exposure
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hxd_wam_exposure
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quantity_of_hxd_burst
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processing_status
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processing_date_mjd
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processing_date
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public_date_mjd
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public_date
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distribution_date_mjd
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distribution_date
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processing_version
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processing_count
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processing_software
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proposal_id
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proposal_abstract
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proposal_category
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proposal_category_code
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proposal_priority
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pi_name
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co_pi_name
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proposal_affiliated_country
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proposal_cycle
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observation_type
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proposal_title
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main_instrument
|
has_xis_injection
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data_access_url
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ql_access_url
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ql_image_url
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1 | COMET_8P_TUTTLE-P2_08 | 40.0642 | -36.6693 | 39.55682 | -36.883219 | 21.03457 | -48.879704 | 242.2833952 | -65.12116443 | 253.2206 | 54490.9649421296 | 2008-01-25 23:09:31 | 54491.0959953704 | 2008-01-26 02:18:14 | 502063080 | 3.5416 | 4 | 3.5496 | 3.5416 | 0 | 3.5576 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3.564 | 3.564 | 11.3119 | 0 | PROCESSED | 57541.3990509259 | 2016-06-02 09:34:38 | 54912 | 2009-03-22 00:00:00 | 54546.1411689815 | 2008-03-21 03:23:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063080/ | Quick Look | ![]() |
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2 | GC_SOUTH_1 | 268.0988 | -29.4771 | 267.30082 | -29.465922 | 268.32614 | -6.047082 | 0.29758282 | -1.54591478 | 274.6002 | 56190.0385069444 | 2012-09-20 00:55:27 | 56191.3341435185 | 2012-09-21 08:01:10 | 507028010 | 51.7619 | 50 | 51.7619 | 51.7699 | 0 | 51.7699 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 41.1534 | 41.1534 | 111.9318 | 1 | PROCESSED | 57607.1304398148 | 2016-08-07 03:07:50 | 56584 | 2013-10-19 00:00:00 | 56218.5464930556 | 2012-10-18 13:06:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507028010/ | Quick Look | ![]() |
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3 | JUPITER | 104.4639 | 23.0622 | 103.708176 | 23.129949 | 103.287865 | 0.285992 | 192.81439153 | 11.62759441 | 264.6138 | 56767.1149421296 | 2014-04-20 02:45:31 | 56767.448125 | 2014-04-20 10:45:18 | 508023110 | 16.7417 | 160 | 16.7417 | 16.7737 | 0 | 16.7657 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9630671296 | 2016-08-14 23:06:49 | 57212 | 2015-07-09 00:00:00 | 56789.801712963 | 2014-05-12 19:14:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023110/ | Quick Look | ![]() |
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4 | CYGNUS LOOP BLOWOUT3 | 312.3799 | 29.0257 | 311.853293 | 28.839005 | 325.853846 | 44.599011 | 72.47923846 | -9.33489782 | 78.1517 | 55688.6493981482 | 2011-05-07 15:35:08 | 55689.9654976852 | 2011-05-08 23:10:19 | 506013010 | 60.2669 | 60 | 60.2669 | 60.2749 | 0 | 60.2669 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.9803 | 55.9803 | 113.6288 | 1 | PROCESSED | 57601.9873611111 | 2016-08-01 23:41:48 | 56066 | 2012-05-19 00:00:00 | 55700.4602083333 | 2011-05-19 11:02:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506013010/ | Quick Look | ![]() |
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5 | G54.1+0.3 | 292.6593 | 18.8091 | 292.105949 | 18.703083 | 298.434306 | 40.039537 | 54.05763723 | 0.20765467 | 245.096 | 54403.6644560185 | 2007-10-30 15:56:49 | 54406.3335532407 | 2007-11-02 08:00:19 | 502077010 | 101.6411 | 100 | 101.6411 | 101.6491 | 0 | 101.6491 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.9235 | 92.9235 | 230.5857 | 3 | PROCESSED | 57540.4530324074 | 2016-06-01 10:52:22 | 54786 | 2008-11-16 00:00:00 | 54417.8870833333 | 2007-11-13 21:17:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022032 | A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae. | GALACTIC DIFFUSE EMISSION | 5 | C | FABRIZIO BOCCHINO | EUR | 2 | AO2 | THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502077010/ | Quick Look | ![]() |
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6 | TYCHO SNR HXD BKGD | 9.2173 | 64.3076 | 8.488109 | 64.032592 | 44.61366 | 53.051862 | 121.35322514 | 1.48051733 | 84.2005 | 53915.6541782407 | 2006-06-29 15:42:01 | 53916.7606944444 | 2006-06-30 18:15:24 | 500025010 | 51.0088 | 50 | 51.0088 | 51.0088 | 51.0088 | 51.0088 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 48.7224 | 48.7224 | 95.5939 | 2 | PROCESSED | 57534.8010300926 | 2016-05-26 19:13:29 | 54302 | 2007-07-21 00:00:00 | 54052.5940509259 | 2006-11-13 14:15:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500025010/ | Quick Look | ![]() |
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7 | GC20 | 265.6604 | -28.73 | 264.867608 | -28.707008 | 266.169302 | -5.346539 | 359.83402449 | 0.66365416 | 262.9349 | 54385.4117939815 | 2007-10-12 09:52:59 | 54385.9099421296 | 2007-10-12 21:50:19 | 502008010 | 23.7786 | 20 | 23.7906 | 23.7866 | 0 | 23.7786 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.9234 | 22.9234 | 43.032 | 0 | PROCESSED | 57540.2572337963 | 2016-06-01 06:10:25 | 54771 | 2008-11-01 00:00:00 | 54403.0227314815 | 2007-10-30 00:32:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502008010/ | Quick Look | ![]() |
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8 | ASO0376 | 263.1417 | -31.5448 | 262.331507 | -31.509592 | 264.088273 | -8.244108 | 356.29011362 | 0.99386623 | 267.5095 | 55082.1506365741 | 2009-09-08 03:36:55 | 55083.1084606482 | 2009-09-09 02:36:11 | 504049010 | 37.2278 | 20 | 38.9878 | 39.2598 | 0 | 37.2278 | 5 | 4 | 0 | 4 | 1 | 0 | 0 | 31.8134 | 31.8134 | 82.7299 | 1 | PROCESSED | 57548.4976041667 | 2016-06-09 11:56:33 | 55479 | 2010-10-10 00:00:00 | 55113.2260069444 | 2009-10-09 05:25:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504049010/ | Quick Look | ![]() |
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9 | VELA JR P26 | 132.8787 | -46.6693 | 132.45444 | -46.480585 | 159.781455 | -60.154541 | 266.46476457 | -1.49839932 | 347.0019 | 54653.4341203704 | 2008-07-06 10:25:08 | 54653.837025463 | 2008-07-06 20:05:19 | 503038010 | 14.553 | 10 | 14.553 | 14.553 | 0 | 14.553 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.9536 | 10.9536 | 34.7839 | 0 | PROCESSED | 57542.9869675926 | 2016-06-03 23:41:14 | 55048 | 2009-08-05 00:00:00 | 54679.3709606482 | 2008-08-01 08:54:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503038010/ | Quick Look | ![]() |
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10 | 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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11 | NEP #4 | 270.0449 | 66.5788 | 270.046703 | 66.578557 | 56.874538 | 89.977746 | 96.40481628 | 29.79358389 | 165.3654 | 55193.4146875 | 2009-12-28 09:57:09 | 55194.4579166667 | 2009-12-29 10:59:24 | 504076010 | 49.8491 | 50 | 49.8571 | 49.8571 | 0 | 49.8491 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.5039 | 43.5039 | 90.114 | 0 | PROCESSED | 57550.0085648148 | 2016-06-11 00:12:20 | 54922 | 2009-04-01 00:00:00 | 55246.2930787037 | 2010-02-19 07:02:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504076010/ | Quick Look | ![]() |
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12 | MRK 421 OFFSET | 165.3836 | 38.6302 | 164.685253 | 38.899103 | 150.412438 | 29.624722 | 179.31913311 | 64.35556561 | 121.9647 | 55146.4480092593 | 2009-11-11 10:45:08 | 55148.3176388889 | 2009-11-13 07:37:24 | 504087010 | 86.0144 | 75 | 86.0144 | 86.0144 | 0 | 86.0144 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8804 | 64.8804 | 161.5199 | 3 | PROCESSED | 57549.3389583333 | 2016-06-10 08:08:06 | 55531 | 2010-12-01 00:00:00 | 55160.2701041667 | 2009-11-25 06:28:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041324 | The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. | GALACTIC DIFFUSE EMISSION | 5 | B | YANGSEN YAO | USA | 4 | AO4 | A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504087010/ | Quick Look | ![]() |
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13 | GALACTIC_BULGE10 | 268.297 | -31.6627 | 267.484676 | -31.652449 | 268.525852 | -8.230314 | 358.49964198 | -2.80216044 | 277.1297 | 55091.579525463 | 2009-09-17 13:54:31 | 55093.1508564815 | 2009-09-19 03:37:14 | 504093010 | 53.2416 | 50 | 53.2495 | 53.2416 | 0 | 53.2575 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.9072 | 46.9072 | 135.734 | 1 | PROCESSED | 57548.6254513889 | 2016-06-09 15:00:39 | 54922 | 2009-04-01 00:00:00 | 55110.3193865741 | 2009-10-06 07:39:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504093010/ | Quick Look | ![]() |
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14 | GALACTIC_BULGE8 | 267.0897 | -31.0498 | 266.281644 | -31.033699 | 267.475091 | -7.634163 | 358.49976827 | -1.60277837 | 260.4349 | 55088.8177777778 | 2009-09-14 19:37:36 | 55090.3043287037 | 2009-09-16 07:18:14 | 504091010 | 51.3316 | 50 | 51.3316 | 51.3392 | 0 | 51.3316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.7514 | 47.7514 | 128.4258 | 2 | PROCESSED | 57548.5976041667 | 2016-06-09 14:20:33 | 54922 | 2009-04-01 00:00:00 | 55109.4226736111 | 2009-10-05 10:08:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504091010/ | Quick Look | ![]() |
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15 | VELA PWN N4 | 128.8415 | -44.0453 | 128.410682 | -43.871484 | 152.26227 | -59.375821 | 262.64764922 | -2.10667439 | 326.4998 | 56110.0169097222 | 2012-07-02 00:24:21 | 56110.3459953704 | 2012-07-02 08:18:14 | 507051010 | 17.289 | 15 | 17.289 | 17.289 | 0 | 17.289 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.6558 | 17.6558 | 28.4019 | 0 | PROCESSED | 57606.5331018518 | 2016-08-06 12:47:40 | 56646 | 2013-12-20 00:00:00 | 56280.6029050926 | 2012-12-19 14:28:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507051010/ | Quick Look | ![]() |
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16 | VELA PWN W1 | 128.3503 | -45.1912 | 127.929525 | -45.019236 | 152.791152 | -60.544208 | 263.35940671 | -3.07091685 | 303.5014 | 56438.6169444444 | 2013-05-26 14:48:24 | 56439.0342476852 | 2013-05-27 00:49:19 | 508042010 | 14.1172 | 15 | 14.1172 | 14.1252 | 0 | 14.1252 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2844 | 13.2844 | 36.0239 | 0 | PROCESSED | 57611.3765046296 | 2016-08-11 09:02:10 | 56864 | 2014-07-26 00:00:00 | 56498.6138888889 | 2013-07-25 14:44:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508042010/ | Quick Look | ![]() |
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17 | G359.0-0.9 NW | 266.56 | -30.3287 | 265.756777 | -30.310042 | 266.999862 | -6.92337 | 358.88098313 | -0.83974756 | 102 | 56723.5510648148 | 2014-03-07 13:13:32 | 56724.8162268518 | 2014-03-08 19:35:22 | 508058010 | 52.0885 | 50 | 52.0885 | 52.0965 | 0 | 52.1045 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.5738 | 45.5738 | 109.2758 | 2 | PROCESSED | 57613.9935416667 | 2016-08-13 23:50:42 | 57100 | 2015-03-19 00:00:00 | 56734.6649189815 | 2014-03-18 15:57:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508058010/ | Quick Look | ![]() |
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18 | SS433_JET_KNOT | 288.5694 | 4.9037 | 287.951117 | 4.816458 | 290.852472 | 27.010013 | 39.90628699 | -2.82264549 | 256.6998 | 56597.9130555556 | 2013-11-01 21:54:48 | 56600.2502314815 | 2013-11-04 06:00:20 | 508024010 | 106.8942 | 100 | 106.8942 | 106.8942 | 0 | 106.8942 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.4583 | 102.4583 | 201.8897 | 3 | PROCESSED | 57613.2427777778 | 2016-08-13 05:49:36 | 56980 | 2014-11-19 00:00:00 | 56611.6875578704 | 2013-11-15 16:30:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080065 | We propose an observation of the jet of SS 433. Our purpose is to detect high-temperature diffuse plasma component made by the black hole jet. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDEKI UCHIYAMA | JAP | 8 | AO8 | SEARCHING DIFFUSE HOT-PLASMA COMPONENT MADE BY A BLACK HOLE JET OF SS 433 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508024010/ | Quick Look | ![]() |
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19 | 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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20 | COMET_8P_TUTTLE-P1-5 | 28.1493 | 7.0036 | 27.492979 | 6.757378 | 28.646774 | -4.267305 | 148.58110255 | -52.79544349 | 248.5006 | 54470.7825810185 | 2008-01-05 18:46:55 | 54470.8487384259 | 2008-01-05 20:22:11 | 502062050 | 1.6746 | 2 | 1.6746 | 1.6746 | 0 | 1.6746 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.703 | 1.703 | 5.6861 | 0 | PROCESSED | 57540.9980208333 | 2016-06-01 23:57:09 | 54908 | 2009-03-18 00:00:00 | 54542.2043055556 | 2008-03-17 04:54:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062050/ | Quick Look | ![]() |
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21 | COMET_8P_TUTTLE-P2_13 | 40.3641 | -37.3366 | 39.860845 | -37.549577 | 20.8839 | -49.581867 | 243.65335896 | -64.71445889 | 253.6857 | 54491.6297106482 | 2008-01-26 15:06:47 | 54491.762662037 | 2008-01-26 18:18:14 | 502063130 | 6.5907 | 6.7 | 6.6147 | 6.5987 | 0 | 6.5907 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.0221 | 5.0221 | 11.4799 | 0 | PROCESSED | 57541.4103356482 | 2016-06-02 09:50:53 | 54912 | 2009-03-22 00:00:00 | 54546.2204861111 | 2008-03-21 05:17:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063130/ | Quick Look | ![]() |
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22 | HESSJ1741-A | 265.3548 | -30.1316 | 264.55314 | -30.107106 | 265.945938 | -6.755753 | 358.50289854 | 0.15030933 | 73.8229 | 54886.7117013889 | 2009-02-24 17:04:51 | 54888.0419328704 | 2009-02-26 01:00:23 | 503076010 | 52.9323 | 50 | 52.9323 | 52.9323 | 0 | 52.9323 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7708 | 43.7708 | 114.9158 | 1 | PROCESSED | 57545.6752546296 | 2016-06-06 16:12:22 | 55330 | 2010-05-14 00:00:00 | 54902.4869791667 | 2009-03-12 11:41:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030113 | HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. | GALACTIC DIFFUSE EMISSION | 5 | C | HIRONORI MATSUMOTO | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503076010/ | Quick Look | ![]() |
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23 | BULGE 2 | 270.6176 | -29.5847 | 269.818763 | -29.585758 | 270.530563 | -6.144879 | 1.30042786 | -3.49803376 | 83.2679 | 53801.7493981482 | 2006-03-07 17:59:08 | 53802.0689699074 | 2006-03-08 01:39:19 | 500002010 | 13.028 | 10 | 13.052 | 13.044 | 13.036 | 13.028 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10.6741 | 10.6741 | 27.5999 | 1 | PROCESSED | 57533.1394444444 | 2016-05-25 03:20:48 | 54247 | 2007-05-27 00:00:00 | 54041.664525463 | 2006-11-02 15:56:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | DAN MCCAMMON | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500002010/ | Quick Look | ![]() |
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24 | 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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25 | 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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26 | COMET_8P_TUTTLE-P2_16 | 40.5411 | -37.7213 | 40.040278 | -37.933718 | 20.796624 | -49.987507 | 244.42429467 | -64.47300408 | 253.9693 | 54492.0297106482 | 2008-01-27 00:42:47 | 54492.162662037 | 2008-01-27 03:54:14 | 502063160 | 3.7705 | 4 | 3.7705 | 3.7705 | 0 | 3.7705 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.9881 | 3.9881 | 11.4799 | 0 | PROCESSED | 57541.4170833333 | 2016-06-02 10:00:36 | 54912 | 2009-03-22 00:00:00 | 54546.2311574074 | 2008-03-21 05:32:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063160/ | Quick Look | ![]() |
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27 | 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 | ![]() |
28 | COMET_8P_TUTTLE-P1-8 | 28.3076 | 6.2429 | 27.652953 | 5.997039 | 28.526064 | -5.034788 | 149.32011202 | -53.43313536 | 248.4984 | 54470.9825 | 2008-01-05 23:34:48 | 54471.0487384259 | 2008-01-06 01:10:11 | 502062080 | 3.219 | 3.2 | 3.219 | 3.219 | 0 | 3.219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.374 | 3.374 | 5.664 | 0 | PROCESSED | 57541.0065046296 | 2016-06-02 00:09:22 | 54908 | 2009-03-18 00:00:00 | 54542.2264583333 | 2008-03-17 05:26:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062080/ | Quick Look | ![]() |
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29 | RCW86_WEST | 220.2753 | -62.427 | 219.29491 | -62.212988 | 240.606158 | -43.963376 | 315.24703456 | -2.20673417 | 96.1553 | 54864.7563194444 | 2009-02-02 18:09:06 | 54866.0134259259 | 2009-02-04 00:19:20 | 503001010 | 53.5519 | 50 | 53.5519 | 53.5519 | 0 | 53.5519 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9081 | 48.9081 | 108.602 | 1 | PROCESSED | 57545.4580324074 | 2016-06-06 10:59:34 | 55329 | 2010-05-13 00:00:00 | 54880.570462963 | 2009-02-18 13:41:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503001010/ | Quick Look | ![]() |
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30 | CYGNUS LOOP (P20) | 311.9894 | 31.1824 | 311.473917 | 30.997098 | 326.586885 | 46.721175 | 73.97872298 | -7.73281487 | 50.0002 | 54596.7397685185 | 2008-05-10 17:45:16 | 54597.51 | 2008-05-11 12:14:24 | 503056010 | 30.1129 | 25 | 30.1129 | 30.1343 | 0 | 30.1209 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.2057 | 27.2057 | 66.5339 | 0 | PROCESSED | 57545.8695023148 | 2016-06-06 20:52:05 | 54972 | 2009-05-21 00:00:00 | 54606.1121759259 | 2008-05-20 02:41:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503056010/ | Quick Look | ![]() |
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31 | 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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32 | VELA JR P30 | 134.1665 | -46.7036 | 133.737948 | -46.510338 | 161.294913 | -59.700207 | 267.059354 | -0.84402772 | 347.0006 | 54654.7208449074 | 2008-07-07 17:18:01 | 54655.0844328704 | 2008-07-08 02:01:35 | 503042010 | 10.1159 | 10 | 10.1159 | 10.1159 | 0 | 10.1159 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.0536 | 10.0536 | 31.3839 | 0 | PROCESSED | 57542.9967592593 | 2016-06-03 23:55:20 | 55048 | 2009-08-05 00:00:00 | 54679.397962963 | 2008-08-01 09:33:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503042010/ | Quick Look | ![]() |
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33 | ERIDANUS HOLE | 67.1401 | -17.0746 | 66.578414 | -17.184035 | 61.759444 | -38.302767 | 213.43674881 | -39.09232011 | 64.2755 | 54311.0359606482 | 2007-07-30 00:51:47 | 54313.2161921296 | 2007-08-01 05:11:19 | 502076010 | 103.7523 | 100 | 103.7523 | 103.7523 | 0 | 103.7523 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.2091 | 92.2091 | 188.3518 | 2 | PROCESSED | 57539.4003356482 | 2016-05-31 09:36:29 | 54710 | 2008-09-01 00:00:00 | 54340.7341898148 | 2007-08-28 17:37:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | MASSIMILIANO GALEAZZI | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502076010/ | Quick Look | ![]() |
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34 | 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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35 | 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 | ![]() |
36 | ASO0078 | 59.472 | 32.09 | 58.682067 | 31.946958 | 63.963224 | 11.368156 | 162.76236061 | -16.0043339 | 83.0007 | 55045.8202777778 | 2009-08-02 19:41:12 | 55046.3273032407 | 2009-08-03 07:51:19 | 504041010 | 21.312 | 20 | 21.32 | 21.32 | 0 | 21.312 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.2959 | 21.2959 | 43.7999 | 0 | PROCESSED | 57548.0349074074 | 2016-06-09 00:50:16 | 55430 | 2010-08-22 00:00:00 | 55064.0383912037 | 2009-08-21 00:55:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504041010/ | Quick Look | ![]() |
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37 | 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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38 | JUPITER | 103.8837 | 23.1078 | 103.127442 | 23.17281 | 102.752218 | 0.279385 | 192.54363279 | 11.16228902 | 264.4065 | 56762.7225115741 | 2014-04-15 17:20:25 | 56763.066099537 | 2014-04-16 01:35:11 | 508023030 | 8.9125 | 160 | 8.9125 | 8.9125 | 0 | 8.9125 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.9063 | 6.9063 | 22.6469 | 0 | PROCESSED | 57614.254212963 | 2016-08-14 06:06:04 | 57212 | 2015-07-09 00:00:00 | 56833.5559722222 | 2014-06-25 13:20:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023030/ | Quick Look | ![]() |
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39 | HESSJ1741-B | 265.2407 | -30.3098 | 264.437915 | -30.284751 | 265.852586 | -6.937089 | 358.29952005 | 0.1396669 | 74.0024 | 54888.0423611111 | 2009-02-26 01:01:00 | 54889.4828587963 | 2009-02-27 11:35:19 | 503077010 | 51.2616 | 50 | 51.2696 | 51.2616 | 0 | 51.2696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7072 | 43.7072 | 124.4239 | 1 | PROCESSED | 57545.6763773148 | 2016-06-06 16:13:59 | 55330 | 2010-05-14 00:00:00 | 54908.5791550926 | 2009-03-18 13:53:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030113 | HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. | GALACTIC DIFFUSE EMISSION | 5 | C | HIRONORI MATSUMOTO | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503077010/ | Quick Look | ![]() |
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40 | JUPITER | 104.3715 | 23.0706 | 103.615684 | 23.137913 | 103.202438 | 0.28593 | 192.77027841 | 11.55390373 | 264.582 | 56766.448287037 | 2014-04-19 10:45:32 | 56766.781400463 | 2014-04-19 18:45:13 | 508023090 | 11.9454 | 160 | 11.9534 | 11.9454 | 0 | 11.9614 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9588773148 | 2016-08-14 23:00:47 | 57212 | 2015-07-09 00:00:00 | 56782.506099537 | 2014-05-05 12:08:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023090/ | Quick Look | ![]() |
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41 | GRXE_E_10 | 267.9015 | -25.9408 | 267.12546 | -25.928719 | 268.101648 | -2.513628 | 3.25115356 | 0.4070413 | 105.0001 | 56362.3793865741 | 2013-03-11 09:06:19 | 56364.8778472222 | 2013-03-13 21:04:06 | 507075010 | 101.3428 | 100 | 101.3428 | 101.3428 | 0 | 101.3428 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.2422 | 88.2422 | 215.806 | 2 | PROCESSED | 57610.8450462963 | 2016-08-10 20:16:52 | 56018 | 2012-04-01 00:00:00 | 56377.5882175926 | 2013-03-26 14:07:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507075010/ | Quick Look | ![]() |
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42 | MBM16 | 49.7694 | 11.5801 | 49.085806 | 11.399029 | 50.444533 | -6.508969 | 170.60605682 | -37.27197306 | 254.9211 | 56331.4284606482 | 2013-02-08 10:16:59 | 56333.553587963 | 2013-02-10 13:17:10 | 507076020 | 80.9506 | 80 | 80.9746 | 80.9506 | 0 | 80.9746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.3076 | 69.3076 | 183.5839 | 2 | PROCESSED | 57610.5874074074 | 2016-08-10 14:05:52 | 56018 | 2012-04-01 00:00:00 | 56349.5813657407 | 2013-02-26 13:57:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076020/ | Quick Look | ![]() |
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43 | VELA JR P27 | 133.2844 | -46.6061 | 132.858246 | -46.415943 | 160.180564 | -59.949881 | 266.59417196 | -1.24373956 | 347.0008 | 54653.8375925926 | 2008-07-06 20:06:08 | 54654.1668865741 | 2008-07-07 04:00:19 | 503039010 | 11.0337 | 10 | 11.0417 | 11.0417 | 0 | 11.0337 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.3372 | 11.3372 | 28.4479 | 0 | PROCESSED | 57542.9844560185 | 2016-06-03 23:37:37 | 55048 | 2009-08-05 00:00:00 | 54679.3497222222 | 2008-08-01 08:23:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503039010/ | Quick Look | ![]() |
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44 | SGR D SNR | 267.1922 | -28.1274 | 266.402882 | -28.111843 | 267.506075 | -4.710631 | 1.05009547 | -0.17236121 | 267.8977 | 54349.018599537 | 2007-09-06 00:26:47 | 54352.6738310185 | 2007-09-09 16:10:19 | 502020010 | 139.0808 | 133 | 139.0808 | 139.0808 | 0 | 139.0808 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124.5025 | 124.5025 | 315.7798 | 1 | PROCESSED | 57540.026087963 | 2016-06-01 00:37:34 | 54776 | 2008-11-06 00:00:00 | 54371.5203472222 | 2007-09-28 12:29:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020031 | We propose a 100 ksec observation of the Sgr D region. This region contains a supernova remnant (SNR), a massive molecular cloud, an HII region and diffuse TeV gamma-ray emission. The objectives are to detect Sgr D SNR and diffuse X-rays from the TeV source, to discover new SNRs and X-ray Reflection Nebulae (XRNe), and to investigate the spatial distribution of high temperature plasma connecting the Galactic center and the Galactic ridge regions. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 2 | AO2 | OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502020010/ | Quick Look | ![]() |
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45 | HESSJ1857-A | 284.2126 | 2.7519 | 283.584668 | 2.685017 | 285.744612 | 25.418977 | 35.99783049 | 0.0515802 | 269.8116 | 55822.9197800926 | 2011-09-18 22:04:29 | 55823.984212963 | 2011-09-19 23:37:16 | 506019010 | 40.9249 | 40 | 40.9249 | 40.9249 | 0 | 40.9249 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.8469 | 35.8469 | 91.9279 | 1 | PROCESSED | 57603.2046180556 | 2016-08-03 04:54:39 | 56233 | 2012-11-02 00:00:00 | 55865.2326157407 | 2011-10-31 05:34:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506019010/ | Quick Look | ![]() |
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46 | IC 443 | 94.2974 | 22.7535 | 93.540286 | 22.772525 | 93.964523 | -0.628288 | 188.8890151 | 3.10517693 | 91.6993 | 56197.2290277778 | 2012-09-27 05:29:48 | 56199.7780324074 | 2012-09-29 18:40:22 | 507015010 | 101.8023 | 400 | 101.8103 | 101.8023 | 0 | 101.8103 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.994 | 91.994 | 220.1877 | 0 | PROCESSED | 57607.2728472222 | 2016-08-07 06:32:54 | 56018 | 2012-04-01 00:00:00 | 56225.5965162037 | 2012-10-25 14:18:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015010/ | Quick Look | ![]() |
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47 | FERMI_BUBBLE_N4 | 233.8333 | 7.0797 | 233.2207 | 7.24518 | 229.504794 | 25.578453 | 13.3126084 | 46.30488493 | 287.5 | 56146.4387268518 | 2012-08-07 10:31:46 | 56146.9862615741 | 2012-08-07 23:40:13 | 507004010 | 20.9469 | 20 | 20.9509 | 20.9469 | 0 | 20.9549 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.7048 | 20.7048 | 47.306 | 2 | PROCESSED | 57606.7955787037 | 2016-08-06 19:05:38 | 56535 | 2013-08-31 00:00:00 | 56169.0484375 | 2012-08-30 01:09:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507004010/ | Quick Look | ![]() |
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48 | BULGE 3 | 274.7046 | -31.4846 | 273.893726 | -31.505472 | 274.041648 | -8.109784 | 1.3002625 | -7.49777303 | 80.4025 | 53800.3437962963 | 2006-03-06 08:15:04 | 53801.7474421296 | 2006-03-07 17:56:19 | 500001010 | 51.8468 | 50 | 51.8548 | 51.8548 | 51.8548 | 51.8468 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.0783 | 45.0783 | 121.2459 | 0 | PROCESSED | 57533.1540972222 | 2016-05-25 03:41:54 | 54247 | 2007-05-27 00:00:00 | 54041.7128703704 | 2006-11-02 17:06:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | DAN MCCAMMON | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500001010/ | Quick Look | ![]() |
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49 | SN1006 NW | 225.6364 | -41.8003 | 224.819551 | -41.604176 | 235.339658 | -23.546444 | 327.59294648 | 14.70833496 | 115.0008 | 53766.4881365741 | 2006-01-31 11:42:55 | 53767.55375 | 2006-02-01 13:17:24 | 500017010 | 53.0194 | 50 | 53.0194 | 53.0277 | 53.0273 | 53.0273 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.4123 | 60.4123 | 92.0679 | 0 | PROCESSED | 57532.8347685185 | 2016-05-24 20:02:04 | 54247 | 2007-05-27 00:00:00 | 54040.7669675926 | 2006-11-01 18:24:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500017010/ | Quick Look | ![]() |
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50 | GC15 | 266.9617 | -29.4257 | 266.164223 | -29.409004 | 267.329759 | -6.012747 | 359.83382525 | -0.66952641 | 260.7835 | 54383.1536226852 | 2007-10-10 03:41:13 | 54383.6391666667 | 2007-10-10 15:20:24 | 502003010 | 21.4671 | 20 | 21.4751 | 21.4671 | 0 | 21.4751 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9225 | 18.9225 | 41.9439 | 0 | PROCESSED | 57540.2312731482 | 2016-06-01 05:33:02 | 54771 | 2008-11-01 00:00:00 | 54402.7485532407 | 2007-10-29 17:57:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502003010/ | Quick Look | ![]() |
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51 | VELA JR P2 | 132.1691 | -45.7748 | 131.740578 | -45.588644 | 157.998003 | -59.663034 | 265.4613949 | -1.31133586 | 347.0033 | 54285.6908217593 | 2007-07-04 16:34:47 | 54285.9036342593 | 2007-07-04 21:41:14 | 502024010 | 10.8502 | 10 | 10.8742 | 10.8662 | 0 | 10.8502 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6037 | 9.6037 | 18.3759 | 0 | PROCESSED | 57539.0914467593 | 2016-05-31 02:11:41 | 54696 | 2008-08-18 00:00:00 | 54328.4167361111 | 2007-08-16 10:00:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502024010/ | Quick Look | ![]() |
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52 | VELA JR P33 | 133.4681 | -47.1616 | 133.045488 | -46.970785 | 161.00407 | -60.345222 | 267.10091899 | -1.50393046 | 347.0007 | 54655.5652777778 | 2008-07-08 13:34:00 | 54656.0084837963 | 2008-07-09 00:12:13 | 503045010 | 12.0155 | 10 | 12.0155 | 12.0155 | 0 | 12.0155 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.0116 | 11.0116 | 38.2899 | 0 | PROCESSED | 57543.0047106482 | 2016-06-04 00:06:47 | 55048 | 2009-08-05 00:00:00 | 54679.4195601852 | 2008-08-01 10:04:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503045010/ | Quick Look | ![]() |
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53 | MBM36 | 238.3613 | -4.7912 | 237.701072 | -4.643799 | 237.20756 | 15.120262 | 4.0047136 | 35.6981582 | 275.8793 | 56894.6980324074 | 2014-08-25 16:45:10 | 56896.6598958333 | 2014-08-27 15:50:15 | 509074010 | 83.1887 | 80 | 83.1967 | 83.1887 | 0 | 83.1967 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3.755 | 3.755 | 8.94 | 0 | PROCESSED | 57616.559525463 | 2016-08-16 13:25:43 | 56748 | 2014-04-01 00:00:00 | 56929.2087615741 | 2014-09-29 05:00:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509074010/ | Quick Look | ![]() |
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54 | GB_NORTH_4 | 264.8998 | -28.3109 | 264.109826 | -28.284233 | 265.484852 | -4.949634 | 359.83607677 | 1.45248781 | 106.6967 | 57110.9717708333 | 2015-03-29 23:19:21 | 57113.0203472222 | 2015-04-01 00:29:18 | 509080010 | 88.1941 | 100 | 88.1941 | 95.0455 | 0 | 95.0615 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8835648148 | 2016-08-17 21:12:20 | 56748 | 2014-04-01 00:00:00 | 57125.4051736111 | 2015-04-13 09:43:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509080010/ | Quick Look | ![]() |
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55 | 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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56 | 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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57 | CTB109 NOTHWEST | 345.2638 | 59.0349 | 344.742477 | 58.766045 | 23.94959 | 57.015916 | 109.14185824 | -0.84931137 | 252.0017 | 55908.2838078704 | 2011-12-13 06:48:41 | 55909.1988078704 | 2011-12-14 04:46:17 | 506037010 | 40.7488 | 40 | 40.7488 | 40.7568 | 0 | 40.7648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.201 | 39.201 | 79.044 | 0 | PROCESSED | 57604.1345601852 | 2016-08-04 03:13:46 | 56288 | 2012-12-27 00:00:00 | 55921.0397685185 | 2011-12-26 00:57:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506037010/ | Quick Look | ![]() |
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58 | OFF-FIELD2 | 312.2284 | -9.8925 | 311.551158 | -10.078408 | 311.903273 | 7.617962 | 37.42106637 | -30.55240738 | 73.668 | 56784.946724537 | 2014-05-07 22:43:17 | 56787.0627314815 | 2014-05-10 01:30:20 | 509043010 | 80.156 | 80 | 80.156 | 80.156 | 0 | 80.156 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.6142 | 69.6142 | 182.8079 | 1 | PROCESSED | 57615.1427430556 | 2016-08-15 03:25:33 | 56748 | 2014-04-01 00:00:00 | 56861.5828240741 | 2014-07-23 13:59:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509043010/ | Quick Look | ![]() |
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59 | CTB109 SOUTHEAST | 345.764 | 58.7015 | 345.237296 | 58.43203 | 23.8569 | 56.597018 | 109.24155205 | -1.25930647 | 252.0022 | 55910.7526851852 | 2011-12-15 18:03:52 | 55911.4007638889 | 2011-12-16 09:37:06 | 506040010 | 30.4455 | 30 | 30.4455 | 30.4455 | 0 | 30.4455 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.7511 | 28.7511 | 55.9879 | 1 | PROCESSED | 57604.1444212963 | 2016-08-04 03:27:58 | 56289 | 2012-12-28 00:00:00 | 55922.0080555556 | 2011-12-27 00:11:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506040010/ | Quick Look | ![]() |
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60 | HESS J1356-645 1 | 209.4297 | -64.5068 | 208.507718 | -64.263148 | 235.862386 | -48.071536 | 309.98959301 | -2.54712319 | 106.5083 | 56318.4192939815 | 2013-01-26 10:03:47 | 56320.0002083333 | 2013-01-28 00:00:18 | 507019010 | 55.7489 | 50 | 55.762 | 55.7569 | 0 | 55.7489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.1023 | 65.1023 | 136.5678 | 2 | PROCESSED | 57608.6328587963 | 2016-08-08 15:11:19 | 56708 | 2014-02-20 00:00:00 | 56342.6666319444 | 2013-02-19 15:59:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070017 | Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission. | GALACTIC DIFFUSE EMISSION | 5 | C | TAKAHISA FUJINAGA | JAP | 7 | AO7 | OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507019010/ | Quick Look | ![]() |
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61 | SN1006_SE1 | 225.8641 | -42.0384 | 225.045074 | -41.843059 | 235.594631 | -23.72201 | 327.62177329 | 14.41744154 | 286.0629 | 56883.8521064815 | 2014-08-14 20:27:02 | 56887.5210648148 | 2014-08-18 12:30:20 | 509082010 | 201.8322 | 480 | 201.8322 | 202.4881 | 0 | 202.5201 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5228240741 | 2016-08-16 12:32:52 | 56748 | 2014-04-01 00:00:00 | 56910.6390509259 | 2014-09-10 15:20:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082010/ | Quick Look | ![]() |
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62 | SN1006_SE1 | 225.857 | -42.039 | 225.037992 | -41.843634 | 235.58934 | -23.724178 | 327.61674963 | 14.4195613 | 107.6985 | 57063.4521643518 | 2015-02-10 10:51:07 | 57069.9807060185 | 2015-02-16 23:32:13 | 509082020 | 258.382 | 280 | 258.382 | 278.7901 | 0 | 278.8541 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6457523148 | 2016-08-17 15:29:53 | 56748 | 2014-04-01 00:00:00 | 57080.4416898148 | 2015-02-27 10:36:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082020/ | Quick Look | ![]() |
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63 | H2356_VICINITY_A | 359.8969 | -30.2089 | 359.255002 | -30.487352 | 346.863445 | -27.454803 | 14.71906615 | -78.22459894 | 68.0006 | 55696.8464583333 | 2011-05-15 20:18:54 | 55698.0938773148 | 2011-05-17 02:15:11 | 506028010 | 52.1657 | 50 | 52.1657 | 52.1657 | 0 | 52.1657 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5791 | 46.5791 | 107.7539 | 1 | PROCESSED | 57602.0723148148 | 2016-08-02 01:44:08 | 56075 | 2012-05-28 00:00:00 | 55708.0697106482 | 2011-05-27 01:40:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060075 | We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium. | GALACTIC DIFFUSE EMISSION | 5 | A | YOH TAKEI | JAP | 6 | AO6 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506028010/ | Quick Look | ![]() |
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64 | H2356_VICINITY_B | 359.9868 | -29.9493 | 359.345168 | -30.227755 | 347.07269 | -27.257526 | 15.89682365 | -78.35224854 | 69.5008 | 55698.0951388889 | 2011-05-17 02:17:00 | 55699.3474305556 | 2011-05-18 08:20:18 | 506029010 | 51.4072 | 50 | 51.4312 | 51.4232 | 0 | 51.4072 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.546 | 42.546 | 108.1559 | 1 | PROCESSED | 57602.0868402778 | 2016-08-02 02:05:03 | 56075 | 2012-05-28 00:00:00 | 55708.1035069444 | 2011-05-27 02:29:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060075 | We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium. | GALACTIC DIFFUSE EMISSION | 5 | A | YOH TAKEI | JAP | 6 | AO6 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506029010/ | Quick Look | ![]() |
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65 | HESS_J1809-193_S | 272.3365 | -19.5311 | 271.597005 | -19.540657 | 272.197453 | 3.891828 | 10.84429394 | 0.04252392 | 106.4999 | 54557.6901851852 | 2008-04-01 16:33:52 | 54558.6161805556 | 2008-04-02 14:47:18 | 503079010 | 44.2481 | 40 | 44.2481 | 44.2481 | 0 | 44.2481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.2142 | 32.2142 | 79.9698 | 1 | PROCESSED | 57542.0277546296 | 2016-06-03 00:39:58 | 54950 | 2009-04-29 00:00:00 | 54570.1866666667 | 2008-04-14 04:28:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030126 | A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAYASU ANADA | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503079010/ | Quick Look | ![]() |
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66 | CYG_BGD1 | 306.6527 | 39.4856 | 306.195949 | 39.320312 | 325.617981 | 56.073001 | 78.0015669 | 0.73572902 | 218.9004 | 56280.1666666667 | 2012-12-19 04:00:00 | 56280.6286458333 | 2012-12-19 15:05:15 | 507041010 | 26.9324 | 25 | 26.9404 | 26.9324 | 0 | 26.9404 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.4527 | 20.4527 | 39.9119 | 0 | PROCESSED | 57608.3151273148 | 2016-08-08 07:33:47 | 56683 | 2014-01-26 00:00:00 | 56316.5312268518 | 2013-01-24 12:44:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070060 | The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507041010/ | Quick Look | ![]() |
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67 | GALACTIC_BULGE1 | 267.2201 | -29.3677 | 266.422949 | -29.352259 | 267.554885 | -5.950193 | 359.99969448 | -0.83243485 | 274.7 | 55118.4798148148 | 2009-10-14 11:30:56 | 55119.6453587963 | 2009-10-15 15:29:19 | 504088010 | 47.23 | 50 | 47.23 | 47.23 | 0 | 47.23 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.6139 | 32.6139 | 100.7 | 2 | PROCESSED | 57548.8825231482 | 2016-06-09 21:10:50 | 54922 | 2009-04-01 00:00:00 | 55134.0688425926 | 2009-10-30 01:39:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504088010/ | Quick Look | ![]() |
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68 | GALACTIC_BULGE9 | 267.6768 | -31.2805 | 266.867115 | -31.267244 | 267.986252 | -7.855618 | 358.55970985 | -2.15232996 | 265.3076 | 55090.3066550926 | 2009-09-16 07:21:35 | 55091.5758564815 | 2009-09-17 13:49:14 | 504092010 | 50.9199 | 50 | 50.9439 | 50.9359 | 0 | 50.9199 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.5744 | 45.5744 | 109.6459 | 1 | PROCESSED | 57548.6135069444 | 2016-06-09 14:43:27 | 54922 | 2009-04-01 00:00:00 | 55109.4315740741 | 2009-10-05 10:21:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504092010/ | Quick Look | ![]() |
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69 | JUPITER | 103.8407 | 23.1129 | 103.084394 | 23.177707 | 102.712362 | 0.280692 | 192.5219391 | 11.12856775 | 264.3937 | 56762.3891782407 | 2014-04-15 09:20:25 | 56762.7223611111 | 2014-04-15 17:20:12 | 508023020 | 15.4083 | 160 | 15.4083 | 15.4083 | 0 | 15.4083 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.2744 | 12.2744 | 28.7839 | 1 | PROCESSED | 57614.2553819445 | 2016-08-14 06:07:45 | 57212 | 2015-07-09 00:00:00 | 56778.6154166667 | 2014-05-01 14:46:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023020/ | Quick Look | ![]() |
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70 | BULGE 6 | 282.6839 | -33.8925 | 281.860158 | -33.951684 | 280.687841 | -10.9215 | 1.99857856 | -14.59644221 | 88.3467 | 53802.7373032407 | 2006-03-08 17:41:43 | 53803.0466087963 | 2006-03-09 01:07:07 | 500003010 | 14.2617 | 10 | 14.2617 | 14.2617 | 14.2617 | 14.2617 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11.414 | 11.414 | 26.7159 | 1 | PROCESSED | 57533.1570833333 | 2016-05-25 03:46:12 | 54247 | 2007-05-27 00:00:00 | 54041.7424305556 | 2006-11-02 17:49:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | DAN MCCAMMON | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500003010/ | Quick Look | ![]() |
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71 | RXJ1713-3946_ID3 | 258.1658 | -40.0306 | 257.296734 | -39.971421 | 260.540524 | -16.976597 | 347.01547145 | -0.49239611 | 87.0009 | 55244.1262847222 | 2010-02-17 03:01:51 | 55244.4779398148 | 2010-02-17 11:28:14 | 504029010 | 20.8716 | 20 | 20.9036 | 20.9036 | 0 | 20.8716 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.8868 | 20.8868 | 30.3759 | 0 | PROCESSED | 57550.6116087963 | 2016-06-11 14:40:43 | 55622 | 2011-03-02 00:00:00 | 55256.0720601852 | 2010-03-01 01:43:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504029010/ | Quick Look | ![]() |
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72 | HOT BLOB 2 | 131.2547 | 53.3234 | 130.330211 | 53.505247 | 118.317658 | 33.861433 | 164.89716269 | 38.20704104 | 284.8982 | 57137.3573842593 | 2015-04-25 08:34:38 | 57139.1293055556 | 2015-04-27 03:06:12 | 509008010 | 46.0224 | 80 | 46.0224 | 77.9795 | 0 | 78.0115 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.041412037 | 2016-08-18 00:59:38 | 57520 | 2016-05-12 00:00:00 | 57154.4516087963 | 2015-05-12 10:50:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090044 | Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIO SEKIYA | JAP | 9 | AO9 | ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509008010/ | Quick Look | ![]() |
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73 | IC 443 | 94.3028 | 22.7465 | 93.545727 | 22.765551 | 93.96971 | -0.635136 | 188.89754986 | 3.10625906 | 259.0005 | 56378.1771527778 | 2013-03-27 04:15:06 | 56379.6668865741 | 2013-03-28 16:00:19 | 507015020 | 59.2712 | 300 | 59.2712 | 59.2712 | 0 | 59.2712 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.2705 | 51.2705 | 128.6878 | 3 | PROCESSED | 57610.9601388889 | 2016-08-10 23:02:36 | 56018 | 2012-04-01 00:00:00 | 56391.749224537 | 2013-04-09 17:58:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015020/ | Quick Look | ![]() |
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74 | LOW_LATITUDE_97-10 | 311.8076 | 60.1112 | 311.52726 | 59.92615 | 0.701483 | 70.601802 | 96.61384914 | 10.40907029 | 101.0346 | 54571.1324652778 | 2008-04-15 03:10:45 | 54572.8890509259 | 2008-04-16 21:20:14 | 503075010 | 79.8119 | 80 | 79.8199 | 79.8279 | 0 | 79.8119 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.8105 | 80.8105 | 151.7498 | 2 | PROCESSED | 57542.342962963 | 2016-06-03 08:13:52 | 54953 | 2009-05-02 00:00:00 | 54581.3271643518 | 2008-04-25 07:51:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030105 | Suzaku observations of diffuse background emission indicate galactic-latitude dependence of OVII intensity. The result of our AO-2 observation strongly supports this dependence. This suggests that the major part of the emission is originating from the halo or the extended disk of our galaxy. In order to confirm the galactic-latitude dependency and to constrain the spatial distribution of the OVII emitting gas, we propose to observe diffuse radiation at a low galactic latitude of ~ 10 deg. | GALACTIC DIFFUSE EMISSION | 5 | B | TOMOTAKA YOSHINO | JAP | 3 | AO3 | RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503075010/ | Quick Look | ![]() |
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75 | 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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76 | 73P/SW3 | 279.6627 | 33.4734 | 279.203358 | 33.427762 | 284.650097 | 56.423756 | 62.35168426 | 17.03145652 | 46.5564 | 53862.4804282407 | 2006-05-07 11:31:49 | 53862.5419444444 | 2006-05-07 13:00:24 | 500012020 | 3.248 | 5 | 3.248 | 3.248 | 3.248 | 3.248 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.1119 | 2.1119 | 5.2799 | 0 | PROCESSED | 57533.7332407407 | 2016-05-25 17:35:52 | 54256 | 2007-06-05 00:00:00 | 54042.2282175926 | 2006-11-03 05:28:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012020/ | Quick Look | ![]() |
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77 | 73P/SW3 | 316.717 | 24.6807 | 316.164001 | 24.478965 | 328.484877 | 39.12074 | 71.53645371 | -15.07849931 | 72.7087 | 53868.1752314815 | 2006-05-13 04:12:20 | 53868.2085532407 | 2006-05-13 05:00:19 | 500013010 | 2.353 | 20 | 2.353 | 2.353 | 2.353 | 2.353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.595 | 2.595 | 2.8719 | 0 | PROCESSED | 57534.2831597222 | 2016-05-26 06:47:45 | 54256 | 2007-06-05 00:00:00 | 54042.2312268518 | 2006-11-03 05:32:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013010/ | Quick Look | ![]() |
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78 | 73P/SW3 | 317.1042 | 24.5187 | 316.549923 | 24.315676 | 328.827114 | 38.838912 | 71.64340536 | -15.45205291 | 72.7099 | 53868.2091666667 | 2006-05-13 05:01:12 | 53868.2752199074 | 2006-05-13 06:36:19 | 500013020 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.467 | 3.467 | 5.7039 | 0 | PROCESSED | 57534.2879398148 | 2016-05-26 06:54:38 | 54256 | 2007-06-05 00:00:00 | 54042.2634027778 | 2006-11-03 06:19:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013020/ | Quick Look | ![]() |
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79 | 73P/SW3 | 319.1503 | 23.6322 | 318.589279 | 23.422515 | 330.602424 | 37.314629 | 72.21442919 | -17.44595626 | 72.7095 | 53868.5425 | 2006-05-13 13:01:12 | 53868.6085532407 | 2006-05-13 14:36:19 | 500013070 | 3.0624 | 20 | 3.0624 | 3.0624 | 3.0624 | 3.0624 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.088 | 2.088 | 5.688 | 1 | PROCESSED | 57534.3049074074 | 2016-05-26 07:19:04 | 54256 | 2007-06-05 00:00:00 | 54042.3037268518 | 2006-11-03 07:17:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013070/ | Quick Look | ![]() |
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80 | 73P/SW3 | 17.8447 | -9.1515 | 17.217751 | -9.416998 | 12.842123 | -15.443966 | 138.54867442 | -71.41609802 | 59.3994 | 53893.7363888889 | 2006-06-07 17:40:24 | 53893.8023032407 | 2006-06-07 19:15:19 | 500014020 | 3.2369 | 35 | 3.2369 | 3.2369 | 3.2369 | 3.2369 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.478 | 2.478 | 5.6879 | 0 | PROCESSED | 57534.5816435185 | 2016-05-26 13:57:34 | 54267 | 2007-06-16 00:00:00 | 54052.5079861111 | 2006-11-13 12:11:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014020/ | Quick Look | ![]() |
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81 | 73P/SW3 | 18.0085 | -9.2093 | 17.381763 | -9.474557 | 12.972897 | -15.560645 | 139.0853548 | -71.43220951 | 59.4015 | 53893.9358333333 | 2006-06-07 22:27:36 | 53894.0023032407 | 2006-06-08 00:03:19 | 500014050 | 3.235 | 35 | 3.235 | 3.235 | 3.235 | 3.235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.5041 | 2.5041 | 5.7359 | 0 | PROCESSED | 57534.5878125 | 2016-05-26 14:06:27 | 54267 | 2007-06-16 00:00:00 | 54052.5317361111 | 2006-11-13 12:45:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014050/ | Quick Look | ![]() |
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82 | 73P/SW3 | 18.1094 | -9.2436 | 17.482792 | -9.508708 | 13.054019 | -15.631304 | 139.41528011 | -71.44015907 | 59.3996 | 53894.0691666667 | 2006-06-08 01:39:36 | 53894.1356365741 | 2006-06-08 03:15:19 | 500014070 | 2.2209 | 35 | 2.2209 | 2.2209 | 2.2209 | 2.2209 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.939 | 1.939 | 5.7359 | 1 | PROCESSED | 57534.589849537 | 2016-05-26 14:09:23 | 54267 | 2007-06-16 00:00:00 | 54052.5472800926 | 2006-11-13 13:08:05 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014070/ | Quick Look | ![]() |
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83 | 73P/SW3 | 18.2503 | -9.299 | 17.623885 | -9.563897 | 13.164284 | -15.736856 | 139.88257526 | -71.45759255 | 59.3985 | 53894.2691435185 | 2006-06-08 06:27:34 | 53894.3356134259 | 2006-06-08 08:03:17 | 500014100 | 1.3121 | 35 | 1.3121 | 1.3121 | 1.3121 | 1.3121 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.322 | 1.322 | 5.742 | 0 | PROCESSED | 57534.5960185185 | 2016-05-26 14:18:16 | 54267 | 2007-06-16 00:00:00 | 54052.5405324074 | 2006-11-13 12:58:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014100/ | Quick Look | ![]() |
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84 | 73P/SW3 | 18.435 | -9.3697 | 17.808837 | -9.63432 | 13.309685 | -15.873419 | 140.49459076 | -71.47695116 | 59.4003 | 53894.5358333333 | 2006-06-08 12:51:36 | 53894.6016087963 | 2006-06-08 14:26:19 | 500014140 | 1.977 | 35 | 1.977 | 1.977 | 1.977 | 1.977 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.951 | 1.951 | 5.6719 | 0 | PROCESSED | 57534.60375 | 2016-05-26 14:29:24 | 54267 | 2007-06-16 00:00:00 | 54052.5450231482 | 2006-11-13 13:04:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014140/ | Quick Look | ![]() |
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85 | MBM12 | 44.0042 | 19.487 | 43.295962 | 19.285573 | 47.250431 | 2.610049 | 159.18888296 | -34.46916863 | 253.4644 | 53769.9600578704 | 2006-02-03 23:02:29 | 53772.6460416667 | 2006-02-06 15:30:18 | 500015010 | 102.9371 | 100 | 102.9371 | 102.9371 | 102.9371 | 102.9371 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.6709 | 93.6709 | 232.0499 | 1 | PROCESSED | 57532.9850694444 | 2016-05-24 23:38:30 | 54247 | 2007-05-27 00:00:00 | 54041.1327662037 | 2006-11-02 03:11:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001059 | Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB. | GALACTIC DIFFUSE EMISSION | 5 | A | RANDALL SMITH | JAP | 0 | SWG | DATING THE LOCAL HOT BUBBLE WITH SUZAKU | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500015010/ | Quick Look | ![]() |
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86 | CYGNUS LOOP NE4 | 313.5005 | 32.369 | 312.987812 | 32.178281 | 329.006135 | 47.302265 | 75.72495347 | -7.98937114 | 221.2023 | 53704.2368287037 | 2005-11-30 05:41:02 | 53704.7661342593 | 2005-11-30 18:23:14 | 500023010 | 25.0049 | 20 | 25.0049 | 25.2689 | 25.0067 | 25.0689 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.1249 | 25.1249 | 45.726 | 1 | PROCESSED | 57532.3510763889 | 2016-05-24 08:25:33 | 54247 | 2007-05-27 00:00:00 | 54038.67625 | 2006-10-30 16:13:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500023010/ | Quick Look | ![]() |
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87 | VICINITY OF LMC X-3 | 83.4844 | -63.8863 | 83.408578 | -63.918105 | 41.435206 | -86.187449 | 273.3865557 | -32.64248934 | 284.6189 | 53811.6008333333 | 2006-03-17 14:25:12 | 53813.9168055556 | 2006-03-19 22:00:12 | 500031010 | 82.0185 | 80 | 82.0265 | 82.0185 | 82.0265 | 82.0265 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74.6148 | 74.6148 | 200.0639 | 2 | PROCESSED | 57533.2849537037 | 2016-05-25 06:50:20 | 54247 | 2007-05-27 00:00:00 | 54056.4806828704 | 2006-11-17 11:32:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000043 | We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ? | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | JAP | 0 | SWG | VICINITY OF LMC X-3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500031010/ | Quick Look | ![]() |
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88 | 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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89 | 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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90 | 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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91 | 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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92 | 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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93 | 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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94 | 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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95 | 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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96 | 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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97 | 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 | ![]() |
98 | 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 | ![]() |
99 | 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 | ![]() |
100 | 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 | ![]() |
101 | 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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102 | 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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103 | 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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104 | 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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105 | 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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106 | 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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107 | 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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108 | 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 | ![]() |
109 | 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 | ![]() |
110 | 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 | ![]() |
111 | GC18 | 266.183 | -28.6222 | 265.39077 | -28.601742 | 266.626489 | -5.225763 | 0.16630142 | 0.32982124 | 260.5302 | 54384.4819560185 | 2007-10-11 11:34:01 | 54384.9633564815 | 2007-10-11 23:07:14 | 502006010 | 22.6311 | 20 | 22.6311 | 22.6413 | 0 | 22.6351 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.6702 | 21.6702 | 41.5841 | 1 | PROCESSED | 57540.2503356482 | 2016-06-01 06:00:29 | 54771 | 2008-11-01 00:00:00 | 54402.6632291667 | 2007-10-29 15:55:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502006010/ | Quick Look | ![]() |
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112 | GC21 | 267.484 | -27.3686 | 266.699338 | -27.354471 | 267.750913 | -3.947195 | 1.83363899 | -0.00346152 | 261.5433 | 54385.9113888889 | 2007-10-12 21:52:24 | 54386.3127199074 | 2007-10-13 07:30:19 | 502009010 | 20.8615 | 20 | 20.8615 | 20.8615 | 0 | 20.8615 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.6483 | 19.6483 | 34.6639 | 1 | PROCESSED | 57540.2599189815 | 2016-06-01 06:14:17 | 54771 | 2008-11-01 00:00:00 | 54402.5769444444 | 2007-10-29 13:50:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502009010/ | Quick Look | ![]() |
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113 | GC22 | 266.3806 | -28.337 | 265.590118 | -28.317504 | 266.793387 | -4.936169 | 0.50023196 | 0.3305092 | 262.5049 | 54386.3138888889 | 2007-10-13 07:32:00 | 54386.785 | 2007-10-13 18:50:24 | 502010010 | 21.6214 | 20 | 21.6214 | 21.6214 | 0 | 21.6214 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1944 | 21.1944 | 40.662 | 1 | PROCESSED | 57540.2655439815 | 2016-06-01 06:22:23 | 54771 | 2008-11-01 00:00:00 | 54402.6900231482 | 2007-10-29 16:33:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502010010/ | Quick Look | ![]() |
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114 | HESS J1745-303 3 | 266.0567 | -30.2413 | 265.254155 | -30.220204 | 266.559978 | -6.847208 | 358.72882707 | -0.42335991 | 69.0003 | 54533.6682523148 | 2008-03-08 16:02:17 | 54535.8752199074 | 2008-03-10 21:00:19 | 502018010 | 79.0162 | 67 | 79.0162 | 79.0402 | 0 | 79.0242 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.201 | 70.201 | 190.658 | 2 | PROCESSED | 57541.8566898148 | 2016-06-02 20:33:38 | 54919 | 2009-03-29 00:00:00 | 54550.3420601852 | 2008-03-25 08:12:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502018010/ | Quick Look | ![]() |
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115 | VELA JR P7 | 133.7759 | -45.5828 | 133.340558 | -45.390922 | 159.660843 | -58.904253 | 266.02998701 | -0.32446592 | 347.0033 | 54286.9870023148 | 2007-07-05 23:41:17 | 54287.3023032407 | 2007-07-06 07:15:19 | 502029010 | 14.5838 | 10 | 14.5838 | 14.5838 | 0 | 14.5838 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.605 | 12.605 | 27.2399 | 0 | PROCESSED | 57539.1100810185 | 2016-05-31 02:38:31 | 54696 | 2008-08-18 00:00:00 | 54328.4686111111 | 2007-08-16 11:14:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502029010/ | Quick Look | ![]() |
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116 | VELA JR P10 | 132.9993 | -45.7656 | 132.567919 | -45.576468 | 158.955645 | -59.347984 | 265.8217159 | -0.85784968 | 347.0018 | 54287.9522337963 | 2007-07-06 22:51:13 | 54288.2308564815 | 2007-07-07 05:32:26 | 502032010 | 13.04 | 10 | 13.048 | 13.04 | 0 | 13.056 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6988 | 10.6988 | 24.0679 | 0 | PROCESSED | 57539.1146527778 | 2016-05-31 02:45:06 | 54703 | 2008-08-25 00:00:00 | 54333.4328240741 | 2007-08-21 10:23:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502032010/ | Quick Look | ![]() |
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117 | VELA JR P14 | 131.9312 | -46.3861 | 131.508056 | -46.200795 | 158.369308 | -60.268301 | 265.83284327 | -1.824218 | 347.0017 | 54290.4416087963 | 2007-07-09 10:35:55 | 54290.675150463 | 2007-07-09 16:12:13 | 502036010 | 11.034 | 10 | 11.034 | 11.042 | 0 | 11.042 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.1391 | 11.1391 | 20.1679 | 0 | PROCESSED | 57539.1311226852 | 2016-05-31 03:08:49 | 54696 | 2008-08-18 00:00:00 | 54328.4740277778 | 2007-08-16 11:22:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502036010/ | Quick Look | ![]() |
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118 | VELA JR P15 | 132.3334 | -46.3288 | 131.908455 | -46.142044 | 158.77835 | -60.071 | 265.96324441 | -1.57253381 | 347.0016 | 54291.1946064815 | 2007-07-10 04:40:14 | 54291.46 | 2007-07-10 11:02:24 | 502037010 | 8.876 | 10 | 8.876 | 8.876 | 0 | 8.876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.3411 | 7.3411 | 22.9121 | 1 | PROCESSED | 57539.1396990741 | 2016-05-31 03:21:10 | 54696 | 2008-08-18 00:00:00 | 54328.472962963 | 2007-08-16 11:21:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502037010/ | Quick Look | ![]() |
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119 | 47 TUCANAE | 6.2112 | -71.9961 | 5.659821 | -72.273106 | 311.457534 | -62.358991 | 305.8317488 | -44.9821189 | 65.5967 | 54261.1765162037 | 2007-06-10 04:14:11 | 54263.5404976852 | 2007-06-12 12:58:19 | 502048010 | 132.1052 | 133 | 132.1452 | 132.1052 | 0 | 132.1372 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.9042 | 132.9042 | 204.2319 | 1 | PROCESSED | 57538.9491666667 | 2016-05-30 22:46:48 | 54745 | 2008-10-06 00:00:00 | 54271.5258796296 | 2007-06-20 12:37:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020066 | We propose a 100 ks observation of the globular cluster 47 Tuc. An extended (~2') hard x-ray emission, presumably of non-thermal origin, was detected with Chandra from a position ~6' toward north east of its center. However, the Chandra ACIS spectrum does not allow us to determine with confidence whether it is a non-thermal emission or a high temperature thermal source. Utilizing the high sensitivity of the XIS, we try to distinguish between these two cases. If confirmed, the result may provide valuable information on particle acceleration in non-relativistic shocks, with potential relations the galactic-ridge x-ray emission. We perform a single pointing observation placing the center of the diffuse emission onto XIS nominal position. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAYUKI YUASA | JAP | 2 | AO2 | OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502048010/ | Quick Look | ![]() |
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120 | M17 EAST BKG | 275.6441 | -15.5803 | 274.925967 | -15.60595 | 275.476675 | 7.75309 | 15.81995827 | -0.84785909 | 271.9998 | 54380.0947800926 | 2007-10-07 02:16:29 | 54381.7571064815 | 2007-10-08 18:10:14 | 502053010 | 71.494 | 67 | 71.494 | 71.5085 | 0 | 71.502 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62.5549 | 62.5549 | 143.61 | 1 | PROCESSED | 57540.2032175926 | 2016-06-01 04:52:38 | 54771 | 2008-11-01 00:00:00 | 54403.2344791667 | 2007-10-30 05:37:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020085 | We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAHIRO TSUJIMOTO | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502053010/ | Quick Look | ![]() |
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121 | GALACTIC BULGE | 268.3774 | -29.9651 | 267.576244 | -29.955267 | 268.575567 | -6.53206 | 359.99980668 | -2.0020922 | 279.4328 | 54372.0700347222 | 2007-09-29 01:40:51 | 54375.590462963 | 2007-10-02 14:10:16 | 502059010 | 136.824 | 133 | 136.824 | 136.824 | 0 | 136.824 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.5156 | 110.5156 | 304.1306 | 2 | PROCESSED | 57540.2260185185 | 2016-06-01 05:25:28 | 54770 | 2008-10-31 00:00:00 | 54402.653275463 | 2007-10-29 15:40:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020118 | We propose a 100 ks observation on the Galactic Bulge (b=-2.0) with Suzaku. The origin of thermal diffuse X-ray emission will be for the first time clarified with a fine spectroscopy with Suzaku XIS, especially from the Fe-K line analysis. The non-thermal emission from the Galactic Bulge will be also investigated with HXD-PIN. | GALACTIC DIFFUSE EMISSION | 5 | A | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502059010/ | Quick Look | ![]() |
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122 | COMET_8P_TUTTLE-P1-9 | 28.3593 | 5.9969 | 27.705197 | 5.751157 | 28.487543 | -5.283181 | 149.56477648 | -53.63811023 | 248.4989 | 54471.0491666667 | 2008-01-06 01:10:48 | 54471.1154050926 | 2008-01-06 02:46:11 | 502062090 | 3.2186 | 3.2 | 3.2186 | 3.2186 | 0 | 3.2186 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.439 | 2.439 | 5.664 | 0 | PROCESSED | 57541.0088425926 | 2016-06-02 00:12:44 | 54908 | 2009-03-18 00:00:00 | 54542.2348611111 | 2008-03-17 05:38:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062090/ | Quick Look | ![]() |
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123 | COMET_8P_TUTTLE-P1-11 | 28.4619 | 5.5053 | 27.808889 | 5.259792 | 28.409931 | -5.779338 | 150.05998726 | -54.04643055 | 248.5015 | 54471.1825 | 2008-01-06 04:22:48 | 54471.2487384259 | 2008-01-06 05:58:11 | 502062110 | 3.219 | 3.2 | 3.219 | 3.219 | 0 | 3.219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.0356 | 2.0356 | 5.688 | 0 | PROCESSED | 57541.2689699074 | 2016-06-02 06:27:19 | 54908 | 2009-03-18 00:00:00 | 54542.2871990741 | 2008-03-17 06:53:34 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062110/ | Quick Look | ![]() |
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124 | COMET_8P_TUTTLE-P1-12 | 28.5143 | 5.2526 | 27.861852 | 5.007213 | 28.369731 | -6.034275 | 150.31791041 | -54.25562458 | 248.4993 | 54471.2491666667 | 2008-01-06 05:58:48 | 54471.3154050926 | 2008-01-06 07:34:11 | 502062120 | 3.2196 | 3.2 | 3.2196 | 3.2196 | 0 | 3.2196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.162 | 2.162 | 5.696 | 0 | PROCESSED | 57541.268587963 | 2016-06-02 06:26:46 | 54908 | 2009-03-18 00:00:00 | 54542.261400463 | 2008-03-17 06:16:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062120/ | Quick Look | ![]() |
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125 | COMET_8P_TUTTLE-P2_03 | 39.7649 | -35.9737 | 39.253357 | -36.188553 | 21.195094 | -48.151161 | 240.80897167 | -65.5250468 | 257.7596 | 54490.2964351852 | 2008-01-25 07:06:52 | 54490.4293287037 | 2008-01-25 10:18:14 | 502063030 | 6.0389 | 6 | 6.0549 | 6.0389 | 0 | 6.0549 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.6011 | 6.6011 | 11.4639 | 0 | PROCESSED | 57541.3810532407 | 2016-06-02 09:08:43 | 54912 | 2009-03-22 00:00:00 | 54546.1040046296 | 2008-03-21 02:29:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063030/ | Quick Look | ![]() |
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126 | COMET_8P_TUTTLE-P2_04 | 39.8249 | -36.1145 | 39.31419 | -36.329166 | 21.162848 | -48.298537 | 241.11100541 | -65.44459708 | 257.8515 | 54490.4297106482 | 2008-01-25 10:18:47 | 54490.562662037 | 2008-01-25 13:30:14 | 502063040 | 6.6876 | 6.7 | 6.6876 | 6.7191 | 0 | 6.6876 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.3887 | 7.3887 | 11.4799 | 0 | PROCESSED | 57541.3859375 | 2016-06-02 09:15:45 | 54912 | 2009-03-22 00:00:00 | 54546.1129513889 | 2008-03-21 02:42:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063040/ | Quick Look | ![]() |
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127 | COMET_8P_TUTTLE-P2_05 | 39.8852 | -36.2545 | 39.375324 | -36.468978 | 21.131041 | -48.445251 | 241.40935004 | -65.36366996 | 257.9439 | 54490.5630439815 | 2008-01-25 13:30:47 | 54490.6959953704 | 2008-01-25 16:42:14 | 502063050 | 6.6974 | 6.7 | 6.6976 | 6.6976 | 0 | 6.6974 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.1619 | 6.1619 | 11.4799 | 0 | PROCESSED | 57541.3887847222 | 2016-06-02 09:19:51 | 54912 | 2009-03-22 00:00:00 | 54546.126712963 | 2008-03-21 03:02:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063050/ | Quick Look | ![]() |
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128 | COMET_8P_TUTTLE-P2_10 | 40.1849 | -36.9375 | 39.679167 | -37.15104 | 20.975454 | -49.162155 | 242.83840601 | -64.95862507 | 253.4045 | 54491.2297106482 | 2008-01-26 05:30:47 | 54491.362662037 | 2008-01-26 08:42:14 | 502063100 | 5.7304 | 5 | 5.7384 | 5.7384 | 0 | 5.7304 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.2091 | 6.2091 | 11.4739 | 0 | PROCESSED | 57541.4028472222 | 2016-06-02 09:40:06 | 54912 | 2009-03-22 00:00:00 | 54546.1949884259 | 2008-03-21 04:40:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063100/ | Quick Look | ![]() |
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129 | COMET_8P_TUTTLE-P2_12 | 40.3045 | -37.2045 | 39.80042 | -37.417664 | 20.914316 | -49.442898 | 243.38522043 | -64.79583615 | 253.5926 | 54491.4963773148 | 2008-01-26 11:54:47 | 54491.6293287037 | 2008-01-26 15:06:14 | 502063120 | 6.6082 | 6.7 | 6.6082 | 6.6082 | 0 | 6.6242 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.4698 | 6.4698 | 11.4799 | 0 | PROCESSED | 57541.4099884259 | 2016-06-02 09:50:23 | 54912 | 2009-03-22 00:00:00 | 54546.2619675926 | 2008-03-21 06:17:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063120/ | Quick Look | ![]() |
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130 | COMET_8P_TUTTLE-P2_14 | 40.423 | -37.4668 | 39.920562 | -37.679591 | 20.853678 | -49.718838 | 243.91615364 | -64.63380941 | 253.7796 | 54491.7630439815 | 2008-01-26 18:18:47 | 54491.8959953704 | 2008-01-26 21:30:14 | 502063140 | 6.5627 | 6.7 | 6.5627 | 6.5867 | 0 | 6.5627 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.833 | 3.833 | 11.4799 | 0 | PROCESSED | 57541.4134143518 | 2016-06-02 09:55:19 | 54912 | 2009-03-22 00:00:00 | 54546.2568518518 | 2008-03-21 06:09:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063140/ | Quick Look | ![]() |
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131 | COMET_8P_TUTTLE-P2_15 | 40.4836 | -37.5961 | 39.981983 | -37.8087 | 20.825541 | -49.855587 | 244.17467378 | -64.55180166 | 253.8725 | 54491.8963773148 | 2008-01-26 21:30:47 | 54492.0293287037 | 2008-01-27 00:42:14 | 502063150 | 3.4717 | 4 | 3.4797 | 3.4717 | 0 | 3.4877 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.3461 | 2.3461 | 11.4799 | 1 | PROCESSED | 57541.4238657407 | 2016-06-02 10:10:22 | 54912 | 2009-03-22 00:00:00 | 54546.2153587963 | 2008-03-21 05:10:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063150/ | Quick Look | ![]() |
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132 | G332.5-5.6 CENTER | 250.7335 | -54.5135 | 249.725841 | -54.419293 | 256.94436 | -31.940577 | 332.53119736 | -5.54004522 | 262.5079 | 54330.694224537 | 2007-08-18 16:39:41 | 54331.8731944444 | 2007-08-19 20:57:24 | 502066010 | 70.1488 | 80 | 70.1488 | 70.1488 | 0 | 70.1568 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 71.4907 | 71.4907 | 101.8399 | 0 | PROCESSED | 57539.62875 | 2016-05-31 15:05:24 | 54721 | 2008-09-12 00:00:00 | 54354.4910300926 | 2007-09-11 11:47:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | STEPHEN REYNOLDS | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502066010/ | Quick Look | ![]() |
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133 | KEPLER | 262.6698 | -21.4886 | 261.920525 | -21.451271 | 263.169114 | 1.778808 | 4.51918955 | 6.82146946 | 98.2145 | 54514.1665393518 | 2008-02-18 03:59:49 | 54516.9793287037 | 2008-02-20 23:30:14 | 502078010 | 116.9636 | 100 | 116.9636 | 116.9636 | 0 | 116.9636 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.9551 | 98.9551 | 242.9956 | 3 | PROCESSED | 57541.7751388889 | 2016-06-02 18:36:12 | 54894 | 2009-03-04 00:00:00 | 54525.6176851852 | 2008-02-29 14:49:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023074 | We propose to observe the Kepler's SNR in which evidence of particle acceleration will be found. Aim of the observation is to determine power-law contribution in the hard-tail spectrum above 10 keV with HXD-PIN. If we also find the Fe-Kb and Ni-K emission lines with XIS which have not observed in any previous missions, temperature and nt parameter of a NEI model will be fixed. The determination will help to distinguish the power-law component from the thermal one. We also memtioned that the amount of Fe and Ni will be a good estimator to determine the type of Kepler's SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | TORU TAMAGAWA | Sangwook Park | JUS | 2 | AO2 | SEARCH FOR EVIDENCE OF COSMIC-RAY ACCELERATION IN THE KEPLER'S SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502078010/ | Quick Look | ![]() |
134 | ANTICENTER2 | 12.9862 | 62.9112 | 12.227424 | 62.639587 | 45.279185 | 50.910305 | 122.98962226 | 0.03950805 | 69.9598 | 54679.0120717593 | 2008-08-01 00:17:23 | 54680.8411921296 | 2008-08-02 20:11:19 | 503006010 | 86.1101 | 80 | 86.123 | 86.123 | 0 | 86.1101 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.785 | 106.785 | 158.0198 | 1 | PROCESSED | 57543.2173726852 | 2016-06-04 05:13:01 | 55070 | 2009-08-27 00:00:00 | 54693.3237847222 | 2008-08-15 07:46:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030020 | We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. The ROSAT 3/4 keV band all sky map does not show significant dip in intensity at galactic plane, where the CXB component is totally absorbed by galactic absorption. Thus unknown emission must be compensating the CXB component in this energy band. Our AO-2 observation of a general direction of the anticenter direction gives a clear clue to understand the origin of the mysterious emission. We propose to make additional observation in order to confirm the emission component detected in the AO-2 observation generally exist in the galactic plane. | GALACTIC DIFFUSE EMISSION | 5 | B | KENSUKE MASUI | JAP | 3 | AO3 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503006010/ | Quick Look | ![]() |
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135 | GC_LARGEPROJECT2 | 266.7785 | -29.1292 | 265.982946 | -29.111621 | 267.162656 | -5.719811 | 0.00479668 | -0.37932142 | 260.8763 | 54712.9538078704 | 2008-09-03 22:53:29 | 54714.2891087963 | 2008-09-05 06:56:19 | 503008010 | 53.6388 | 50 | 53.6548 | 53.6388 | 0 | 53.6548 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8111 | 42.8111 | 115.3338 | 0 | PROCESSED | 57543.7762615741 | 2016-06-04 18:37:49 | 54557 | 2008-04-01 00:00:00 | 54780.4880092593 | 2008-11-10 11:42:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503008010/ | Quick Look | ![]() |
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136 | GC_LARGEPROJECT3 | 266.4525 | -29.3384 | 265.655678 | -29.319237 | 266.881748 | -5.935661 | 359.67825031 | -0.24492188 | 260.8779 | 54714.2896759259 | 2008-09-05 06:57:08 | 54715.6634722222 | 2008-09-06 15:55:24 | 503009010 | 52.3975 | 50 | 52.4055 | 52.3975 | 0 | 52.4114 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2691 | 40.2691 | 118.6778 | 2 | PROCESSED | 57543.769375 | 2016-06-04 18:27:54 | 54557 | 2008-04-01 00:00:00 | 54780.6767476852 | 2008-11-10 16:14:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503009010/ | Quick Look | ![]() |
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137 | GC_LARGEPROJECT5 | 265.9469 | -29.8331 | 265.147019 | -29.811478 | 266.45285 | -6.44183 | 359.02671432 | -0.12852462 | 265.43 | 54717.3806597222 | 2008-09-08 09:08:09 | 54718.8981365741 | 2008-09-09 21:33:19 | 503011010 | 57.6334 | 50 | 57.6334 | 57.6334 | 0 | 57.6334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1555 | 40.1555 | 131.0998 | 1 | PROCESSED | 57543.8408449074 | 2016-06-04 20:10:49 | 54557 | 2008-04-01 00:00:00 | 54780.6683912037 | 2008-11-10 16:02:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503011010/ | Quick Look | ![]() |
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138 | GC_LARGEPROJECT9 | 265.0297 | -30.9626 | 264.222709 | -30.936519 | 265.692051 | -7.595667 | 357.64981902 | -0.05267713 | 269.1132 | 54728.3146412037 | 2008-09-19 07:33:05 | 54729.4140393518 | 2008-09-20 09:56:13 | 503015010 | 56.7716 | 50 | 56.7796 | 56.7716 | 0 | 56.7876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.8454 | 52.8454 | 94.9759 | 0 | PROCESSED | 57543.8851041667 | 2016-06-04 21:14:33 | 54557 | 2008-04-01 00:00:00 | 54780.4933564815 | 2008-11-10 11:50:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503015010/ | Quick Look | ![]() |
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139 | GC_LARGEPROJECT12 | 264.5606 | -31.5967 | 263.749555 | -31.56834 | 265.310874 | -8.24393 | 356.89961278 | -0.05143068 | 268.4538 | 54742.7536226852 | 2008-10-03 18:05:13 | 54743.154375 | 2008-10-04 03:42:18 | 503018020 | 12.2466 | 10 | 12.2466 | 12.2466 | 0 | 12.2466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.232 | 10.232 | 34.6179 | 1 | PROCESSED | 57544.0096527778 | 2016-06-05 00:13:54 | 54557 | 2008-04-01 00:00:00 | 54780.5624652778 | 2008-11-10 13:29:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018020/ | Quick Look | ![]() |
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140 | HESS J1825-137 | 276.5024 | -13.9965 | 275.79256 | -14.02632 | 276.383198 | 9.300131 | 17.60816681 | -0.84042551 | 271.0002 | 54754.9096064815 | 2008-10-15 21:49:50 | 54756.458599537 | 2008-10-17 11:00:23 | 503028010 | 57.2104 | 50 | 57.2104 | 57.2104 | 0 | 57.2104 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.5485 | 51.5485 | 133.7938 | 1 | PROCESSED | 57544.1955324074 | 2016-06-05 04:41:34 | 55148 | 2009-11-13 00:00:00 | 54780.7053703704 | 2008-11-10 16:55:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAAKI TANAKA | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503028010/ | Quick Look | ![]() |
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141 | VELA JR P24 | 132.0303 | -46.6729 | 131.609003 | -46.487232 | 158.79782 | -60.473277 | 266.0989339 | -1.95139979 | 347.001 | 54652.7719328704 | 2008-07-05 18:31:35 | 54653.1668865741 | 2008-07-06 04:00:19 | 503036010 | 12.3735 | 10 | 12.3735 | 12.3735 | 0 | 12.3735 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2548 | 12.2548 | 34.12 | 1 | PROCESSED | 57542.9791203704 | 2016-06-03 23:29:56 | 55048 | 2009-08-05 00:00:00 | 54679.3185763889 | 2008-08-01 07:38:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503036010/ | Quick Look | ![]() |
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142 | VELA JR P28 | 133.7109 | -46.6037 | 133.283226 | -46.412037 | 160.667114 | -59.788002 | 266.78076878 | -1.01777641 | 347.0004 | 54654.1674537037 | 2008-07-07 04:01:08 | 54654.4259143518 | 2008-07-07 10:13:19 | 503040010 | 13.093 | 10 | 13.101 | 13.093 | 0 | 13.101 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.054 | 12.054 | 22.296 | 0 | PROCESSED | 57542.9904282407 | 2016-06-03 23:46:13 | 55048 | 2009-08-05 00:00:00 | 54679.3674421296 | 2008-08-01 08:49:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503040010/ | Quick Look | ![]() |
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143 | VELA JR P29 | 134.0711 | -46.43 | 133.640871 | -46.237075 | 160.890422 | -59.507166 | 266.80859879 | -0.71638658 | 347 | 54654.4264814815 | 2008-07-07 10:14:08 | 54654.7203703704 | 2008-07-07 17:17:20 | 503041010 | 11.3685 | 10 | 11.3802 | 11.3685 | 0 | 11.3802 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.2225 | 8.2225 | 25.3679 | 0 | PROCESSED | 57542.9909606482 | 2016-06-03 23:46:59 | 55048 | 2009-08-05 00:00:00 | 54679.3958217593 | 2008-08-01 09:29:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503041010/ | Quick Look | ![]() |
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144 | VELA JR P38 | 132.2003 | -47.2308 | 131.782721 | -47.04451 | 159.617188 | -60.877835 | 266.60579829 | -2.21244802 | 347.0003 | 54657.2423958333 | 2008-07-10 05:49:03 | 54657.5209953704 | 2008-07-10 12:30:14 | 503050010 | 14.0436 | 10 | 14.0436 | 14.0436 | 0 | 14.0596 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.426 | 11.426 | 24.0639 | 0 | PROCESSED | 57543.0197800926 | 2016-06-04 00:28:29 | 55037 | 2009-07-25 00:00:00 | 54670.2561111111 | 2008-07-23 06:08:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503050010/ | Quick Look | ![]() |
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145 | RCW 38 | 134.7638 | -47.5154 | 134.339139 | -47.320051 | 162.870038 | -60.148721 | 267.93999829 | -1.06526988 | 109.8553 | 54788.5064351852 | 2008-11-18 12:09:16 | 54790.699525463 | 2008-11-20 16:47:19 | 503054010 | 81.5377 | 80 | 81.5495 | 81.5377 | 0 | 81.5415 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.9281 | 60.9281 | 189.4597 | 1 | PROCESSED | 57544.5092013889 | 2016-06-05 12:13:15 | 55171 | 2009-12-06 00:00:00 | 54811.741099537 | 2008-12-11 17:47:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030069 | We propose to make Suzaku observation of HII region RCW 38 for 80 ksec in order to study non-thermal phenomena in a massive star-forming region. The region is thought to be a site of high energy particle acceleration by interaction of strong stellar wind from high-mass stars. The main purpose is to observe extended emission from RCW 38. The high resolution spectroscopy by XIS enables us to distinguish non-thermal emission from thermal component and to obtain properties of non-thermal component. In addition, HXD will detect non-thermal radiation from RCW 38. | GALACTIC DIFFUSE EMISSION | 5 | C | HIROKAZU ODAKA | JAP | 3 | AO3 | SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503054010/ | Quick Look | ![]() |
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146 | CYGNUS LOOP (P21) | 313.196 | 32.4197 | 312.684204 | 32.23006 | 328.688835 | 47.452326 | 75.60030214 | -7.75821821 | 61.9243 | 54619.9401967593 | 2008-06-02 22:33:53 | 54620.2975 | 2008-06-03 07:08:24 | 503057010 | 16.1703 | 15 | 16.1783 | 16.1703 | 0 | 16.1783 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.8903 | 12.8903 | 30.8639 | 0 | PROCESSED | 57542.700474537 | 2016-06-03 16:48:41 | 55003 | 2009-06-21 00:00:00 | 54636.2238078704 | 2008-06-19 05:22:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503057010/ | Quick Look | ![]() |
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147 | RABBIT | 214.6544 | -60.9713 | 213.733054 | -60.740946 | 236.398817 | -43.82174 | 313.31134091 | 0.131367 | 105.7763 | 54876.850787037 | 2009-02-14 20:25:08 | 54877.5224421296 | 2009-02-15 12:32:19 | 503071010 | 21.274 | 20 | 21.282 | 21.274 | 0 | 21.29 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.0126 | 18.0126 | 57.984 | 0 | PROCESSED | 57545.5405439815 | 2016-06-06 12:58:23 | 55330 | 2010-05-14 00:00:00 | 54892.945162037 | 2009-03-02 22:41:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030076 | K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. | GALACTIC DIFFUSE EMISSION | 5 | C | TETSUICHI KISHISHITA | JAP | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503071010/ | Quick Look | ![]() |
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148 | HESS_J1809-193_N | 272.4044 | -19.3551 | 271.665869 | -19.36499 | 272.264534 | 4.066746 | 11.02929838 | 0.07166066 | 112.001 | 54556.5874421296 | 2008-03-31 14:05:55 | 54557.6877662037 | 2008-04-01 16:30:23 | 503078010 | 51.5309 | 40 | 51.5389 | 51.5309 | 0 | 51.5461 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8186 | 34.8186 | 95.0518 | 2 | PROCESSED | 57542.0290740741 | 2016-06-03 00:41:52 | 54950 | 2009-04-29 00:00:00 | 54571.3638888889 | 2008-04-15 08:44:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030126 | A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAYASU ANADA | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503078010/ | Quick Look | ![]() |
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149 | VICINITY_OF_PKS_2155-1 | 329.2367 | -30.5281 | 328.510685 | -30.766467 | 320.669664 | -16.905257 | 17.16872193 | -51.86657338 | 55.8337 | 54585.7726736111 | 2008-04-29 18:32:39 | 54588.3542592593 | 2008-05-02 08:30:08 | 503082010 | 90.1812 | 80 | 90.1812 | 90.1812 | 0 | 90.1812 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.7921 | 76.7921 | 223.0237 | 4 | PROCESSED | 57542.4840277778 | 2016-06-03 11:37:00 | 54975 | 2009-05-24 00:00:00 | 54608.3373726852 | 2008-05-22 08:05:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030135 | The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | A | TOSHISHIGE HAGIHARA | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503082010/ | Quick Look | ![]() |
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150 | B1920+10(1) | 293.0298 | 10.9618 | 292.438521 | 10.854204 | 297.004439 | 32.268855 | 47.34140504 | -3.87470613 | 252.2888 | 54772.350462963 | 2008-11-02 08:24:40 | 54774.137662037 | 2008-11-04 03:18:14 | 503090010 | 73.6033 | 70 | 73.6124 | 73.6033 | 0 | 73.6113 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66.6682 | 66.6682 | 154.4039 | 3 | PROCESSED | 57544.3491550926 | 2016-06-05 08:22:47 | 55154 | 2009-11-19 00:00:00 | 54788.4472337963 | 2008-11-18 10:44:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | ZDENKA MISANOVIC | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503090010/ | Quick Look | ![]() |
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151 | HESS J1023-575 | 155.5616 | -57.7533 | 155.104313 | -57.500238 | 195.408014 | -59.737737 | 284.06754503 | -0.45248582 | 284.3289 | 54617.1411458333 | 2008-05-31 03:23:15 | 54617.4515509259 | 2008-05-31 10:50:14 | 503092010 | 13.826 | 10 | 13.826 | 13.826 | 0 | 13.826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0573 | 11.0573 | 26.8159 | 1 | PROCESSED | 57542.6773842593 | 2016-06-03 16:15:26 | 54999 | 2009-06-17 00:00:00 | 54633.6961458333 | 2008-06-16 16:42:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031207 | We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts. | GALACTIC DIFFUSE EMISSION | 5 | B | MALLORY ROBERTS | USA | 3 | AO3 | SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503092010/ | Quick Look | ![]() |
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152 | GCL2 | 264.8888 | -28.9255 | 264.094972 | -28.898771 | 265.497098 | -5.564174 | 359.31035513 | 1.13376438 | 106.9569 | 54905.2789467593 | 2009-03-15 06:41:41 | 54905.9169444444 | 2009-03-15 22:00:24 | 503100010 | 25.7179 | 25 | 25.7179 | 25.7179 | 0 | 25.7179 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.146 | 24.146 | 55.1199 | 1 | PROCESSED | 57545.8116666667 | 2016-06-06 19:28:48 | 55329 | 2010-05-13 00:00:00 | 54917.3744675926 | 2009-03-27 08:59:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503100010/ | Quick Look | ![]() |
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153 | GCL3 | 265.2728 | -28.8569 | 264.479303 | -28.83203 | 265.832305 | -5.484097 | 359.5469331 | 0.88519 | 106.9023 | 54906.6133912037 | 2009-03-16 14:43:17 | 54907.3252777778 | 2009-03-17 07:48:24 | 503101010 | 33.8911 | 25 | 33.8991 | 33.8991 | 0 | 33.8911 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8309 | 30.8309 | 61.4979 | 0 | PROCESSED | 57545.8349652778 | 2016-06-06 20:02:21 | 55329 | 2010-05-13 00:00:00 | 54917.3115393518 | 2009-03-27 07:28:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503101010/ | Quick Look | ![]() |
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154 | K3/PSR J1420-6048 | 215.0274 | -60.7627 | 214.105774 | -60.533369 | 236.492647 | -43.553641 | 313.55205119 | 0.26755801 | 90.771 | 54842.5598263889 | 2009-01-11 13:26:09 | 54843.8801388889 | 2009-01-12 21:07:24 | 503110010 | 50.269 | 50 | 50.269 | 50.269 | 0 | 50.269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 50.0618 | 50.0618 | 114.0639 | 2 | PROCESSED | 57545.1792013889 | 2016-06-06 04:18:03 | 55328 | 2010-05-12 00:00:00 | 54854.3728703704 | 2009-01-23 08:56:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 033076 | K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. | GALACTIC DIFFUSE EMISSION | 5 | C | TETSUICHI KISHISHITA | ROGER ROMANI | JUS | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503110010/ | Quick Look | ![]() |
155 | SGR_B2 | 266.8788 | -28.4436 | 266.087557 | -28.426518 | 267.23571 | -5.032452 | 0.63679 | -0.09938091 | 266.4718 | 55096.836412037 | 2009-09-22 20:04:26 | 55102.6667592593 | 2009-09-28 16:00:08 | 504004020 | 202.0945 | 200 | 202.0945 | 202.1025 | 0 | 202.0945 | 3 | 4 | 0 | 3 | 1 | 0 | 0 | 178.2831 | 178.2831 | 303.5437 | 4 | PROCESSED | 57548.82125 | 2016-06-09 19:42:36 | 55500 | 2010-10-31 00:00:00 | 55133.4505092593 | 2009-10-29 10:48:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040002 | The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004020/ | Quick Look | ![]() |
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156 | BLOWOUT1 | 312.2225 | 31.7347 | 311.709294 | 31.548551 | 327.170903 | 47.151978 | 74.53998499 | -7.54540267 | 244.0864 | 55158.2754166667 | 2009-11-23 06:36:36 | 55158.9655555556 | 2009-11-23 23:10:24 | 504011010 | 24.1854 | 23 | 24.2014 | 24.1854 | 0 | 24.1934 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4768 | 19.4768 | 59.6039 | 1 | PROCESSED | 57549.5243055556 | 2016-06-10 12:35:00 | 55545 | 2010-12-15 00:00:00 | 55176.2112731482 | 2009-12-11 05:04:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504011010/ | Quick Look | ![]() |
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157 | BLOWOUT3 | 311.7021 | 31.3134 | 311.187829 | 31.12914 | 326.330215 | 46.937186 | 73.92913651 | -7.4588166 | 242.4356 | 55160.1363888889 | 2009-11-25 03:16:24 | 55160.4723611111 | 2009-11-25 11:20:12 | 504013010 | 16.1599 | 16 | 16.1599 | 16.1599 | 0 | 16.1599 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.8101 | 11.8101 | 29.0219 | 0 | PROCESSED | 57549.5443634259 | 2016-06-10 13:03:53 | 55545 | 2010-12-15 00:00:00 | 55176.2365740741 | 2009-12-11 05:40:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504013010/ | Quick Look | ![]() |
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158 | FESI1 | 313.4345 | 30.6099 | 312.913405 | 30.419428 | 327.914732 | 45.71047 | 74.31119672 | -9.05841998 | 226.3696 | 55182.5546180556 | 2009-12-17 13:18:39 | 55183.3334837963 | 2009-12-18 08:00:13 | 504017010 | 32.2876 | 24 | 32.2876 | 32.2876 | 0 | 32.2876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.2129 | 27.2129 | 67.2859 | 0 | PROCESSED | 57549.881099537 | 2016-06-10 21:08:47 | 55575 | 2011-01-14 00:00:00 | 55204.4679976852 | 2010-01-08 11:13:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504017010/ | Quick Look | ![]() |
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159 | HESS J1731-347 N | 262.8483 | -34.6425 | 262.016963 | -34.605825 | 263.993904 | -11.350062 | 353.56257635 | -0.49517094 | 91.6366 | 55244.8937037037 | 2010-02-17 21:26:56 | 55245.7189699074 | 2010-02-18 17:15:19 | 504032010 | 41.5263 | 40 | 41.5263 | 41.5263 | 0 | 41.5263 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.8653 | 32.8653 | 71.2719 | 0 | PROCESSED | 57550.6405555556 | 2016-06-11 15:22:24 | 55623 | 2011-03-03 00:00:00 | 55257.0108449074 | 2010-03-02 00:15:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040026 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504032010/ | Quick Look | ![]() |
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160 | GALACTICDISC3-1 | 15.309 | 67.9759 | 14.492554 | 67.706941 | 51.801719 | 54.210388 | 123.85392042 | 5.12169353 | 244.2747 | 55214.8348148148 | 2010-01-18 20:02:08 | 55216.0225 | 2010-01-20 00:32:24 | 504038010 | 55.2279 | 50 | 55.2279 | 55.2279 | 0 | 55.2279 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3329 | 43.3329 | 102.5998 | 2 | PROCESSED | 57550.2600231482 | 2016-06-11 06:14:26 | 55594 | 2011-02-02 00:00:00 | 55228.2005092593 | 2010-02-01 04:48:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040097 | To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | C | SHUNSUKE KIMURA | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504038010/ | Quick Look | ![]() |
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161 | ASO0505 | 339.5988 | 59.0734 | 339.120995 | 58.812928 | 20.160721 | 59.131044 | 106.55945745 | 0.49758229 | 62.7751 | 55001.185775463 | 2009-06-19 04:27:31 | 55001.7494675926 | 2009-06-19 17:59:14 | 504048010 | 26.3616 | 20 | 26.3696 | 26.3616 | 0 | 26.3776 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8416 | 23.8416 | 48.6959 | 1 | PROCESSED | 57547.5983449074 | 2016-06-08 14:21:37 | 55381 | 2010-07-04 00:00:00 | 55015.2523148148 | 2009-07-03 06:03:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504048010/ | Quick Look | ![]() |
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162 | ASO0418 | 279.775 | -5.7085 | 279.106672 | -5.754175 | 280.186655 | 17.387028 | 26.44714681 | 0.13153934 | 86.843 | 54934.6472800926 | 2009-04-13 15:32:05 | 54935.7578587963 | 2009-04-14 18:11:19 | 504052010 | 41.0684 | 40 | 41.0802 | 41.0844 | 0 | 41.0684 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.5258 | 33.5258 | 95.9378 | 0 | PROCESSED | 57546.1671296296 | 2016-06-07 04:00:40 | 55324 | 2010-05-08 00:00:00 | 54949.5662268518 | 2009-04-28 13:35:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504052010/ | Quick Look | ![]() |
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163 | ASO0215 | 154.6836 | -58.9426 | 154.241353 | -58.691332 | 196.521873 | -60.887637 | 284.32918046 | -1.70077172 | 314.5017 | 55019.3141782407 | 2009-07-07 07:32:25 | 55020.3404976852 | 2009-07-08 08:10:19 | 504053010 | 40.0868 | 40 | 40.0868 | 40.0868 | 0 | 40.0868 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.4782 | 35.4782 | 88.6598 | 0 | PROCESSED | 57547.8126851852 | 2016-06-08 19:30:16 | 55399 | 2010-07-22 00:00:00 | 55029.2468055556 | 2009-07-17 05:55:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504053010/ | Quick Look | ![]() |
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164 | ASO0319 | 224.8822 | -60.8823 | 223.89321 | -60.683278 | 242.498215 | -41.674426 | 317.89227503 | -1.78687667 | 277.7774 | 55049.7078125 | 2009-08-06 16:59:15 | 55051.0238425926 | 2009-08-08 00:34:20 | 504055010 | 42.3613 | 40 | 42.3613 | 42.3668 | 0 | 42.3773 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.5233 | 37.5233 | 113.6859 | 0 | PROCESSED | 57548.1027083333 | 2016-06-09 02:27:54 | 55430 | 2010-08-22 00:00:00 | 55062.2941782407 | 2009-08-19 07:03:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504055010/ | Quick Look | ![]() |
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165 | NEP #2 | 270.0521 | 66.5655 | 270.053494 | 66.565223 | 19.553337 | 89.984047 | 96.38949161 | 29.79071779 | 194.6438 | 55172.5015162037 | 2009-12-07 12:02:11 | 55173.6411342593 | 2009-12-08 15:23:14 | 504072010 | 48.6977 | 50 | 48.6977 | 48.6977 | 0 | 48.6977 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.4582 | 38.4582 | 98.456 | 1 | PROCESSED | 57549.730775463 | 2016-06-10 17:32:19 | 54922 | 2009-04-01 00:00:00 | 55190.01875 | 2009-12-25 00:27:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504072010/ | Quick Look | ![]() |
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166 | HESS J1809-193A | 273.0012 | -19.0034 | 272.264617 | -19.016192 | 272.836277 | 4.407781 | 11.60922783 | -0.25253702 | 270.0939 | 55083.2051967593 | 2009-09-09 04:55:29 | 55084.4828009259 | 2009-09-10 11:35:14 | 504077010 | 52.1109 | 50 | 52.1745 | 52.1908 | 0 | 52.1109 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 44.109 | 44.109 | 110.376 | 1 | PROCESSED | 57548.5474189815 | 2016-06-09 13:08:17 | 55475 | 2010-10-06 00:00:00 | 55109.4207638889 | 2009-10-05 10:05:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | OLEG KARGALTSEV | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504077010/ | Quick Look | ![]() |
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167 | G156.2+5.7 (S) | 74.9073 | 51.0204 | 73.935792 | 50.94566 | 79.297666 | 28.139899 | 156.85145441 | 5.28162006 | 265.6871 | 55259.9832407407 | 2010-03-04 23:35:52 | 55261.1495833333 | 2010-03-06 03:35:24 | 504080010 | 52.6413 | 50 | 52.6493 | 52.6413 | 0 | 52.6493 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6566 | 47.6566 | 100.7578 | 0 | PROCESSED | 57550.7899189815 | 2016-06-11 18:57:29 | 55689 | 2011-05-08 00:00:00 | 55323.2891666667 | 2010-05-07 06:56:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504080010/ | Quick Look | ![]() |
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168 | 330.2+1.0 | 240.2338 | -51.5878 | 239.290441 | -51.447552 | 249.060918 | -30.286354 | 330.14022152 | 0.98429318 | 285.0004 | 55081.4851273148 | 2009-09-07 11:38:35 | 55082.1453472222 | 2009-09-08 03:29:18 | 504083020 | 30.8896 | 30 | 30.8896 | 30.8896 | 0 | 30.8971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.0764 | 27.0764 | 57.0379 | 0 | PROCESSED | 57548.4451736111 | 2016-06-09 10:41:03 | 55458 | 2010-09-19 00:00:00 | 55092.1620949074 | 2009-09-18 03:53:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | GLENN ALLEN | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083020/ | Quick Look | ![]() |
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169 | NGC 6888 | 302.9954 | 38.2382 | 302.538596 | 38.087534 | 320.045193 | 56.092572 | 75.36419968 | 2.38310331 | 253.873 | 55139.4126388889 | 2009-11-04 09:54:12 | 55141.3127777778 | 2009-11-06 07:30:24 | 504085010 | 77.349 | 75 | 77.461 | 77.349 | 0 | 77.461 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 62.1002 | 62.1002 | 164.1558 | 0 | PROCESSED | 57549.1334837963 | 2016-06-10 03:12:13 | 55518 | 2010-11-18 00:00:00 | 55152.1455671296 | 2009-11-17 03:29:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041321 | Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. | GALACTIC DIFFUSE EMISSION | 5 | A | SVETOZAR ZHEKOV | USA | 4 | AO4 | X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504085010/ | Quick Look | ![]() |
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170 | MRK 421 OFFSET | 166.8026 | 37.7335 | 166.111285 | 38.004105 | 152.017379 | 29.315723 | 180.50489089 | 65.69633084 | 129.0398 | 55144.0655092593 | 2009-11-09 01:34:20 | 55145.8091087963 | 2009-11-10 19:25:07 | 504086010 | 75.2595 | 75 | 75.2675 | 75.2595 | 0 | 75.2675 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.94 | 51.94 | 150.6288 | 2 | PROCESSED | 57549.2648148148 | 2016-06-10 06:21:20 | 55542 | 2010-12-12 00:00:00 | 55176.2291319444 | 2009-12-11 05:29:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041324 | The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. | GALACTIC DIFFUSE EMISSION | 5 | B | YANGSEN YAO | USA | 4 | AO4 | A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504086010/ | Quick Look | ![]() |
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171 | KEPLER_BG_GE | 263.5357 | -20.2632 | 262.792974 | -20.230061 | 263.919291 | 3.041451 | 5.99779838 | 6.79710869 | 273.0028 | 55072.0030208333 | 2009-08-29 00:04:21 | 55072.5002662037 | 2009-08-29 12:00:23 | 504101020 | 24.7227 | 60 | 24.7467 | 24.7387 | 0 | 24.7227 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2528 | 19.2528 | 42.9559 | 0 | PROCESSED | 57548.3891550926 | 2016-06-09 09:20:23 | 54922 | 2009-04-01 00:00:00 | 55109.4155324074 | 2009-10-05 09:58:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101020/ | Quick Look | ![]() |
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172 | KEPLER_BG_GW | 261.806 | -22.7684 | 261.049806 | -22.726898 | 262.438757 | 0.457902 | 2.99933771 | 6.7960859 | 273.0885 | 55109.2984143518 | 2009-10-05 07:09:43 | 55111.1057175926 | 2009-10-07 02:32:14 | 504102010 | 65.2949 | 60 | 65.3029 | 65.2949 | 0 | 65.3029 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.7821 | 50.7821 | 156.128 | 1 | PROCESSED | 57548.8038425926 | 2016-06-09 19:17:32 | 54922 | 2009-04-01 00:00:00 | 55125.6963888889 | 2009-10-21 16:42:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504102010/ | Quick Look | ![]() |
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173 | KEPLER_BG_GS | 263.1005 | -22.949 | 262.342899 | -22.913725 | 263.639389 | 0.339875 | 3.49961978 | 5.69692486 | 272.6396 | 55107.43 | 2009-10-03 10:19:12 | 55109.2973842593 | 2009-10-05 07:08:14 | 504104010 | 67.2508 | 60 | 67.2508 | 67.2805 | 0 | 67.2748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.1585 | 53.1585 | 161.3298 | 1 | PROCESSED | 57548.7538425926 | 2016-06-09 18:05:32 | 54922 | 2009-04-01 00:00:00 | 55125.3521180556 | 2009-10-21 08:27:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504104010/ | Quick Look | ![]() |
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174 | 3C_391 | 282.3812 | -0.9417 | 281.735823 | -0.99987 | 283.351934 | 21.926784 | 31.87573789 | -0.00377867 | 261.9952 | 55491.0759722222 | 2010-10-22 01:49:24 | 55493.8224537037 | 2010-10-24 19:44:20 | 505007010 | 99.3887 | 100 | 99.4607 | 99.3887 | 0 | 99.4687 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.374 | 89.374 | 237.2779 | 2 | PROCESSED | 57553.8698032407 | 2016-06-14 20:52:31 | 55287 | 2010-04-01 00:00:00 | 55502.3356597222 | 2010-11-02 08:03:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505007010/ | Quick Look | ![]() |
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175 | CYGNUS LOOP 1 | 313.2462 | 32.1399 | 312.732912 | 31.950084 | 328.580357 | 47.179033 | 75.40840203 | -7.96786776 | 81.7816 | 55300.7096759259 | 2010-04-14 17:01:56 | 55301.0293402778 | 2010-04-15 00:42:15 | 505009010 | 15.9992 | 13 | 15.9992 | 15.9992 | 0 | 15.9992 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.242 | 12.242 | 27.612 | 0 | PROCESSED | 57551.2105787037 | 2016-06-12 05:03:14 | 55287 | 2010-04-01 00:00:00 | 55362.3098726852 | 2010-06-15 07:26:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505009010/ | Quick Look | ![]() |
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176 | CYGNUS LOOP 2 | 312.7259 | 32.1633 | 312.213805 | 31.975338 | 327.998937 | 47.37656 | 75.14683323 | -7.61088939 | 81.0273 | 55301.0300925926 | 2010-04-15 00:43:20 | 55301.2897569444 | 2010-04-15 06:57:15 | 505010010 | 12.932 | 10 | 12.932 | 12.932 | 0 | 12.932 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.924 | 11.924 | 22.4319 | 0 | PROCESSED | 57551.2143402778 | 2016-06-12 05:08:39 | 55287 | 2010-04-01 00:00:00 | 55362.2959375 | 2010-06-15 07:06:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505010010/ | Quick Look | ![]() |
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177 | CYGNUS LOOP 3 | 312.9529 | 31.9301 | 312.439181 | 31.741329 | 328.122092 | 47.08601 | 75.08571271 | -7.90709143 | 81.0389 | 55301.2902777778 | 2010-04-15 06:58:00 | 55301.6209953704 | 2010-04-15 14:54:14 | 505011010 | 13.4448 | 12 | 13.4448 | 13.4448 | 0 | 13.4448 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.427 | 10.427 | 28.5719 | 0 | PROCESSED | 57551.2233333333 | 2016-06-12 05:21:36 | 55287 | 2010-04-01 00:00:00 | 55362.3557060185 | 2010-06-15 08:32:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505011010/ | Quick Look | ![]() |
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178 | CYGNUS LOOP 10 | 314.1171 | 30.7461 | 313.595298 | 30.553225 | 328.763604 | 45.604555 | 74.79486269 | -9.42625359 | 82.0017 | 55328.2812152778 | 2010-05-12 06:44:57 | 55328.6981134259 | 2010-05-12 16:45:17 | 505018010 | 16.268 | 16 | 16.276 | 16.276 | 0 | 16.268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6551 | 12.6551 | 36.012 | 0 | PROCESSED | 57551.4785069444 | 2016-06-12 11:29:03 | 55287 | 2010-04-01 00:00:00 | 55393.3335069445 | 2010-07-16 08:00:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505018010/ | Quick Look | ![]() |
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179 | G22.0+0.0 | 277.823 | -9.7151 | 277.134886 | -9.751345 | 277.921132 | 13.510599 | 22.00005623 | 0.00370699 | 89.3658 | 55302.6023842593 | 2010-04-16 14:27:26 | 55303.7272222222 | 2010-04-17 17:27:12 | 505025010 | 50.5294 | 50 | 50.5294 | 50.5294 | 0 | 50.5294 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.6208 | 44.6208 | 97.1598 | 0 | PROCESSED | 57551.270775463 | 2016-06-12 06:29:55 | 55737 | 2011-06-25 00:00:00 | 55375.7533101852 | 2010-06-28 18:04:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050009 | ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. | GALACTIC DIFFUSE EMISSION | 5 | B | SHIGEO YAMAUCHI | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505025010/ | Quick Look | ![]() |
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180 | G37.0-0.1 | 284.8009 | 3.5813 | 284.176842 | 3.511637 | 286.494967 | 26.178305 | 37.00394757 | -0.09218404 | 68.6266 | 55303.7327893518 | 2010-04-17 17:35:13 | 55304.8814583333 | 2010-04-18 21:09:18 | 505027010 | 50.9694 | 50 | 50.9774 | 50.9774 | 0 | 50.9694 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.3361 | 45.3361 | 99.23 | 1 | PROCESSED | 57551.2689699074 | 2016-06-12 06:27:19 | 55693 | 2011-05-12 00:00:00 | 55326.2903125 | 2010-05-10 06:58:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050009 | ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. | GALACTIC DIFFUSE EMISSION | 5 | B | SHIGEO YAMAUCHI | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505027010/ | Quick Look | ![]() |
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181 | SGR_C | 266.2461 | -29.3903 | 265.44899 | -29.370135 | 266.702279 | -5.992122 | 359.54016882 | -0.1184914 | 267.0744 | 55464.5256481482 | 2010-09-25 12:36:56 | 55466.608599537 | 2010-09-27 14:36:23 | 505031010 | 99.916 | 100 | 99.9561 | 99.916 | 0 | 99.956 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 89.0712 | 89.0712 | 179.9499 | 2 | PROCESSED | 57553.5757175926 | 2016-06-14 13:49:02 | 55853 | 2011-10-19 00:00:00 | 55484.3402777778 | 2010-10-15 08:10:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050018 | The Sagittarius C Complex (Sgr C) @is composed of many giant molecular clouds (MCs) in two distinct velocity zones, indicating two separate line-of-sight positions of the MCs. Past X-ray flares of Sgr A* likely produced the FeI 6.4 keV emission in the MCs (XRN: X-ray Reflection Nebulae). In Sgr C, the XRN have been solely found in one of the velocity zones. We hence propose to find new XRN in the other velocity zone, which is possibly located at the different distance from the known XRN. With the Suzaku observation, we will determine the 3-dimensional positions of the XRN. Since the presence (or absence) of the XRN largely depends on the epoch of the Sgr A* flares and the 3-dimensional positions of the MCs, Sgr C is a "Rosetta Stone" of the origin and production of the XRN. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 5 | AO5 | THE SAGITTARIUS C COMPLEX A ROSETTA STONE OF THE PAST ACTIVITY OF SAGITTARIUS A* | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505031010/ | Quick Look | ![]() |
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182 | BLOWOUT SHELL 1 | 311.9978 | 28.9736 | 311.471635 | 28.788286 | 325.391021 | 44.676168 | 72.22846422 | -9.10440661 | 48.7676 | 55360.0953587963 | 2010-06-13 02:17:19 | 55361.2627546296 | 2010-06-14 06:18:22 | 505055010 | 52.1945 | 50 | 52.2185 | 52.1945 | 0 | 52.2185 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43.6927 | 43.6927 | 100.8559 | 1 | PROCESSED | 57552.0261226852 | 2016-06-13 00:37:37 | 55741 | 2011-06-29 00:00:00 | 55375.7594907407 | 2010-06-28 18:13:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050088 | The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYUKI UCHIDA | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505055010/ | Quick Look | ![]() |
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183 | BLOWOUT SHELL 2 | 312.2035 | 28.7297 | 311.67582 | 28.543644 | 325.497444 | 44.382569 | 72.14669544 | -9.39669734 | 48.0881 | 55361.263599537 | 2010-06-14 06:19:35 | 55362.5155439815 | 2010-06-15 12:22:23 | 505056010 | 52.0698 | 50 | 52.0698 | 52.0698 | 0 | 52.0698 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0827 | 46.0827 | 108.1558 | 1 | PROCESSED | 57552.3493634259 | 2016-06-13 08:23:05 | 55741 | 2011-06-29 00:00:00 | 55375.7627893518 | 2010-06-28 18:18:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050088 | The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYUKI UCHIDA | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505056010/ | Quick Look | ![]() |
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184 | HE FOCUSING CONE | 49.5928 | 10.9507 | 48.911727 | 10.768982 | 50.111751 | -7.072007 | 170.97872575 | -37.85410489 | 253.7002 | 55591.1307291667 | 2011-01-30 03:08:15 | 55593.7710763889 | 2011-02-01 18:30:21 | 505062010 | 100.1678 | 100 | 100.1678 | 100.1678 | 0 | 100.1678 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.7852 | 82.7852 | 228.1037 | 2 | PROCESSED | 57600.8639351852 | 2016-07-31 20:44:04 | 55973 | 2012-02-16 00:00:00 | 55607.305462963 | 2011-02-15 07:19:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050129 | We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI YOSHITAKE | JAP | 5 | AO5 | OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505062010/ | Quick Look | ![]() |
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185 | 0548-70.4 | 86.9619 | -70.4173 | 87.103378 | -70.431737 | 284.612052 | -85.985846 | 280.90214015 | -30.75163284 | 12.6051 | 55378.8779861111 | 2010-07-01 21:04:18 | 55381.6286689815 | 2010-07-04 15:05:17 | 505065010 | 103.6746 | 100 | 103.6746 | 103.6746 | 0 | 103.6746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 156.9716 | 156.9716 | 237.6358 | 1 | PROCESSED | 57552.5583912037 | 2016-06-13 13:24:05 | 55287 | 2010-04-01 00:00:00 | 55434.3854513889 | 2010-08-26 09:15:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | B | KAZIMIERZ BORKOWSKI | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505065010/ | Quick Look | ![]() |
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186 | VELA SNR CB2 | 130.2058 | -44.7742 | 129.776213 | -44.595251 | 154.639113 | -59.522265 | 263.81853128 | -1.77251278 | 293.5729 | 55318.5746412037 | 2010-05-02 13:47:29 | 55318.9238425926 | 2010-05-02 22:10:20 | 505069010 | 19.3805 | 20 | 19.4125 | 19.4045 | 0 | 19.3805 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.8298 | 18.8298 | 30.1679 | 0 | PROCESSED | 57551.3535763889 | 2016-06-12 08:29:09 | 55696 | 2011-05-15 00:00:00 | 55330.2121643518 | 2010-05-14 05:05:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505069010/ | Quick Look | ![]() |
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187 | AX J1714.1-3912 | 258.5249 | -39.1972 | 257.66219 | -39.139743 | 260.755226 | -16.122974 | 347.85266774 | -0.22742448 | 85.6964 | 55608.0538078704 | 2011-02-16 01:17:29 | 55608.9654050926 | 2011-02-16 23:10:11 | 505076010 | 32.6017 | 30 | 32.6017 | 32.6017 | 0 | 32.6017 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.3362 | 28.3362 | 78.7579 | 1 | PROCESSED | 57600.9625115741 | 2016-07-31 23:06:01 | 55988 | 2012-03-02 00:00:00 | 55621.1409027778 | 2011-03-01 03:22:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052012 | Molecular clouds are predicted to emit strong non-thermal X-rays when they are close to particle-accelerating SNRs, but this emission has not been confirmed yet. We propose to observe the non-thermal X-ray source AX J1714.1-3912 to investigate its relationship with the SNR RX J1713.7-3946. ASCA observations have shown that the hard spectrum of the source may be associated with bremsstrahlung emission from particles accelerated in the SNR and diffusing in a nearby molecular cloud. This emission has never been observed in other SNRs. However, the association of the source with the remnant is still controversial and the ASCA data do not allow us to constrain the spectral properties. We aim at verifying the association with the remnant and at investigating the physical origin of the emission. | GALACTIC DIFFUSE EMISSION | 5 | A | MARCO MICELI | EUR | 5 | AO5 | INVESTIGATING THE PHYSICAL ORIGIN OF AX J1714.1-3912 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505076010/ | Quick Look | ![]() |
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188 | GALACTIC_BULGE3 | 267.9488 | -29.7963 | 267.148788 | -29.784389 | 268.199437 | -6.368042 | 359.95634845 | -1.5962466 | 107.1729 | 55624.8013310185 | 2011-03-04 19:13:55 | 55626.2292939815 | 2011-03-06 05:30:11 | 505078010 | 51.2756 | 50 | 51.2756 | 51.2756 | 0 | 51.2756 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3124 | 39.3124 | 123.3618 | 0 | PROCESSED | 57601.0957407407 | 2016-08-01 02:17:52 | 55287 | 2010-04-01 00:00:00 | 55642.1205787037 | 2011-03-22 02:53:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505078010/ | Quick Look | ![]() |
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189 | GALACTIC_BULGE15 | 265.6963 | -32.7784 | 264.876935 | -32.755516 | 266.323781 | -9.39206 | 356.40742505 | -1.49294303 | 89.8786 | 55626.2338425926 | 2011-03-06 05:36:44 | 55627.5424884259 | 2011-03-07 13:01:11 | 505084010 | 50.3097 | 50 | 50.3172 | 50.3097 | 0 | 50.3252 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37.5095 | 37.5095 | 113.0559 | 0 | PROCESSED | 57601.1030439815 | 2016-08-01 02:28:23 | 55287 | 2010-04-01 00:00:00 | 55645.2697222222 | 2011-03-25 06:28:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505084010/ | Quick Look | ![]() |
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190 | GALACTIC_BULGE16 | 266.5113 | -33.2224 | 265.68867 | -33.203457 | 267.02907 | -9.817155 | 356.38592507 | -2.30771737 | 275.4625 | 55482.2533217593 | 2010-10-13 06:04:47 | 55483.5626967593 | 2010-10-14 13:30:17 | 505085010 | 55.0315 | 50 | 55.0315 | 55.0315 | 0 | 55.0315 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.6341 | 48.6341 | 113.1139 | 1 | PROCESSED | 57553.750787037 | 2016-06-14 18:01:08 | 55287 | 2010-04-01 00:00:00 | 55502.290150463 | 2010-11-02 06:57:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505085010/ | Quick Look | ![]() |
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191 | GALACTIC_BULGE17 | 267.7467 | -33.8391 | 266.919516 | -33.82614 | 268.087567 | -10.412886 | 356.3863118 | -3.50805248 | 275.261 | 55483.5637731482 | 2010-10-14 13:31:50 | 55485.0627893518 | 2010-10-16 01:30:25 | 505086010 | 53.1266 | 50 | 53.1266 | 54.0895 | 0 | 54.0895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.2769 | 46.2769 | 129.4938 | 1 | PROCESSED | 57553.7652430556 | 2016-06-14 18:21:57 | 55287 | 2010-04-01 00:00:00 | 55508.2025694444 | 2010-11-08 04:51:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505086010/ | Quick Look | ![]() |
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192 | HESS J1841-55 3 | 280.1471 | -5.609 | 279.479279 | -5.656459 | 280.581257 | 17.459575 | 26.70525302 | -0.15199861 | 87.0298 | 55647.6397685185 | 2011-03-27 15:21:16 | 55648.791875 | 2011-03-28 19:00:18 | 505090010 | 49.549 | 50 | 49.581 | 49.549 | 0 | 49.581 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7935 | 42.7935 | 99.5239 | 1 | PROCESSED | 57601.3633101852 | 2016-08-01 08:43:10 | 55287 | 2010-04-01 00:00:00 | 55666.2655439815 | 2011-04-15 06:22:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505090010/ | Quick Look | ![]() |
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193 | BD+43 3654 | 308.4185 | 44.0658 | 307.988834 | 43.893641 | 331.745866 | 59.550103 | 82.48241574 | 2.36274642 | 104.8287 | 55655.0785416667 | 2011-04-04 01:53:06 | 55657.0925231482 | 2011-04-06 02:13:14 | 506004010 | 97.0478 | 100 | 98.9638 | 97.0478 | 0 | 98.9638 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 88.9256 | 88.9256 | 173.9877 | 0 | PROCESSED | 57601.4465972222 | 2016-08-01 10:43:06 | 56037 | 2012-04-20 00:00:00 | 55670.3073842593 | 2011-04-19 07:22:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060010 | It is very important to search for possible particle-acceleration sites among the astrophysical objects. Very recently, synchrotron emission has been discovered with the VLA radio observation from a bow shock region of a runaway star, BD+43 3654, having a very fast stellar wind whose velocity reaches up to 2300 km/s. The maximum energy is estimated to be about 10 TeV, and thus the emission should come to the X-ray band. Here, we propose to perform the 100 ksec observation of BD+43 3654 with Suzaku, in order to determine the strength of the shock from the temperature of the post-shock plasma and to determine the maximum energy of the accelerated electrons. | GALACTIC DIFFUSE EMISSION | 5 | A | YUKIKATSU TERADA | JAP | 6 | AO6 | SUZAKU OBSERVATION OF NON-THERMAL EMISSION FROM A BOW SHOCK REGION OF A RUNAWAY STAR, BD+43 3654 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506004010/ | Quick Look | ![]() |
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194 | JUPITER | 28.9811 | 10.6021 | 28.315769 | 10.357786 | 30.678261 | -1.183373 | 147.5984875 | -49.15640747 | 249.1843 | 55937.2038773148 | 2012-01-11 04:53:35 | 55938.208599537 | 2012-01-12 05:00:23 | 506006030 | 34.8942 | 160 | 34.9022 | 34.9102 | 0 | 34.8942 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.2081 | 32.2081 | 86.7918 | 2 | PROCESSED | 57604.3101273148 | 2016-08-04 07:26:35 | 56319 | 2013-01-27 00:00:00 | 55952.170787037 | 2012-01-26 04:05:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006030/ | Quick Look | ![]() |
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195 | CYGNUS LOOP W-B-S | 311.1967 | 30.3719 | 310.678738 | 30.189494 | 325.222144 | 46.233696 | 72.9110541 | -7.69596159 | 71.021 | 55693.7715277778 | 2011-05-12 18:31:00 | 55694.9794212963 | 2011-05-13 23:30:22 | 506008010 | 55.6499 | 56 | 55.6499 | 55.6499 | 0 | 55.6499 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.8516 | 49.8516 | 104.3259 | 1 | PROCESSED | 57602.0472916667 | 2016-08-02 01:08:06 | 56072 | 2012-05-25 00:00:00 | 55705.1847800926 | 2011-05-24 04:26:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060042 | The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 6 | AO6 | HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506008010/ | Quick Look | ![]() |
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196 | HESSJ1857-B | 284.5485 | 2.7494 | 283.920534 | 2.680934 | 286.113501 | 25.379812 | 36.14879968 | -0.24805898 | 252.48 | 55866.7917592593 | 2011-11-01 19:00:08 | 55867.6946990741 | 2011-11-02 16:40:22 | 506020010 | 40.6869 | 40 | 40.6869 | 40.6949 | 0 | 40.6949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.0513 | 40.0513 | 78.0119 | 0 | PROCESSED | 57603.6841435185 | 2016-08-03 16:25:10 | 56246 | 2012-11-15 00:00:00 | 55879.1725 | 2011-11-14 04:08:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506020010/ | Quick Look | ![]() |
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197 | NGC 7618 | 349.8326 | 42.9144 | 349.23867 | 42.640678 | 11.92237 | 42.546584 | 105.51742003 | -16.82119292 | 269.9991 | 55911.4056828704 | 2011-12-16 09:44:11 | 55913.6161458333 | 2011-12-18 14:47:15 | 506027010 | 101.1772 | 100 | 101.1852 | 101.1772 | 0 | 101.1852 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.774 | 95.774 | 190.9399 | 0 | PROCESSED | 57604.196712963 | 2016-08-04 04:43:16 | 56289 | 2012-12-28 00:00:00 | 55922.1112847222 | 2011-12-27 02:40:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060073 | We propose to observe nearby merging galaxy group NGC 7618. The asymmetric X-ray shape with a tail and a sharp brightness discontinuity were discoverd by observations of ASCA and Chandra. This is due to a merging with an another galaxy group, UGC 12491, which has similar mass of NGC 7618. The pair is in the primary stage of merging, then we need to obtain the information of the gas outside region to clarify the process of the merging. By taking advantage of low background and high energy resolution of XIS, we estimate accurately distribuion of temperature and metal abundances around both galaxy groups. Then we aim to clarify the process of the merging system of the galaxy groups. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUHIRO HAYASHI | JAP | 6 | AO6 | OBSERVATION OF NEARBY MERGING GALAXY GROUP NGC 7618 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506027010/ | Quick Look | ![]() |
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198 | VELA PWN E5 | 130.8405 | -45.4455 | 130.413883 | -45.264192 | 156.083116 | -59.869195 | 264.62375514 | -1.83200273 | 304.5067 | 55712.7368402778 | 2011-05-31 17:41:03 | 55712.9570601852 | 2011-05-31 22:58:10 | 506048010 | 15.9196 | 15 | 15.9196 | 15.9196 | 0 | 15.9436 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.9129 | 11.9129 | 19.0159 | 0 | PROCESSED | 57602.1724305556 | 2016-08-02 04:08:18 | 56093 | 2012-06-15 00:00:00 | 55726.0610185185 | 2011-06-14 01:27:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506048010/ | Quick Look | ![]() |
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199 | VELA PWN E7 | 131.6969 | -45.5129 | 131.268004 | -45.328458 | 157.17001 | -59.613979 | 265.05012769 | -1.40367097 | 303.5042 | 55713.2300925926 | 2011-06-01 05:31:20 | 55713.4688310185 | 2011-06-01 11:15:07 | 506050010 | 13.0454 | 15 | 13.0494 | 13.0454 | 0 | 13.0534 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0751 | 11.0751 | 20.622 | 0 | PROCESSED | 57602.181875 | 2016-08-02 04:21:54 | 56093 | 2012-06-15 00:00:00 | 55726.0999768518 | 2011-06-14 02:23:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506050010/ | Quick Look | ![]() |
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200 | G236+38 OFF | 149.4117 | 1.4719 | 148.767122 | 1.710754 | 151.004118 | -10.298746 | 237.07053965 | 41.11953464 | 293.1755 | 55719.6375462963 | 2011-06-07 15:18:04 | 55721.2780092593 | 2011-06-09 06:40:20 | 506056010 | 70.8135 | 70 | 70.8215 | 70.8295 | 0 | 70.8135 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.4444 | 64.4444 | 141.7278 | 0 | PROCESSED | 57602.2364583333 | 2016-08-02 05:40:30 | 56127 | 2012-07-19 00:00:00 | 55757.6968518518 | 2011-07-15 16:43:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061321 | Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. | GALACTIC DIFFUSE EMISSION | 5 | B | DAVID HENLEY | USA | 6 | AO6 | UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506056010/ | Quick Look | ![]() |
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201 | KES 27 | 237.1872 | -53.7777 | 236.229597 | -53.624833 | 247.581589 | -32.858337 | 327.32071311 | 0.47884394 | 101.6269 | 55983.5400231482 | 2012-02-26 12:57:38 | 55985.4633217593 | 2012-02-28 11:07:11 | 506063010 | 109.3535 | 120 | 109.4015 | 109.3535 | 0 | 109.4015 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 115.3321 | 115.3321 | 166.148 | 4 | PROCESSED | 57604.7717592593 | 2016-08-04 18:31:20 | 55652 | 2011-04-01 00:00:00 | 55995.1904976852 | 2012-03-09 04:34:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506063010/ | Quick Look | ![]() |
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202 | G349.7+0.2 | 259.4954 | -37.4452 | 258.645482 | -37.392398 | 261.399155 | -14.316641 | 349.72102569 | 0.17051597 | 282.4112 | 55833.4324537037 | 2011-09-29 10:22:44 | 55838.1341898148 | 2011-10-04 03:13:14 | 506064010 | 160.4024 | 160 | 160.4264 | 160.4024 | 0 | 160.4344 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 144.6151 | 144.6151 | 404.22 | 5 | PROCESSED | 57603.3931134259 | 2016-08-03 09:26:05 | 55652 | 2011-04-01 00:00:00 | 55858.5356018518 | 2011-10-24 12:51:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506064010/ | Quick Look | ![]() |
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203 | FERMI_BUBBLE_N2 | 234.4045 | 4.1242 | 233.780349 | 4.287466 | 230.936286 | 22.866796 | 10.25580888 | 44.20015183 | 287.5 | 56145.3990740741 | 2012-08-06 09:34:40 | 56145.971099537 | 2012-08-06 23:18:23 | 507002010 | 22.491 | 20 | 22.491 | 22.491 | 0 | 22.491 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.5 | 22.5 | 49.4059 | 0 | PROCESSED | 57606.7805555556 | 2016-08-06 18:44:00 | 56630 | 2013-12-04 00:00:00 | 56264.5602662037 | 2012-12-03 13:26:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507002010/ | Quick Look | ![]() |
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204 | FERMI_BUBBLE_N3 | 234.0339 | 6.0902 | 233.417441 | 6.254904 | 230.000126 | 24.67426 | 12.27048516 | 45.60209416 | 287.4996 | 56145.9724537037 | 2012-08-06 23:20:20 | 56146.4377893518 | 2012-08-07 10:30:25 | 507003010 | 22.4846 | 20 | 22.4846 | 22.5086 | 0 | 22.4926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.836 | 19.836 | 40.1959 | 0 | PROCESSED | 57606.7866782407 | 2016-08-06 18:52:49 | 56535 | 2013-08-31 00:00:00 | 56169.009837963 | 2012-08-30 00:14:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507003010/ | Quick Look | ![]() |
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205 | FERMI_BUBBLE_N6 | 233.4001 | 9.0706 | 232.795243 | 9.23775 | 228.456067 | 27.38567 | 15.47217439 | 47.71191257 | 287.5008 | 56147.4330324074 | 2012-08-08 10:23:34 | 56147.9606134259 | 2012-08-08 23:03:17 | 507006010 | 20.607 | 20 | 20.607 | 20.6246 | 0 | 20.619 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.3045 | 20.3045 | 45.58 | 0 | PROCESSED | 57606.8039467593 | 2016-08-06 19:17:41 | 56626 | 2013-11-30 00:00:00 | 56260.4951851852 | 2012-11-29 11:53:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507006010/ | Quick Look | ![]() |
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206 | FERMI_BUBBLE_S6 | 326.677 | -46.8481 | 325.870677 | -47.079705 | 311.980005 | -31.325121 | 351.64382858 | -48.94656928 | 44.0056 | 56037.1166087963 | 2012-04-20 02:47:55 | 56037.6009027778 | 2012-04-20 14:25:18 | 507014010 | 19.6439 | 20 | 19.6519 | 19.6439 | 0 | 19.6599 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.1827 | 14.1827 | 41.8399 | 1 | PROCESSED | 57605.2222916667 | 2016-08-05 05:20:06 | 56420 | 2013-05-08 00:00:00 | 56054.1845833333 | 2012-05-07 04:25:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507014010/ | Quick Look | ![]() |
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207 | GC_SOUTH_2 | 268.3751 | -29.7084 | 267.575601 | -29.69856 | 268.570633 | -6.275404 | 0.22024801 | -1.8703349 | 273.7998 | 56192.7899421296 | 2012-09-22 18:57:31 | 56194.081412037 | 2012-09-24 01:57:14 | 507029010 | 52.4469 | 50 | 52.4629 | 52.4469 | 0 | 52.4549 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45.2307 | 45.2307 | 111.5759 | 1 | PROCESSED | 57607.1634259259 | 2016-08-07 03:55:20 | 56689 | 2014-02-01 00:00:00 | 56321.5121875 | 2013-01-29 12:17:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507029010/ | Quick Look | ![]() |
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208 | G298.6-0.0 | 183.3873 | -62.6234 | 182.718198 | -62.34531 | 219.474963 | -53.500968 | 298.59191859 | -0.0713547 | 133.8706 | 56341.7597222222 | 2013-02-18 18:14:00 | 56342.6981712963 | 2013-02-19 16:45:22 | 507037020 | 39.7247 | 35 | 39.7247 | 39.7247 | 0 | 39.7247 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 36.2621 | 36.2621 | 81.0699 | 0 | PROCESSED | 57610.644849537 | 2016-08-10 15:28:35 | 56721 | 2014-03-05 00:00:00 | 56362.8029861111 | 2013-03-11 19:16:18 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037020/ | Quick Look | ![]() |
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209 | MSH15-56_SW | 238.0528 | -56.3239 | 237.060386 | -56.174494 | 248.949341 | -35.191477 | 326.11105465 | -1.81589779 | 86.2015 | 56326.3325 | 2013-02-03 07:58:48 | 56327.8577314815 | 2013-02-04 20:35:08 | 507039010 | 86.0122 | 100 | 86.0122 | 86.0122 | 0 | 86.0122 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.3912 | 88.3912 | 131.7719 | 2 | PROCESSED | 57610.534849537 | 2016-08-10 12:50:11 | 56714 | 2014-02-26 00:00:00 | 56345.5312847222 | 2013-02-22 12:45:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070055 | The magnetic field upstream the shock front of the SN blast wave is the key parameter for discussing particle acceleration. In this study we try to constrain the upstream magnetic field and its amplification based on the ionization parameter of heated ISM just behind the shock. For this purpose, we propose a 100 ks XIS observation of an middle aged SNR MSH 15-56 with non-thermal filaments and an anomalously large ionization age for its dynamical age. | GALACTIC DIFFUSE EMISSION | 5 | C | YOICHI YATSU | JAP | 7 | AO7 | A STUDY OF PARTICLE ACCELERATION BASED ON THE THERMAL PLASMA BEHIND THE SHOCK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507039010/ | Quick Look | ![]() |
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210 | VELA PWN N1 | 128.8231 | -44.9507 | 128.399065 | -44.776941 | 153.1311 | -60.168643 | 263.36545364 | -2.659461 | 324.0013 | 56108.9552083333 | 2012-06-30 22:55:30 | 56109.3487962963 | 2012-07-01 08:22:16 | 507048010 | 17.8014 | 15 | 17.8094 | 17.8014 | 0 | 17.8094 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.2047 | 19.2047 | 33.9999 | 1 | PROCESSED | 57606.5230439815 | 2016-08-06 12:33:11 | 56592 | 2013-10-27 00:00:00 | 56226.6327083333 | 2012-10-26 15:11:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507048010/ | Quick Look | ![]() |
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211 | VELA PWN N2 | 128.845 | -44.6374 | 128.418547 | -44.463562 | 152.844801 | -59.889474 | 263.12360018 | -2.45940596 | 325.4993 | 56109.3500115741 | 2012-07-01 08:24:01 | 56109.7210185185 | 2012-07-01 17:18:16 | 507049010 | 18.4118 | 15 | 18.4198 | 18.4118 | 0 | 18.4198 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.7623 | 18.7623 | 32.024 | 0 | PROCESSED | 57606.5242939815 | 2016-08-06 12:34:59 | 56493 | 2013-07-20 00:00:00 | 56127.0941319444 | 2012-07-19 02:15:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507049010/ | Quick Look | ![]() |
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212 | VELA PWN N3 | 128.8419 | -44.3423 | 128.413265 | -44.168478 | 152.550585 | -59.63427 | 262.88578161 | -2.28439697 | 325.9006 | 56109.7216782407 | 2012-07-01 17:19:13 | 56110.0161574074 | 2012-07-02 00:23:16 | 507050010 | 12.3984 | 15 | 12.3984 | 12.3984 | 0 | 12.3984 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2454 | 13.2454 | 25.4319 | 1 | PROCESSED | 57606.5311805556 | 2016-08-06 12:44:54 | 56493 | 2013-07-20 00:00:00 | 56127.104849537 | 2012-07-19 02:30:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507050010/ | Quick Look | ![]() |
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213 | VELA PWN N6 | 128.8205 | -43.4604 | 128.385504 | -43.286672 | 151.68228 | -58.872108 | 262.17003306 | -1.76832201 | 122.021 | 56258.4379050926 | 2012-11-27 10:30:35 | 56258.805625 | 2012-11-27 19:20:06 | 507053010 | 15.3401 | 15 | 15.3481 | 15.3481 | 0 | 15.3401 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.9013 | 13.9013 | 31.7599 | 0 | PROCESSED | 57608.0978819444 | 2016-08-08 02:20:57 | 56641 | 2013-12-15 00:00:00 | 56275.6586111111 | 2012-12-14 15:48:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507053010/ | Quick Look | ![]() |
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214 | G7.6+2.0 | 268.7973 | -21.391 | 268.047539 | -21.383335 | 268.869887 | 2.045161 | 7.58937554 | 2.00788461 | 270.4016 | 56194.0843865741 | 2012-09-24 02:01:31 | 56194.4237037037 | 2012-09-24 10:10:08 | 507065010 | 16.521 | 10 | 16.529 | 16.521 | 0 | 16.5347 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.1603 | 12.1603 | 29.3139 | 2 | PROCESSED | 57607.1654050926 | 2016-08-07 03:58:11 | 56676 | 2014-01-19 00:00:00 | 56315.5110069444 | 2013-01-23 12:15:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | TOBIAS PRINZ | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507065010/ | Quick Look | ![]() |
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215 | GRXE_E_2 | 267.6193 | -27.2463 | 266.835371 | -27.232829 | 267.869305 | -3.822869 | 2.00029183 | -0.04392641 | 105.0002 | 56366.4085532407 | 2013-03-15 09:48:19 | 56368.7772569444 | 2013-03-17 18:39:15 | 507069010 | 103.6873 | 100 | 103.6873 | 103.6873 | 0 | 103.6873 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.5834 | 95.5834 | 204.6259 | 2 | PROCESSED | 57610.8702314815 | 2016-08-10 20:53:08 | 56018 | 2012-04-01 00:00:00 | 56379.6047106482 | 2013-03-28 14:30:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507069010/ | Quick Look | ![]() |
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216 | GRXE_E_3 | 267.7634 | -27.0307 | 266.980773 | -27.017932 | 267.994323 | -3.605243 | 2.25114568 | -0.04369036 | 105.0001 | 56368.7777314815 | 2013-03-17 18:39:56 | 56371.1111458333 | 2013-03-20 02:40:03 | 507070010 | 101.1726 | 100 | 101.1806 | 101.1726 | 0 | 101.1806 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.6028 | 103.6028 | 201.5898 | 0 | PROCESSED | 57610.8916782407 | 2016-08-10 21:24:01 | 56018 | 2012-04-01 00:00:00 | 56380.5799768518 | 2013-03-29 13:55:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507070010/ | Quick Look | ![]() |
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217 | MBM36 | 238.3612 | -4.7913 | 237.700971 | -4.643898 | 237.207481 | 15.120143 | 4.00454082 | 35.69817373 | 279.4993 | 56155.0155787037 | 2012-08-16 00:22:26 | 56156.7563425926 | 2012-08-17 18:09:08 | 507077010 | 81.0158 | 80 | 81.0158 | 81.0176 | 0 | 81.0176 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.3301 | 80.3301 | 150.3877 | 4 | PROCESSED | 57606.8991782407 | 2016-08-06 21:34:49 | 56018 | 2012-04-01 00:00:00 | 56170.1653240741 | 2012-08-31 03:58:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507077010/ | Quick Look | ![]() |
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218 | MBM20 | 68.9377 | -14.6308 | 68.365051 | -14.732172 | 64.468357 | -36.225149 | 211.4041789 | -36.56532035 | 78.376 | 56164.0544328704 | 2012-08-25 01:18:23 | 56166.3530092593 | 2012-08-27 08:28:20 | 507079010 | 82.8814 | 80 | 82.8814 | 82.8814 | 0 | 82.8814 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.8668 | 73.8668 | 198.5577 | 2 | PROCESSED | 57606.9726851852 | 2016-08-06 23:20:40 | 56018 | 2012-04-01 00:00:00 | 56212.7316087963 | 2012-10-12 17:33:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507079010/ | Quick Look | ![]() |
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219 | 3C 397 | 286.9092 | 7.1226 | 286.301586 | 7.04303 | 289.342559 | 29.434869 | 41.11337729 | -0.33398163 | 251.9939 | 56595.6848611111 | 2013-10-30 16:26:12 | 56597.9106828704 | 2013-11-01 21:51:23 | 508001010 | 103.5157 | 100 | 103.5157 | 103.5157 | 0 | 103.5157 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.6753 | 98.6753 | 192.2937 | 2 | PROCESSED | 57613.2313425926 | 2016-08-13 05:33:08 | 57012 | 2014-12-21 00:00:00 | 56645.6863541667 | 2013-12-19 16:28:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080011 | 3C 397 is a Galactic Supernova remnant (SNR) ,whose X-ray spectrum has prominent Fe K line emission. We analyzed Suzaku AO5 data, it resulted in finding of Fe Lya Line. This is a symptomatic of over-ionized (recombining) plasma. On the other hand, the Fe K line center indicates under-ionized (ionizing) plasma. This means that 3C 397 may consisting of two opposite type of plasma: ionizing and recombining. Such a strange state of plasma is not discovered in any SNR.This discovery will be a key to uncovering a mystery of the origin of recombining plasma. However, we still not detect Fe Radiative recombination continuum (RRC),which is a evidence of recombining plasma. To detect the Fe RRC, we propose 150 ks additional observation of 3C 397. | GALACTIC DIFFUSE EMISSION | 5 | C | RYUSUKE SUGAWARA | JAP | 8 | AO8 | THE INDICATION OF RECOMBINING PLASMA COEXISTING WITH IONIZING PLASMA IN 3C 397 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508001010/ | Quick Look | ![]() |
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220 | W44_EAST | 284.1459 | 1.2991 | 283.51111 | 1.232548 | 285.500202 | 23.981686 | 34.67473844 | -0.5521979 | 254.9985 | 56583.3375231482 | 2013-10-18 08:06:02 | 56584.8897337963 | 2013-10-19 21:21:13 | 508004010 | 58.2965 | 60 | 58.3045 | 58.2965 | 0 | 58.3149 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 52.7276 | 52.7276 | 134.0958 | 2 | PROCESSED | 57613.0782407407 | 2016-08-13 01:52:40 | 57004 | 2014-12-13 00:00:00 | 56637.6520949074 | 2013-12-11 15:39:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508004010/ | Quick Look | ![]() |
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221 | NW_SRC | 221.7499 | -1.3162 | 221.105287 | -1.10746 | 219.72393 | 14.106437 | 351.9522425 | 50.22344256 | 289.0003 | 56499.3402430556 | 2013-07-26 08:09:57 | 56499.8412037037 | 2013-07-26 20:11:20 | 508007010 | 23.554 | 20 | 23.554 | 23.5554 | 0 | 23.554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.103 | 24.103 | 43.274 | 0 | PROCESSED | 57612.0357986111 | 2016-08-12 00:51:33 | 56955 | 2014-10-25 00:00:00 | 56587.4553819444 | 2013-10-22 10:55:45 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508007010/ | Quick Look | ![]() |
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222 | SE_SRC | 287.3947 | -27.2493 | 286.61657 | -27.330736 | 285.457559 | -4.737737 | 9.97288902 | -15.74410072 | 84.5985 | 56404.7026967593 | 2013-04-22 16:51:53 | 56405.330775463 | 2013-04-23 07:56:19 | 508009010 | 20.3287 | 20 | 20.3287 | 20.3287 | 0 | 20.3287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.5938 | 17.5938 | 54.2639 | 1 | PROCESSED | 57611.1595833333 | 2016-08-11 03:49:48 | 56792 | 2014-05-15 00:00:00 | 56425.5555092593 | 2013-05-13 13:19:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508009010/ | Quick Look | ![]() |
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223 | SE_BGD | 288.7458 | -25.773 | 287.977196 | -25.860714 | 286.843449 | -3.422342 | 11.87589948 | -16.28754896 | 81.8427 | 56405.3324537037 | 2013-04-23 07:58:44 | 56405.8329050926 | 2013-04-23 19:59:23 | 508010010 | 20.9653 | 20 | 20.9693 | 20.9653 | 0 | 20.9733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.7626 | 18.7626 | 43.234 | 0 | PROCESSED | 57618.7907291667 | 2016-08-18 18:58:39 | 56792 | 2014-05-15 00:00:00 | 56425.5426851852 | 2013-05-13 13:01:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508010010/ | Quick Look | ![]() |
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224 | HESS J1534-571 2 | 233.1754 | -57.1 | 232.193457 | -56.931173 | 246.039407 | -36.679353 | 323.50919975 | -0.81659232 | 295.9986 | 56544.0219212963 | 2013-09-09 00:31:34 | 56544.6695949074 | 2013-09-09 16:04:13 | 508014010 | 38.9186 | 40 | 38.9426 | 38.9186 | 0 | 38.9506 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.8565 | 36.8565 | 55.9539 | 0 | PROCESSED | 57612.5722916667 | 2016-08-12 13:44:06 | 56990 | 2014-11-29 00:00:00 | 56622.6062268518 | 2013-11-26 14:32:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508014010/ | Quick Look | ![]() |
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225 | HESSJ1858-B | 284.4324 | 2.2013 | 283.801854 | 2.133387 | 285.919657 | 24.847772 | 35.60820996 | -0.39516335 | 251.7997 | 56593.9763310185 | 2013-10-28 23:25:55 | 56595.1313541667 | 2013-10-30 03:09:09 | 508022010 | 52.595 | 50 | 52.619 | 52.611 | 0 | 52.595 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49.9941 | 49.9941 | 99.7858 | 2 | PROCESSED | 57613.1665393518 | 2016-08-13 03:59:49 | 56975 | 2014-11-14 00:00:00 | 56608.7129166667 | 2013-11-12 17:06:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080052 | HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 8 | AO8 | DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508022010/ | Quick Look | ![]() |
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226 | JUPITER | 104.0103 | 23.0994 | 103.254149 | 23.165009 | 102.868934 | 0.282188 | 192.60135744 | 11.26438783 | 264.454 | 56763.7225 | 2014-04-16 17:20:24 | 56764.0627083333 | 2014-04-17 01:30:18 | 508023060 | 8.8696 | 160 | 8.8776 | 8.8696 | 0 | 8.8856 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9524652778 | 2016-08-14 22:51:33 | 57212 | 2015-07-09 00:00:00 | 56846.5928472222 | 2014-07-08 14:13:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023060/ | Quick Look | ![]() |
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227 | JUPITER | 104.4171 | 23.0664 | 103.66133 | 23.133929 | 103.244601 | 0.2859 | 192.79210183 | 11.59024455 | 264.5983 | 56766.7815972222 | 2014-04-19 18:45:30 | 56767.1147916667 | 2014-04-20 02:45:18 | 508023100 | 9.3759 | 160 | 9.3839 | 9.3919 | 0 | 9.3759 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9623263889 | 2016-08-14 23:05:45 | 57212 | 2015-07-09 00:00:00 | 56782.4942824074 | 2014-05-05 11:51:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023100/ | Quick Look | ![]() |
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228 | VELA JR WEST3 | 131.773 | -46.2743 | 131.349543 | -46.08957 | 158.06279 | -60.232297 | 265.67717372 | -1.83917649 | 116.21 | 56620.0804861111 | 2013-11-24 01:55:54 | 56620.7320949074 | 2013-11-24 17:34:13 | 508038010 | 34.9611 | 30 | 34.9911 | 34.9611 | 0 | 34.9611 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.4434 | 40.4434 | 56.2959 | 0 | PROCESSED | 57613.4017708333 | 2016-08-13 09:38:33 | 56995 | 2014-12-04 00:00:00 | 56629.6399421296 | 2013-12-03 15:21:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDETOSHI SANO | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508038010/ | Quick Look | ![]() |
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229 | VELA PWN W5 | 126.0444 | -45.2057 | 125.630533 | -45.042674 | 149.898743 | -61.36183 | 262.42223435 | -4.39970467 | 94.9992 | 56591.8819560185 | 2013-10-26 21:10:01 | 56592.3202777778 | 2013-10-27 07:41:12 | 508046010 | 15.8569 | 15 | 15.8729 | 15.8569 | 0 | 15.8809 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.7358 | 12.7358 | 37.8639 | 0 | PROCESSED | 57613.1438657407 | 2016-08-13 03:27:10 | 57009 | 2014-12-18 00:00:00 | 56643.6567824074 | 2013-12-17 15:45:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508046010/ | Quick Look | ![]() |
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230 | VELA PWN W6 | 125.6171 | -45.2116 | 125.2045 | -45.05026 | 149.354915 | -61.513653 | 262.25511101 | -4.65051542 | 95.0008 | 56592.3208912037 | 2013-10-27 07:42:05 | 56592.8209722222 | 2013-10-27 19:42:12 | 508047010 | 17.2398 | 15 | 17.2478 | 17.2398 | 0 | 17.2398 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.2299 | 16.2299 | 43.1999 | 0 | PROCESSED | 57613.1284606482 | 2016-08-13 03:04:59 | 57011 | 2014-12-20 00:00:00 | 56645.5849421296 | 2013-12-19 14:02:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508047010/ | Quick Look | ![]() |
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231 | RX J1713 SOUTHEAST | 258.9281 | -40.015 | 258.058505 | -39.959445 | 261.147328 | -16.912866 | 347.36958165 | -0.95677146 | 84 | 56711.6431018518 | 2014-02-23 15:26:04 | 56713.2190046296 | 2014-02-25 05:15:22 | 508067010 | 80.0774 | 80 | 80.0854 | 80.0854 | 0 | 80.0774 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.9291 | 74.9291 | 118.0069 | 0 | PROCESSED | 57613.9112152778 | 2016-08-13 21:52:09 | 57173 | 2015-05-31 00:00:00 | 56806.6951851852 | 2014-05-29 16:41:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081313 | Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield. | GALACTIC DIFFUSE EMISSION | 5 | A | FABIO ACERO | USA | 8 | AO8 | STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508067010/ | Quick Look | ![]() |
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232 | MBM36-OFF | 238.9304 | -1.7878 | 238.282545 | -1.642781 | 237.109098 | 18.17526 | 7.39248129 | 37.0792042 | 270.0134 | 56533.8916319444 | 2013-08-29 21:23:57 | 56535.9634606482 | 2013-08-31 23:07:23 | 508074010 | 74.1565 | 80 | 74.1645 | 74.1645 | 0 | 74.1565 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 64.2521 | 64.2521 | 178.982 | 1 | PROCESSED | 57612.4561574074 | 2016-08-12 10:56:52 | 56970 | 2014-11-09 00:00:00 | 56603.6967476852 | 2013-11-07 16:43:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081322 | We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission. | GALACTIC DIFFUSE EMISSION | 5 | A | EUGENIO URSINO | USA | 8 | AO8 | PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508074010/ | Quick Look | ![]() |
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233 | GRXE_E_1 | 267.4747 | -27.4596 | 266.689479 | -27.445424 | 267.744238 | -4.038324 | 1.75131157 | -0.04310182 | 105.3995 | 56726.0649537037 | 2014-03-10 01:33:32 | 56728.6459722222 | 2014-03-12 15:30:12 | 508075010 | 103.5331 | 100 | 103.5491 | 103.5331 | 0 | 103.5559 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 85.3446 | 85.3446 | 222.9818 | 2 | PROCESSED | 57614.0622453704 | 2016-08-14 01:29:38 | 56383 | 2013-04-01 00:00:00 | 56740.8547453704 | 2014-03-24 20:30:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086001 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508075010/ | Quick Look | ![]() |
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234 | LDN1563 | 75.5195 | 13.8744 | 74.812622 | 13.803125 | 75.779261 | -8.85474 | 187.14092451 | -16.70693442 | 81.1182 | 56523.4274768518 | 2013-08-19 10:15:34 | 56525.2535648148 | 2013-08-21 06:05:08 | 508080010 | 83.588 | 80 | 83.588 | 83.596 | 0 | 83.604 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.6741 | 79.6741 | 157.7538 | 2 | PROCESSED | 57612.368912037 | 2016-08-12 08:51:14 | 56383 | 2013-04-01 00:00:00 | 56587.8175694445 | 2013-10-22 19:37:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508080010/ | Quick Look | ![]() |
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235 | W49B | 287.7839 | 9.1153 | 287.185543 | 9.031646 | 290.654077 | 31.289696 | 43.2808507 | -0.18308455 | 82.0062 | 57122.7467013889 | 2015-04-10 17:55:15 | 57125.7127777778 | 2015-04-13 17:06:24 | 509001010 | 81.4763 | 400 | 81.4763 | 113.9098 | 0 | 113.9162 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.986724537 | 2016-08-17 23:40:53 | 56748 | 2014-04-01 00:00:00 | 57136.5735300926 | 2015-04-24 13:45:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001010/ | Quick Look | ![]() |
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236 | W49B | 287.7843 | 9.1147 | 287.18594 | 9.031044 | 290.654435 | 31.289046 | 43.28050127 | -0.18371216 | 82.0064 | 57128.6891203704 | 2015-04-16 16:32:20 | 57131.6619328704 | 2015-04-19 15:53:11 | 509001030 | 100.9959 | 400 | 100.9959 | 106.4207 | 0 | 106.3967 | 4 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0043518518 | 2016-08-18 00:06:16 | 56748 | 2014-04-01 00:00:00 | 57220.3809722222 | 2015-07-17 09:08:36 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001030/ | Quick Look | ![]() |
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237 | G1.9+0.3 | 267.1939 | -27.1714 | 266.410492 | -27.155866 | 267.488865 | -3.754805 | 1.87009843 | 0.31910459 | 104.2133 | 57099.6072569445 | 2015-03-18 14:34:27 | 57101.7854976852 | 2015-03-20 18:51:07 | 509003010 | 92.0313 | 100 | 92.0313 | 97.0859 | 0 | 97.0699 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8499189815 | 2016-08-17 20:23:53 | 57527 | 2016-05-19 00:00:00 | 57160.6404861111 | 2015-05-18 15:22:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090030 | We propose a Suzaku observations of the youngest supernova remnant (SNR) G1.9+0.3. We aim to detect flux increase and spectral hardening of synchrotron X-rays since 2011 when the previous Suzaku observation was performed. The measurement should provide us with important information about the maximum acceleration energy attainable by diffusive shock acceleration in SNRs. Suzaku XIS is the most suitable detector since it has the large effective area even in the hard band up to 10 keV. If X-ray flux increase is significantly larger than that measured in the radio band, we can conclude that maximum acceleration energy is becoming higher at present. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAAKI TANAKA | YASUNOBU UCHIYAMA | JAP | 9 | AO9 | MEASUREMENT OF TIME VARIABILITY OF SYNCHROTRON X-RAYS FROM THE YOUNGEST SUPERNOVA REMNANT G1.9+0.3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509003010/ | Quick Look | ![]() |
238 | VELA PWN GEV5 | 128.1777 | -45.5057 | 127.759875 | -45.334391 | 152.900781 | -60.876983 | 263.54099229 | -3.35509044 | 120.3003 | 56987.5594328704 | 2014-11-26 13:25:35 | 56987.9009490741 | 2014-11-26 21:37:22 | 509015010 | 16.1889 | 15 | 16.1889 | 16.2127 | 0 | 16.1969 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.822025463 | 2016-08-16 19:43:43 | 57368 | 2015-12-12 00:00:00 | 57002.4333564815 | 2014-12-11 10:24:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509015010/ | Quick Look | ![]() |
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239 | G166.0+4.3_SE | 81.6718 | 42.6436 | 80.778042 | 42.601144 | 83.516564 | 19.390604 | 166.37682371 | 4.1455421 | 266.8508 | 57094.5870486111 | 2015-03-13 14:05:21 | 57095.305 | 2015-03-14 07:19:12 | 509024020 | 26.0329 | 27 | 26.0329 | 27.3929 | 0 | 27.3929 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.780625 | 2016-08-17 18:44:06 | 57478 | 2016-03-31 00:00:00 | 57108.4092939815 | 2015-03-27 09:49:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024020/ | Quick Look | ![]() |
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240 | CIZA J1358.9-4750_NE | 209.8984 | -47.6059 | 209.108141 | -47.363535 | 225.843523 | -32.945776 | 314.66509294 | 13.70714471 | 293.0012 | 56879.8864467593 | 2014-08-10 21:16:29 | 56880.8606481482 | 2014-08-11 20:39:20 | 509025010 | 40.2748 | 40 | 40.2828 | 40.2828 | 0 | 40.2748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.7468 | 7.7468 | 19.736 | 0 | PROCESSED | 57616.4833333333 | 2016-08-16 11:36:00 | 57270 | 2015-09-05 00:00:00 | 56902.1990972222 | 2014-09-02 04:46:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509025010/ | Quick Look | ![]() |
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241 | VERJ2019_P2 | 305.0647 | 36.873 | 304.594845 | 36.714007 | 321.75914 | 54.196272 | 75.14540231 | 0.26023113 | 251.4317 | 56970.0347453704 | 2014-11-09 00:50:02 | 56971.0419097222 | 2014-11-10 01:00:21 | 509029010 | 40.4941 | 40 | 40.4941 | 40.5021 | 0 | 40.5021 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7544791667 | 2016-08-16 18:06:27 | 57436 | 2016-02-18 00:00:00 | 57071.4171527778 | 2015-02-18 10:00:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090120 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 9 | AO9 | SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509029010/ | Quick Look | ![]() |
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242 | HB9-EAST | 75.4362 | 46.2793 | 74.514835 | 46.207153 | 79.087021 | 23.389602 | 160.82107477 | 2.65100841 | 76.7663 | 56929.6809722222 | 2014-09-29 16:20:36 | 56930.7918518518 | 2014-09-30 19:00:16 | 509033010 | 51.0581 | 50 | 51.0581 | 51.0581 | 0 | 51.0581 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6020949074 | 2016-08-16 14:27:01 | 57358 | 2015-12-02 00:00:00 | 56986.4031481482 | 2014-11-25 09:40:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091312 | We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509033010/ | Quick Look | ![]() |
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243 | G93.3+6.9 SE RIM | 313.3308 | 55.275 | 312.981985 | 55.084608 | 352.240038 | 66.77051 | 93.30192448 | 6.7583673 | 52.5 | 56812.4202314815 | 2014-06-04 10:05:08 | 56814.806412037 | 2014-06-06 19:21:14 | 509039010 | 108.0493 | 100 | 108.0493 | 108.0493 | 0 | 108.0493 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2124074074 | 2016-08-15 05:05:52 | 57205 | 2015-07-02 00:00:00 | 56835.7633912037 | 2014-06-27 18:19:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | MICHAEL STAGE | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509039010/ | Quick Look | ![]() |
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244 | OFF-FIELD3 | 339.5497 | 30.5758 | 338.966926 | 30.315472 | 354.778732 | 35.902508 | 91.73533627 | -24.10496467 | 65.4693 | 56819.1115625 | 2014-06-11 02:40:39 | 56821.2502199074 | 2014-06-13 06:00:19 | 509044010 | 97.3343 | 80 | 97.3343 | 97.3343 | 0 | 97.3343 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.618 | 38.618 | 77.04 | 0 | PROCESSED | 57615.247974537 | 2016-08-15 05:57:05 | 56748 | 2014-04-01 00:00:00 | 56834.8146527778 | 2014-06-26 19:33:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | C | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509044010/ | Quick Look | ![]() |
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245 | FERMI_JET_COCOON_3 | 314.5039 | -35.288 | 313.721159 | -35.481827 | 306.823334 | -17.363917 | 8.28342789 | -40.13197139 | 258.2411 | 56980.5600694445 | 2014-11-19 13:26:30 | 56980.9689583333 | 2014-11-19 23:15:18 | 509049010 | 18.6742 | 20 | 18.6742 | 18.6742 | 0 | 18.6742 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7925347222 | 2016-08-16 19:01:15 | 57362 | 2015-12-06 00:00:00 | 56995.6103240741 | 2014-12-04 14:38:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509049010/ | Quick Look | ![]() |
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246 | FERMI_JET_COCOON_4 | 313.0188 | -30.9125 | 312.254939 | -31.101111 | 306.880758 | -12.815318 | 13.57103518 | -38.16097703 | 249.0341 | 56968.206412037 | 2014-11-07 04:57:14 | 56968.8473958333 | 2014-11-07 20:20:15 | 509050010 | 21.6767 | 20 | 21.6767 | 21.8127 | 0 | 21.8207 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7496412037 | 2016-08-16 17:59:29 | 57358 | 2015-12-02 00:00:00 | 56982.4333333333 | 2014-11-21 10:24:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509050010/ | Quick Look | ![]() |
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247 | FERMI_JET_COCOON_6 | 319.6218 | -32.8375 | 318.863263 | -33.048426 | 311.821395 | -16.319347 | 12.30967968 | -44.01160773 | 252.671 | 56969.3646296296 | 2014-11-08 08:45:04 | 56970.0259375 | 2014-11-09 00:37:21 | 509052010 | 21.3583 | 20 | 21.3583 | 21.3583 | 0 | 21.3583 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7516782407 | 2016-08-16 18:02:25 | 57358 | 2015-12-02 00:00:00 | 56982.4382407407 | 2014-11-21 10:31:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509052010/ | Quick Look | ![]() |
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248 | DIFFUSE1B | 201.171 | 8.6653 | 200.545653 | 8.925438 | 196.184358 | 16.273856 | 327.54408522 | 69.93225444 | 119.3004 | 57014.7841898148 | 2014-12-23 18:49:14 | 57015.2196759259 | 2014-12-24 05:16:20 | 509059010 | 20.7335 | 20 | 20.7335 | 20.7415 | 0 | 20.7335 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.558275463 | 2016-08-17 13:23:55 | 57475 | 2016-03-28 00:00:00 | 57107.4265162037 | 2015-03-26 10:14:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509059010/ | Quick Look | ![]() |
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249 | 3C400.2 SE | 294.8215 | 17.1213 | 294.25847 | 17.005668 | 300.577132 | 37.964226 | 53.58084569 | -2.4098547 | 81.5889 | 56770.9416898148 | 2014-04-23 22:36:02 | 56771.4758449074 | 2014-04-24 11:25:13 | 509070010 | 24.9467 | 20 | 24.9547 | 24.9467 | 0 | 24.9627 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.7494 | 22.7494 | 46.1359 | 0 | PROCESSED | 57614.9903009259 | 2016-08-14 23:46:02 | 57152 | 2015-05-10 00:00:00 | 56789.6293865741 | 2014-05-12 15:06:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | JACCO VINK | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509070010/ | Quick Look | ![]() |
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250 | MBM16 | 49.7701 | 11.5795 | 49.086508 | 11.398432 | 50.445044 | -6.509726 | 170.60720168 | -37.27195697 | 254.3636 | 57057.0973726852 | 2015-02-04 02:20:13 | 57059.5349421296 | 2015-02-06 12:50:19 | 509073020 | 92.0425 | 80 | 92.0425 | 92.0665 | 0 | 92.0665 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6060763889 | 2016-08-17 14:32:45 | 56748 | 2014-04-01 00:00:00 | 57107.434224537 | 2015-03-26 10:25:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073020/ | Quick Look | ![]() |
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251 | VELA JR SE3 | 133.7724 | -47.2478 | 133.349347 | -47.055911 | 161.448089 | -60.302336 | 267.30006641 | -1.40128647 | 110.0008 | 56629.9618055556 | 2013-12-03 23:05:00 | 56630.5806828704 | 2013-12-04 13:56:11 | 508062010 | 27.3638 | 25 | 27.3644 | 27.3638 | 0 | 27.3658 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.7141 | 21.7141 | 53.4599 | 1 | PROCESSED | 57613.4843055556 | 2016-08-13 11:37:24 | 57005 | 2014-12-14 00:00:00 | 56639.5938888889 | 2013-12-13 14:15:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | TARO FUKUYAMA | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508062010/ | Quick Look | ![]() |
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252 | W51SW | 290.8908 | 14.1062 | 290.315286 | 14.008227 | 295.206632 | 35.736826 | 49.1149541 | -0.54215584 | 104.3698 | 55285.3081944444 | 2010-03-30 07:23:48 | 55286.3752314815 | 2010-03-31 09:00:20 | 504067010 | 43.7287 | 40 | 43.7287 | 43.7287 | 0 | 43.7287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.8137 | 9.8137 | 92.1799 | 0 | PROCESSED | 57551.0856597222 | 2016-06-12 02:03:21 | 55671 | 2011-04-20 00:00:00 | 55302.2468055556 | 2010-04-16 05:55:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDEAKI KATAGIRI | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504067010/ | Quick Look | ![]() |
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253 | GALACTIC_BULGE11 | 269.3164 | -32.1646 | 268.50059 | -32.159293 | 269.404915 | -8.724949 | 358.50010375 | -3.80248777 | 271.7893 | 55093.1531365741 | 2009-09-19 03:40:31 | 55095.6064699074 | 2009-09-21 14:33:19 | 504094010 | 93.1403 | 50 | 93.1403 | 93.1403 | 0 | 93.1403 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.9543 | 82.9543 | 211.9538 | 1 | PROCESSED | 57548.674224537 | 2016-06-09 16:10:53 | 54922 | 2009-04-01 00:00:00 | 55110.4114236111 | 2009-10-06 09:52:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504094010/ | Quick Look | ![]() |
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254 | 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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255 | VELA SOUTHWEST 1 | 126.2671 | -48.2152 | 125.877652 | -48.051248 | 153.532268 | -63.870386 | 264.99036518 | -5.99332729 | 119.5649 | 55164.9700925926 | 2009-11-29 23:16:56 | 55165.818900463 | 2009-11-30 19:39:13 | 504063010 | 32.7331 | 30 | 32.7492 | 32.7331 | 0 | 32.7411 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23.7674 | 23.7674 | 73.3099 | 0 | PROCESSED | 57549.6219791667 | 2016-06-10 14:55:39 | 55546 | 2010-12-16 00:00:00 | 55179.268587963 | 2009-12-14 06:26:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040121 | We propose 2 pointing-observations of south western part of Vela supernova remnant. Vela SNR has the largest angular size of 8 degree in diameter, so it is suitable to carry out spatial resolved spectroscopy with Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNKO HIRAGA | JAP | 4 | AO4 | X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504063010/ | Quick Look | ![]() |
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256 | (L,B)=(-20,0) | 276.6688 | -11.87 | 275.969796 | -11.90065 | 276.648122 | 11.416809 | 19.56512772 | 0.0074406 | 263.6004 | 56215.5456944444 | 2012-10-15 13:05:48 | 56219.7479861111 | 2012-10-19 17:57:06 | 507044010 | 171.8231 | 200 | 171.8231 | 171.8231 | 0 | 171.8231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 147.1192 | 147.1192 | 363.0377 | 4 | PROCESSED | 57607.9036342593 | 2016-08-07 21:41:14 | 56602 | 2013-11-06 00:00:00 | 56238.7999884259 | 2012-11-07 19:11:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070084 | We will observe the region at (l,b)=(19.57, 0.0112) to measure spatial and temporal fluctuations of the Galactic Ridge X-ray Emission (GRXE). Measuring these fluctuations is a good test to check the scenarios of point sources and star flare for the GRXE origin. Combined with archival data of XMM-Newton, 200 ks observation of Suzaku makes us able to detect the fluctuations lager than 3% of the GRXE flux. The observation mode of XIS is planed to be a normal clocking mode with no window option. | GALACTIC DIFFUSE EMISSION | 5 | B | HIDEKI UCHIYAMA | JAP | 7 | AO7 | SUZAKU STUDY OF SPATIAL AND TEMPORAL FLUCTUATIONS IN THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507044010/ | Quick Look | ![]() |
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257 | GC17 | 267.2896 | -29.5968 | 266.49097 | -29.581693 | 267.620125 | -6.178087 | 359.83441438 | -1.00224826 | 260.2809 | 54384.0425578704 | 2007-10-11 01:01:17 | 54384.480787037 | 2007-10-11 11:32:20 | 502005010 | 20.6035 | 20 | 20.6035 | 20.6035 | 0 | 20.6035 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.1743 | 18.1743 | 37.854 | 1 | PROCESSED | 57540.245787037 | 2016-06-01 05:53:56 | 54777 | 2008-11-07 00:00:00 | 54402.5689583333 | 2007-10-29 13:39:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502005010/ | Quick Look | ![]() |
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258 | VELA PWN NE2 | 130.6211 | -44.2844 | 130.186671 | -44.103918 | 154.655956 | -58.950029 | 263.6136326 | -1.23809583 | 141.8635 | 55917.0080439815 | 2011-12-22 00:11:35 | 55917.6126273148 | 2011-12-22 14:42:11 | 506042010 | 18.514 | 15 | 18.538 | 18.514 | 0 | 18.514 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.8755 | 16.8755 | 52.2259 | 0 | PROCESSED | 57604.2062962963 | 2016-08-04 04:57:04 | 56305 | 2013-01-13 00:00:00 | 55937.7869212963 | 2012-01-11 18:53:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506042010/ | Quick Look | ![]() |
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259 | SGR C BGD | 265.7856 | -29.8854 | 264.98542 | -29.862996 | 266.313646 | -6.498142 | 358.90876565 | -0.03691694 | 81.9998 | 53789.4522106482 | 2006-02-23 10:51:11 | 53789.8349421296 | 2006-02-23 20:02:19 | 500019010 | 13.3073 | 10 | 13.3153 | 13.3153 | 13.3153 | 13.3073 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12.2404 | 12.2404 | 33.0639 | 0 | PROCESSED | 57533.050462963 | 2016-05-25 01:12:40 | 54247 | 2007-05-27 00:00:00 | 54041.3629166667 | 2006-11-02 08:42:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI MURAKAMI | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500019010/ | Quick Look | ![]() |
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260 | HESS J1356-645 2 | 208.8016 | -64.5041 | 207.885224 | -64.258991 | 235.51443 | -48.210014 | 309.72820731 | -2.47708999 | 123.7329 | 56340.1852430556 | 2013-02-17 04:26:45 | 56341.4863425926 | 2013-02-18 11:40:20 | 507020010 | 51.2594 | 50 | 51.2636 | 51.2594 | 0 | 51.2594 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.1505 | 45.1505 | 112.4059 | 2 | PROCESSED | 57610.6176157407 | 2016-08-10 14:49:22 | 56718 | 2014-03-02 00:00:00 | 56352.5089930556 | 2013-03-01 12:12:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070017 | Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission. | GALACTIC DIFFUSE EMISSION | 5 | C | TAKAHISA FUJINAGA | JAP | 7 | AO7 | OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507020010/ | Quick Look | ![]() |
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261 | 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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262 | 73P/SW3 | 17.9545 | -9.1915 | 17.327695 | -9.456837 | 12.929266 | -15.523337 | 138.90931762 | -71.42827213 | 59.4015 | 53893.8691666667 | 2006-06-07 20:51:36 | 53893.9356365741 | 2006-06-07 22:27:19 | 500014040 | 3.236 | 35 | 3.236 | 3.236 | 3.236 | 3.236 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.4909 | 2.4909 | 5.7359 | 0 | PROCESSED | 57534.5832407407 | 2016-05-26 13:59:52 | 54267 | 2007-06-16 00:00:00 | 54052.5308912037 | 2006-11-13 12:44:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014040/ | Quick Look | ![]() |
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263 | G1.9+0.3 | 267.1951 | -27.1633 | 266.411742 | -27.147772 | 267.489777 | -3.746686 | 1.87759006 | 0.32236452 | 104.4114 | 55643.1608217593 | 2011-03-23 03:51:35 | 55645.2856481482 | 2011-03-25 06:51:20 | 505053010 | 100.9235 | 100 | 100.9235 | 100.9315 | 0 | 100.9315 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.4251 | 83.4251 | 183.5657 | 1 | PROCESSED | 57601.3345833333 | 2016-08-01 08:01:48 | 56025 | 2012-04-08 00:00:00 | 55658.2502546296 | 2011-04-07 06:00:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050084 | We propose to observe the youngest (100yr) SNR G1.9+0.3 with Suzaku for 100 ks. The expected scientific fruits are to reveal the earliest stage of SNR evolution via the time variation of synchrotron emission, and to investigate the nuclear synthesis in the SN explosion via the detection of gamma-ray lines from 44Ti. | GALACTIC DIFFUSE EMISSION | 5 | A | MOTOHIDE KOKUBUN | JAP | 5 | AO5 | INVESTIGATION OF THE YOUNGEST SNR G1.9+0.3 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505053010/ | Quick Look | ![]() |
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264 | 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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265 | 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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266 | 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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267 | 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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268 | 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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269 | 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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270 | 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 | ![]() |
271 | 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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272 | 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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273 | 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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274 | MBM16 | 49.752 | 11.6015 | 49.068335 | 11.420365 | 50.433531 | -6.483887 | 170.57212752 | -37.26756171 | 73.5786 | 56139.0841666667 | 2012-07-31 02:01:12 | 56140.9710416667 | 2012-08-01 23:18:18 | 507076010 | 24.9499 | 80 | 24.9499 | 24.9499 | 0 | 24.9499 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.2376 | 18.2376 | 162.962 | 1 | PROCESSED | 57606.7578703704 | 2016-08-06 18:11:20 | 56018 | 2012-04-01 00:00:00 | 56260.533125 | 2012-11-29 12:47:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076010/ | Quick Look | ![]() |
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275 | VELA JR P9 | 133.4161 | -45.7633 | 132.983285 | -45.572688 | 159.43463 | -59.191033 | 266.00615013 | -0.63304204 | 347.0009 | 54287.7015856482 | 2007-07-06 16:50:17 | 54287.9516666667 | 2007-07-06 22:50:24 | 502031010 | 13.2524 | 10 | 13.2684 | 13.2524 | 0 | 13.2684 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.8877 | 9.8877 | 21.5999 | 0 | PROCESSED | 57539.1152546296 | 2016-05-31 02:45:58 | 54703 | 2008-08-25 00:00:00 | 54333.4413657407 | 2007-08-21 10:35:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502031010/ | Quick Look | ![]() |
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276 | VELA JR P5 | 132.9105 | -45.488 | 132.477402 | -45.299188 | 158.564821 | -59.145564 | 265.56829981 | -0.72857938 | 347.002 | 54286.4486458333 | 2007-07-05 10:46:03 | 54286.7502777778 | 2007-07-05 18:00:24 | 502027010 | 10.977 | 10 | 10.977 | 10.977 | 0 | 10.977 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.7858 | 10.7858 | 26.0539 | 0 | PROCESSED | 57539.1013541667 | 2016-05-31 02:25:57 | 54696 | 2008-08-18 00:00:00 | 54328.4697800926 | 2007-08-16 11:16:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502027010/ | Quick Look | ![]() |
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277 | VELA JR P12 | 132.2515 | -46.051 | 131.824752 | -45.864543 | 158.385677 | -59.866647 | 265.71195175 | -1.4410688 | 347.0011 | 54289.0722106482 | 2007-07-08 01:43:59 | 54289.4078009259 | 2007-07-08 09:47:14 | 502034010 | 9.9479 | 10 | 9.9479 | 9.9479 | 0 | 9.9479 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.494 | 10.494 | 28.9839 | 0 | PROCESSED | 57539.1227546296 | 2016-05-31 02:56:46 | 54696 | 2008-08-18 00:00:00 | 54328.4792939815 | 2007-08-16 11:30:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502034010/ | Quick Look | ![]() |
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278 | HE FOCUSING CONE | 49.5833 | 10.9603 | 48.902196 | 10.778547 | 50.105188 | -7.060313 | 170.9618047 | -37.8533007 | 73.6953 | 55410.7011921296 | 2010-08-02 16:49:43 | 55413.1439699074 | 2010-08-05 03:27:19 | 505061010 | 101.9651 | 100 | 101.9731 | 101.9731 | 0 | 101.9651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.1452 | 89.1452 | 211.0459 | 2 | PROCESSED | 57552.9158796296 | 2016-06-13 21:58:52 | 55808 | 2011-09-04 00:00:00 | 55441.4075694444 | 2010-09-02 09:46:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050129 | We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI YOSHITAKE | JAP | 5 | AO5 | OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505061010/ | Quick Look | ![]() |
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279 | VELA JR P17 | 133.087 | -46.0455 | 132.657371 | -45.856052 | 159.351353 | -59.55196 | 266.0760896 | -0.98967894 | 347.0002 | 54291.7369444444 | 2007-07-10 17:41:12 | 54291.9238773148 | 2007-07-10 22:10:23 | 502039010 | 13.0326 | 10 | 13.0645 | 13.0646 | 0 | 13.0326 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.8272 | 8.8272 | 16.1439 | 0 | PROCESSED | 57539.1455555556 | 2016-05-31 03:29:36 | 54707 | 2008-08-29 00:00:00 | 54333.4040277778 | 2007-08-21 09:41:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502039010/ | Quick Look | ![]() |
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280 | GC_G0.9+0.1 | 266.9332 | -28.1474 | 266.1438 | -28.130586 | 267.277369 | -4.735296 | 0.91503767 | 0.01290063 | 105.8953 | 54536.2637152778 | 2008-03-11 06:19:45 | 54540.229375 | 2008-03-15 05:30:18 | 502051010 | 138.7614 | 133 | 138.7614 | 138.7614 | 0 | 138.7614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122.2214 | 122.2214 | 342.5768 | 1 | PROCESSED | 57541.9299305556 | 2016-06-02 22:19:06 | 54919 | 2009-03-29 00:00:00 | 54550.6988078704 | 2008-03-25 16:46:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020071 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 2 | AO2 | SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502051010/ | Quick Look | ![]() |
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281 | M17 EAST | 275.3895 | -16.2062 | 274.668063 | -16.230609 | 275.205572 | 7.137102 | 15.15230897 | -0.92571433 | 271.9996 | 54377.3569907407 | 2007-10-04 08:34:04 | 54380.0940277778 | 2007-10-07 02:15:24 | 502052010 | 114.5695 | 107 | 114.5775 | 114.5695 | 0 | 114.5775 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100.8873 | 100.8873 | 236.4498 | 3 | PROCESSED | 57540.2317939815 | 2016-06-01 05:33:47 | 54771 | 2008-11-01 00:00:00 | 54403.5436111111 | 2007-10-30 13:02:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020085 | We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAHIRO TSUJIMOTO | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502052010/ | Quick Look | ![]() |
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282 | VELA JR P32 | 133.3695 | -46.8865 | 132.945153 | -46.696038 | 160.585523 | -60.152729 | 266.8467839 | -1.37881435 | 347.0018 | 54655.3279166667 | 2008-07-08 07:52:12 | 54655.5648032407 | 2008-07-08 13:33:19 | 503044010 | 11.2649 | 10 | 11.2729 | 11.2649 | 0 | 11.2809 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.3375 | 8.3375 | 20.4559 | 0 | PROCESSED | 57543.0006828704 | 2016-06-04 00:00:59 | 55048 | 2009-08-05 00:00:00 | 54679.381087963 | 2008-08-01 09:08:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503044010/ | Quick Look | ![]() |
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283 | COMET_8P_TUTTLE-P2_01 | 39.6412 | -35.6843 | 39.127956 | -35.899537 | 21.259605 | -47.847912 | 240.18300744 | -65.68930545 | 257.5577 | 54490.0082291667 | 2008-01-25 00:11:51 | 54490.1627083333 | 2008-01-25 03:54:18 | 502063010 | 4.3468 | 5 | 4.3468 | 4.3468 | 0 | 4.3468 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.4029 | 4.4029 | 13.3279 | 1 | PROCESSED | 57541.3739236111 | 2016-06-02 08:58:27 | 54912 | 2009-03-22 00:00:00 | 54546.0974189815 | 2008-03-21 02:20:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063010/ | Quick Look | ![]() |
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284 | COMET_8P_TUTTLE-P2_06 | 39.9457 | -36.3936 | 39.436659 | -36.607889 | 21.099638 | -48.591179 | 241.70384829 | -65.28238509 | 258.0349 | 54490.6963773148 | 2008-01-25 16:42:47 | 54490.8293287037 | 2008-01-25 19:54:14 | 502063060 | 6.6904 | 6.7 | 6.6906 | 6.6906 | 0 | 6.6904 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.338 | 4.338 | 11.4799 | 0 | PROCESSED | 57541.3927893518 | 2016-06-02 09:25:37 | 54912 | 2009-03-22 00:00:00 | 54546.1201736111 | 2008-03-21 02:53:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063060/ | Quick Look | ![]() |
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285 | G332.5-5.6 NE | 251.0925 | -54.3783 | 250.085838 | -54.28574 | 257.162856 | -31.775018 | 332.77088512 | -5.61037777 | 77.916 | 54504.4521296296 | 2008-02-08 10:51:04 | 54505.6669444444 | 2008-02-09 16:00:24 | 502067010 | 71.1926 | 80 | 71.2006 | 71.2086 | 0 | 71.1926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65.2508 | 65.2508 | 104.9418 | 0 | PROCESSED | 57541.5340277778 | 2016-06-02 12:49:00 | 54883 | 2009-02-21 00:00:00 | 54515.6965509259 | 2008-02-19 16:43:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | STEPHEN REYNOLDS | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502067010/ | Quick Look | ![]() |
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286 | GC_LARGEPROJECT6 | 266.2992 | -29.9408 | 265.498546 | -29.920884 | 266.763082 | -6.541223 | 359.09468885 | -0.44519015 | 265.9621 | 54723.8160532407 | 2008-09-14 19:35:07 | 54725.0348842593 | 2008-09-16 00:50:14 | 503012010 | 57.6855 | 50 | 57.6935 | 57.6855 | 0 | 57.6981 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.9032 | 51.9032 | 105.2878 | 1 | PROCESSED | 57543.8433217593 | 2016-06-04 20:14:23 | 54557 | 2008-04-01 00:00:00 | 54780.6521643518 | 2008-11-10 15:39:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503012010/ | Quick Look | ![]() |
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287 | HESS_J1825-137_3 | 276.1966 | -13.9971 | 275.486722 | -14.025442 | 276.082794 | 9.312755 | 17.46909054 | -0.57831059 | 271.0001 | 54758.195775463 | 2008-10-19 04:41:55 | 54759.7917476852 | 2008-10-20 19:00:07 | 503030010 | 55.4996 | 50 | 55.4996 | 55.4996 | 0 | 55.4996 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.3252 | 47.3252 | 137.8379 | 1 | PROCESSED | 57544.2257407407 | 2016-06-05 05:25:04 | 55148 | 2009-11-13 00:00:00 | 54780.7804050926 | 2008-11-10 18:43:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAAKI TANAKA | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503030010/ | Quick Look | ![]() |
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288 | HESS J1804-216 | 271.1693 | -21.6722 | 270.417896 | -21.676057 | 271.077547 | 1.764239 | 8.44223916 | -0.04647489 | 89.0483 | 53831.6120138889 | 2006-04-06 14:41:18 | 53832.4919328704 | 2006-04-07 11:48:23 | 500007010 | 37.5222 | 50 | 37.5222 | 37.5222 | 37.5222 | 37.5222 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.9336 | 28.9336 | 75.9901 | 0 | PROCESSED | 57533.4045138889 | 2016-05-25 09:42:30 | 54247 | 2007-05-27 00:00:00 | 54042.288900463 | 2006-11-03 06:56:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500007010/ | Quick Look | ![]() |
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289 | HESS J1804-216 BGD | 270.9564 | -22.0176 | 270.203045 | -22.020418 | 270.877317 | 1.420312 | 8.04431311 | -0.04388906 | 89.2004 | 53832.4925462963 | 2006-04-07 11:49:16 | 53833.454375 | 2006-04-08 10:54:18 | 500008010 | 40.7171 | 50 | 40.7171 | 40.7171 | 40.7171 | 40.7171 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.6429 | 30.6429 | 83.0879 | 1 | PROCESSED | 57533.4349537037 | 2016-05-25 10:26:20 | 54247 | 2007-05-27 00:00:00 | 54056.4266666667 | 2006-11-17 10:14:24 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500008010/ | Quick Look | ![]() |
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290 | RXJ_0852-4622_NW | 132.2926 | -45.6157 | 131.862494 | -45.429101 | 157.976747 | -59.482382 | 265.39238743 | -1.14402175 | 137.763 | 53723.4478240741 | 2005-12-19 10:44:52 | 53727.3016666667 | 2005-12-23 07:14:24 | 500010010 | 175.453 | 150 | 175.453 | 175.525 | 175.4608 | 175.461 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 230.0025 | 230.0025 | 332.9437 | 7 | PROCESSED | 57532.5654513889 | 2016-05-24 13:34:15 | 54247 | 2007-05-27 00:00:00 | 54059.902662037 | 2006-11-20 21:39:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010010/ | Quick Look | ![]() |
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291 | SMC DIFFUSE 1 | 13.0188 | -72.8206 | 12.579325 | -73.092182 | 312.037754 | -64.558836 | 302.86615918 | -44.30756989 | 221.6864 | 53687.4452893518 | 2005-11-13 10:41:13 | 53688.2231944445 | 2005-11-14 05:21:24 | 500011010 | 46.7789 | 50 | 46.7789 | 46.7869 | 46.7869 | 46.7869 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 47.8684 | 47.8684 | 67.1999 | 0 | PROCESSED | 57527.967337963 | 2016-05-19 23:12:58 | 54247 | 2007-05-27 00:00:00 | 54038.3531712963 | 2006-10-30 08:28:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001049 | We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | JAP | 0 | SWG | DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500011010/ | Quick Look | ![]() |
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292 | 73P/SW3 | 18.4857 | -9.3839 | 17.859598 | -9.648443 | 13.351737 | -15.906108 | 140.65827116 | -71.47693301 | 59.4008 | 53893.6903703704 | 2006-06-07 16:34:08 | 53893.7356365741 | 2006-06-07 17:39:19 | 500014010 | 3.228 | 35 | 3.228 | 3.228 | 3.228 | 3.228 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.312 | 3.312 | 3.9039 | 0 | PROCESSED | 57534.5195486111 | 2016-05-26 12:28:09 | 54267 | 2007-06-16 00:00:00 | 54052.5070949074 | 2006-11-13 12:10:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014010/ | Quick Look | ![]() |
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293 | 73P/SW3 | 18.2949 | -9.3163 | 17.668546 | -9.581131 | 13.199293 | -15.770045 | 140.03044964 | -71.46265703 | 59.3979 | 53894.3358101852 | 2006-06-08 08:03:34 | 53894.4022800926 | 2006-06-08 09:39:17 | 500014110 | 1.4249 | 35 | 1.4249 | 1.4249 | 1.4249 | 1.4249 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.433 | 1.433 | 5.742 | 0 | PROCESSED | 57534.5994444445 | 2016-05-26 14:23:12 | 54267 | 2007-06-16 00:00:00 | 54052.5225694444 | 2006-11-13 12:32:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014110/ | Quick Look | ![]() |
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294 | HESS J1800-240A | 270.4845 | -23.9659 | 269.719972 | -23.966397 | 270.433159 | -0.525758 | 6.13495239 | -0.62617494 | 86.9255 | 54558.6209606482 | 2008-04-02 14:54:11 | 54559.3266087963 | 2008-04-03 07:50:19 | 503025010 | 34.7822 | 30 | 34.7822 | 34.7902 | 0 | 34.7902 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7033 | 25.7033 | 60.9679 | 0 | PROCESSED | 57542.0259837963 | 2016-06-03 00:37:25 | 54953 | 2009-05-02 00:00:00 | 54574.0504861111 | 2008-04-18 01:12:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAAKI TANAKA | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503025010/ | Quick Look | ![]() |
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295 | HESS J1800-240C | 269.7173 | -24.0469 | 268.95232 | -24.043667 | 269.732245 | -0.606264 | 5.71665641 | -0.05804766 | 87.3071 | 54563.0147337963 | 2008-04-07 00:21:13 | 54563.6877662037 | 2008-04-07 16:30:23 | 503027010 | 30.9755 | 30 | 30.9755 | 30.9755 | 0 | 30.9755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.8155 | 27.8155 | 58.1239 | 1 | PROCESSED | 57542.2510185185 | 2016-06-03 06:01:28 | 54953 | 2009-05-02 00:00:00 | 54580.1897453704 | 2008-04-24 04:33:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAAKI TANAKA | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503027010/ | Quick Look | ![]() |
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296 | 73P/SW3 | 18.4874 | -9.3902 | 17.861309 | -9.65474 | 13.350771 | -15.912562 | 140.66879726 | -71.4825298 | 59.4036 | 53894.6018055556 | 2006-06-08 14:26:36 | 53894.680775463 | 2006-06-08 16:20:19 | 500014150 | 3.232 | 35 | 3.232 | 3.232 | 3.232 | 3.232 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3.293 | 3.293 | 6.8159 | 0 | PROCESSED | 57534.6057638889 | 2016-05-26 14:32:18 | 54267 | 2007-06-16 00:00:00 | 54052.5265509259 | 2006-11-13 12:38:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014150/ | Quick Look | ![]() |
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297 | VELA JR P23 | 132.7881 | -46.3947 | 132.362089 | -46.206312 | 159.378374 | -59.957558 | 266.21323714 | -1.3716571 | 347.0013 | 54652.3896759259 | 2008-07-05 09:21:08 | 54652.7710416667 | 2008-07-05 18:30:18 | 503035010 | 15.6901 | 10 | 15.6981 | 15.6901 | 0 | 15.7061 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.039 | 11.039 | 32.9439 | 1 | PROCESSED | 57542.9759490741 | 2016-06-03 23:25:22 | 55031 | 2009-07-19 00:00:00 | 54664.7904513889 | 2008-07-17 18:58:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503035010/ | Quick Look | ![]() |
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298 | VELA JR P35 | 132.966 | -46.9473 | 132.543542 | -46.75827 | 160.188354 | -60.35477 | 266.71715615 | -1.62954887 | 347.0008 | 54656.2642592593 | 2008-07-09 06:20:32 | 54656.5141087963 | 2008-07-09 12:20:19 | 503047010 | 11.5621 | 10 | 11.5861 | 11.5621 | 0 | 11.5941 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6198 | 9.6198 | 21.5839 | 0 | PROCESSED | 57543.0120486111 | 2016-06-04 00:17:21 | 55037 | 2009-07-25 00:00:00 | 54670.2319212963 | 2008-07-23 05:33:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503047010/ | Quick Look | ![]() |
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299 | CYGNUS LOOP NE3 | 313.7583 | 32.1826 | 313.244151 | 31.990973 | 329.188805 | 47.043725 | 75.71932756 | -8.27611719 | 222.9011 | 53703.7415162037 | 2005-11-29 17:47:47 | 53704.2355208333 | 2005-11-30 05:39:09 | 500022010 | 21.1338 | 20 | 21.1916 | 21.7199 | 21.1338 | 21.3599 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.2445 | 20.2445 | 42.6799 | 1 | PROCESSED | 57528.1127893518 | 2016-05-20 02:42:25 | 54247 | 2007-05-27 00:00:00 | 54038.7522106482 | 2006-10-30 18:03:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500022010/ | Quick Look | ![]() |
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300 | HIGH LAT. DIFFUSE A | 246.1745 | 43.4846 | 245.775383 | 43.597905 | 228.822222 | 63.555652 | 68.4171583 | 44.39202319 | 129.9994 | 53780.2926388889 | 2006-02-14 07:01:24 | 53781.9640509259 | 2006-02-15 23:08:14 | 500027010 | 73.5787 | 70 | 73.5867 | 73.5867 | 73.5787 | 73.5867 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67.3993 | 67.3993 | 144.3979 | 3 | PROCESSED | 57533.0379976852 | 2016-05-25 00:54:43 | 54247 | 2007-05-27 00:00:00 | 54041.3110416667 | 2006-11-02 07:27:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000044 | We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027010/ | Quick Look | ![]() |
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301 | 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 | ![]() |
302 | 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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303 | CYGNUS LOOP (P26) | 314.1252 | 30.3135 | 313.601346 | 30.1206 | 328.529731 | 45.204244 | 74.46090737 | -9.70687059 | 49.7995 | 54599.1203587963 | 2008-05-13 02:53:19 | 54599.5474421296 | 2008-05-13 13:08:19 | 503062010 | 16.9247 | 15 | 16.9247 | 16.9327 | 0 | 16.9327 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.441 | 15.441 | 36.892 | 1 | PROCESSED | 57542.5181944444 | 2016-06-03 12:26:12 | 54975 | 2009-05-24 00:00:00 | 54609.1293981482 | 2008-05-23 03:06:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503062010/ | Quick Look | ![]() |
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304 | 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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305 | 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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306 | 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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307 | CAS A | 351.0231 | 59.0265 | 350.456601 | 58.751794 | 27.744986 | 54.948342 | 111.88943817 | -1.95981315 | 208.1115 | 54876.0965740741 | 2009-02-14 02:19:04 | 54876.8363310185 | 2009-02-14 20:04:19 | 503080010 | 30.0355 | 30 | 30.0355 | 30.0355 | 0 | 30.0355 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0731 | 30.0731 | 63.9139 | 0 | PROCESSED | 57545.551087963 | 2016-06-06 13:13:34 | 55330 | 2010-05-14 00:00:00 | 54892.9889699074 | 2009-03-02 23:44:07 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030127 | Cas A is the youngest supernova remnant(SNR) in our Galaxy. Recently, the Spitzer Space Telescope discovered moving structures nearly at the speed of light outside the shell of the SNR. These structures are likely infrared echoes, where interstellar dust is heated by the outward moving photon shell of a bright flash. The bright flash is probably due to a giant flare from the central point source of Cas A, and if so, it requires that the central point source is a magnetar. Magnetars are known to emit luminous flares in the X-ray band, so it is expected that we can detect Fe-K fluorescence emission accompanied by IR echo. Here, we propose to observe on IR-emitting cloud around Cas A for 30ks to search for Fe-K emission which is naturally expected if the central point source is a magnetar. | GALACTIC DIFFUSE EMISSION | 5 | C | HIROYUKI AONO | JAP | 3 | AO3 | INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503080010/ | Quick Look | ![]() |
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308 | 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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309 | 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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310 | 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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311 | TYCHO SNR | 6.3139 | 64.1469 | 5.613879 | 63.870082 | 42.846574 | 53.765969 | 120.08177164 | 1.42013769 | 53.7834 | 54682.0646759259 | 2008-08-04 01:33:08 | 54686.9529398148 | 2008-08-08 22:52:14 | 503085010 | 312.892 | 400 | 312.916 | 312.892 | 0 | 312.908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 289.9494 | 289.9494 | 307.8699 | 3 | PROCESSED | 57543.3766782407 | 2016-06-04 09:02:25 | 54557 | 2008-04-01 00:00:00 | 54707.038287037 | 2008-08-29 00:55:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085010/ | Quick Look | ![]() |
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312 | 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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313 | 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 | ![]() |
314 | B1920+10(2) | 292.8971 | 10.8605 | 292.305399 | 10.753499 | 296.831046 | 32.19317 | 47.18977478 | -3.80874006 | 248.6642 | 54783.7420833333 | 2008-11-13 17:48:36 | 54785.8981365741 | 2008-11-15 21:33:19 | 503091010 | 100.4577 | 100 | 100.4577 | 100.4577 | 0 | 100.4577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.8731 | 93.8731 | 186.248 | 0 | PROCESSED | 57544.4390972222 | 2016-06-05 10:32:18 | 55167 | 2009-12-02 00:00:00 | 54797.1537731482 | 2008-11-27 03:41:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | ZDENKA MISANOVIC | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503091010/ | Quick Look | ![]() |
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315 | GCL4 | 265.3437 | -29.192 | 264.548064 | -29.167468 | 265.905576 | -5.816983 | 359.29532739 | 0.65531706 | 106.9407 | 54907.3257986111 | 2009-03-17 07:49:09 | 54908.0711111111 | 2009-03-18 01:42:24 | 503102010 | 33.6554 | 25 | 33.6794 | 33.6558 | 0 | 33.6554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0521 | 30.0521 | 64.3899 | 0 | PROCESSED | 57545.8492939815 | 2016-06-06 20:22:59 | 55329 | 2010-05-13 00:00:00 | 54920.054837963 | 2009-03-30 01:18:58 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503102010/ | Quick Look | ![]() |
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316 | HESS J1745-303 1 | 266.2249 | -30.1096 | 265.423171 | -30.089321 | 266.702778 | -6.71164 | 358.91712668 | -0.478438 | 70.5005 | 54527.7555555556 | 2008-03-02 18:08:00 | 54529.7363310185 | 2008-03-04 17:40:19 | 502016010 | 70.5291 | 67 | 70.5371 | 70.5291 | 0 | 70.5451 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.7932 | 61.7932 | 171.0959 | 3 | PROCESSED | 57541.8000810185 | 2016-06-02 19:12:07 | 54908 | 2009-03-18 00:00:00 | 54539.3190509259 | 2008-03-14 07:39:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502016010/ | Quick Look | ![]() |
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317 | ANTICENTER | 113.3357 | -19.5305 | 112.785719 | -19.421448 | 119.46206 | -40.613154 | 234.9976882 | 0.00424804 | 280.7829 | 54212.8606481482 | 2007-04-22 20:39:20 | 54215.4197222222 | 2007-04-25 10:04:24 | 502021010 | 89.5429 | 80 | 89.5509 | 89.5589 | 0 | 89.5429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.9887 | 78.9887 | 221.0508 | 3 | PROCESSED | 57538.5236689815 | 2016-05-30 12:34:05 | 54744 | 2008-10-05 00:00:00 | 54223.2040046296 | 2007-05-03 04:53:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020032 | We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. Absolute measurement of the O VII and O VIII line fluxes will help establish the origin of this mysterious component of the diffuse background. This will allow a search for spectral signatures of non-thermal emission, i.e. charge- exchange emission, in the 3/4 keV band and the determination of abundances in hot gas thermal emission without risk of confusion by emission from hot gas in the Galactic Bulge. | GALACTIC DIFFUSE EMISSION | 5 | B | KENSUKE MASUI | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502021010/ | Quick Look | ![]() |
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318 | VELA JR P1 | 131.9787 | -45.8064 | 131.551046 | -45.620931 | 157.807694 | -59.76004 | 265.40235777 | -1.43438498 | 347.0031 | 54285.3151273148 | 2007-07-04 07:33:47 | 54285.6904398148 | 2007-07-04 16:34:14 | 502023010 | 10.6496 | 10 | 10.6496 | 10.6576 | 0 | 10.6576 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.0446 | 9.0446 | 32.4199 | 0 | PROCESSED | 57539.086412037 | 2016-05-31 02:04:26 | 54696 | 2008-08-18 00:00:00 | 54328.4268402778 | 2007-08-16 10:14:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502023010/ | Quick Look | ![]() |
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319 | VELA JR P8 | 133.862 | -45.8612 | 133.428362 | -45.669016 | 160.04869 | -59.10729 | 266.28131071 | -0.45847751 | 347.0005 | 54287.3028240741 | 2007-07-06 07:16:04 | 54287.7009722222 | 2007-07-06 16:49:24 | 502030010 | 13.2196 | 10 | 13.2196 | 13.2196 | 0 | 13.2196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.441 | 14.441 | 34.3919 | 0 | PROCESSED | 57539.112662037 | 2016-05-31 02:42:14 | 54703 | 2008-08-25 00:00:00 | 54333.4507175926 | 2007-08-21 10:49:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502030010/ | Quick Look | ![]() |
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320 | VELA JR P13 | 131.851 | -46.106 | 131.426011 | -45.92099 | 157.974394 | -60.061119 | 265.57984888 | -1.69160478 | 347.0011 | 54290.1290162037 | 2007-07-09 03:05:47 | 54290.4411342593 | 2007-07-09 10:35:14 | 502035010 | 9.4089 | 10 | 9.4089 | 9.4089 | 0 | 9.4089 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.9531 | 8.9531 | 26.9639 | 0 | PROCESSED | 57539.1321412037 | 2016-05-31 03:10:17 | 54696 | 2008-08-18 00:00:00 | 54328.4906134259 | 2007-08-16 11:46:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502035010/ | Quick Look | ![]() |
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321 | SN1006 | 225.7268 | -41.9424 | 224.908794 | -41.746586 | 235.456683 | -23.661429 | 327.58003425 | 14.55159393 | 117.0193 | 54521.6264351852 | 2008-02-25 15:02:04 | 54526.8613310185 | 2008-03-01 20:40:19 | 502046010 | 211.7373 | 200 | 211.7453 | 211.7373 | 0 | 211.7453 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 184.3622 | 184.3622 | 417.2759 | 6 | PROCESSED | 57541.8622337963 | 2016-06-02 20:41:37 | 54904 | 2009-03-14 00:00:00 | 54535.729375 | 2008-03-10 17:30:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020052 | Thermal plasma incident SN1006 has very interesting characteristic. Suzaku PV spectrum revealed ionization parameter of the plasma is significantly low. We investigated the spatial variation of the ionization parameter, and found the outer region of SN1006 has lower ionization parameter than the inner region. However, since the center region of SN1006 is placed on the edge of FOV in the PV observation, the spectra have poor statistics, and the ionization state and the metal abundance cannot be decided with good precision. We propose to observe the center region of SN1006 deeply to decide the physical condition of the plasma of young SNR. Necessary exposure time is 150ksec. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | JAP | 2 | AO2 | THE CENTER REGION OF SN1006 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502046010/ | Quick Look | ![]() |
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322 | HESS J1702-420 | 255.6874 | -42.0709 | 254.803902 | -41.999975 | 258.786548 | -19.184424 | 344.26217794 | -0.21974248 | 106.4451 | 54550.458599537 | 2008-03-25 11:00:23 | 54555.625162037 | 2008-03-30 15:00:14 | 502049010 | 215.6932 | 200 | 215.7053 | 215.6932 | 0 | 215.7053 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140.6375 | 140.6375 | 395.7215 | 6 | PROCESSED | 57542.1678356482 | 2016-06-03 04:01:41 | 54933 | 2009-04-12 00:00:00 | 54566.9486458333 | 2008-04-10 22:46:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020067 | The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the most mysterious sample, HESS J1702-420, which has the brightest HESS compact source without clear counterparts. ASCA Galactic plane survey shows no evidence of X-ray emission although the exposure was too short. With the large effective area and the low background of XISs, we will be able to detect quite dim counterpart or make strong upper-limit in the hard X-ray band. This result will lead us to distinguish that HESS J1702-420 is the true "dark" protonic accelerator, or a hypothetical PWN powered by PSR J1702-4128. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 2 | AO2 | RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502049010/ | Quick Look | ![]() |
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323 | COMET_8P_TUTTLE-P1-6 | 28.2017 | 6.7525 | 27.54593 | 6.506397 | 28.607042 | -4.520684 | 148.82276905 | -53.00641332 | 248.5018 | 54470.8491666667 | 2008-01-05 20:22:48 | 54470.9154050926 | 2008-01-05 21:58:11 | 502062060 | 2.0266 | 2 | 2.0266 | 2.0266 | 0 | 2.0266 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.044 | 2.044 | 5.664 | 0 | PROCESSED | 57541.0007986111 | 2016-06-02 00:01:09 | 54908 | 2009-03-18 00:00:00 | 54542.2318634259 | 2008-03-17 05:33:53 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062060/ | Quick Look | ![]() |
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324 | COMET_8P_TUTTLE-P2_02 | 39.704 | -35.8295 | 39.191609 | -36.044542 | 21.228259 | -48.000366 | 240.49763907 | -65.60654763 | 257.6692 | 54490.1630902778 | 2008-01-25 03:54:51 | 54490.2960069444 | 2008-01-25 07:06:15 | 502063020 | 5.2049 | 5 | 5.2049 | 5.2049 | 0 | 5.2049 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.5919 | 5.5919 | 11.4499 | 0 | PROCESSED | 57541.3791898148 | 2016-06-02 09:06:02 | 54912 | 2009-03-22 00:00:00 | 54546.1091666667 | 2008-03-21 02:37:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063020/ | Quick Look | ![]() |
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325 | COMET_8P_TUTTLE-P2_07 | 40.0041 | -36.5319 | 39.495887 | -36.746007 | 21.066088 | -48.735556 | 241.99586619 | -65.20252382 | 258.1285 | 54490.8297106482 | 2008-01-25 19:54:47 | 54490.962662037 | 2008-01-25 23:06:14 | 502063070 | 5.2676 | 5 | 5.2916 | 5.2676 | 0 | 5.2994 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.753 | 2.753 | 11.4799 | 0 | PROCESSED | 57541.3952777778 | 2016-06-02 09:29:12 | 54912 | 2009-03-22 00:00:00 | 54546.130462963 | 2008-03-21 03:07:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063070/ | Quick Look | ![]() |
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326 | COMET_8P_TUTTLE-P2_BGD-2 | 40.4817 | -37.5941 | 39.980067 | -37.806706 | 20.824934 | -49.853115 | 244.17118034 | -64.55380496 | 254.4101 | 54492.5631365741 | 2008-01-27 13:30:55 | 54492.7293287037 | 2008-01-27 17:30:14 | 502064020 | 6.9797 | 5 | 6.9797 | 7.0037 | 0 | 6.9877 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.5471 | 5.5471 | 14.3519 | 0 | PROCESSED | 57554.5355671296 | 2016-06-15 12:51:13 | 54912 | 2009-03-22 00:00:00 | 54546.2537847222 | 2008-03-21 06:05:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064020/ | Quick Look | ![]() |
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327 | G21.5-0.9 | 278.4035 | -10.5067 | 277.711514 | -10.545731 | 278.460081 | 12.687392 | 21.56184596 | -0.8687642 | 103.5554 | 54188.7945023148 | 2007-03-29 19:04:05 | 54189.6252199074 | 2007-03-30 15:00:19 | 502065010 | 25.1416 | 100 | 25.156 | 25.1416 | 0 | 25.156 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 22.889 | 22.889 | 71.7699 | 1 | PROCESSED | 57538.0286921296 | 2016-05-30 00:41:19 | 54695 | 2008-08-17 00:00:00 | 54209.5181018518 | 2007-04-19 12:26:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | ILANA HARRUS | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065010/ | Quick Look | ![]() |
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328 | G296.1-0.5N | 177.8287 | -62.3875 | 177.210977 | -62.109277 | 215.982021 | -55.076396 | 296.02814016 | -0.3243747 | 322.3815 | 54321.2538541667 | 2007-08-09 06:05:33 | 54323.4522453704 | 2007-08-11 10:51:14 | 502068010 | 77.1759 | 67 | 77.1759 | 77.1759 | 0 | 77.1759 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.4846 | 68.4846 | 189.9237 | 1 | PROCESSED | 57539.4859953704 | 2016-05-31 11:39:50 | 54716 | 2008-09-07 00:00:00 | 54347.5137268518 | 2007-09-04 12:19:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | B | KAZIMIERZ BORKOWSKI | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502068010/ | Quick Look | ![]() |
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329 | GC CENTER #2 | 266.7693 | -28.6295 | 265.976908 | -28.611884 | 267.143281 | -5.22043 | 0.42794484 | -0.11339991 | 74.7707 | 53821.958587963 | 2006-03-27 23:00:22 | 53823.7585069444 | 2006-03-29 18:12:15 | 500005010 | 88.4247 | 100 | 88.4327 | 88.4247 | 88.4327 | 88.4327 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64.5911 | 64.5911 | 155.5019 | 2 | PROCESSED | 57533.3630324074 | 2016-05-25 08:42:46 | 54247 | 2007-05-27 00:00:00 | 54133.0079861111 | 2007-02-02 00:11:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001020 | We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 0 | SWG | SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1 | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500005010/ | Quick Look | ![]() |
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330 | HESS J1731-347 SW | 263.0074 | -34.9458 | 262.173825 | -34.909887 | 264.142527 | -11.646447 | 353.3803333 | -0.77058494 | 92.6086 | 55245.72 | 2010-02-18 17:16:48 | 55246.5231365741 | 2010-02-19 12:33:19 | 504031010 | 41.8615 | 40 | 41.8779 | 41.8615 | 0 | 41.8695 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.1028 | 34.1028 | 69.382 | 0 | PROCESSED | 57550.6419675926 | 2016-06-11 15:24:26 | 55623 | 2011-03-03 00:00:00 | 55257.0493981482 | 2010-03-02 01:11:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040026 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504031010/ | Quick Look | ![]() |
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331 | SNR 0049-73.6 | 12.7817 | -73.3677 | 12.345533 | -73.639533 | 310.812589 | -64.728588 | 302.96274339 | -43.76053264 | 62.7682 | 54629.4818518518 | 2008-06-12 11:33:52 | 54632.7605787037 | 2008-06-15 18:15:14 | 503094010 | 120.478 | 120 | 120.486 | 120.478 | 0 | 120.486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 107.7079 | 107.7079 | 283.2419 | 3 | PROCESSED | 57542.894525463 | 2016-06-03 21:28:07 | 55008 | 2009-06-26 00:00:00 | 54642.6050694444 | 2008-06-25 14:31:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031211 | We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6. | GALACTIC DIFFUSE EMISSION | 5 | B | SANGWOOK PARK | USA | 3 | AO3 | OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503094010/ | Quick Look | ![]() |
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332 | TORNADO | 265.1272 | -30.949 | 264.32027 | -30.923391 | 265.775878 | -7.579198 | 357.70572925 | -0.11631727 | 269.1137 | 55072.5037037037 | 2009-08-29 12:05:20 | 55075.0093055556 | 2009-09-01 00:13:24 | 504036010 | 125.0692 | 120 | 125.0692 | 125.0772 | 0 | 125.0772 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.0913 | 97.0913 | 216.4598 | 3 | PROCESSED | 57548.5178356482 | 2016-06-09 12:25:41 | 55454 | 2010-09-15 00:00:00 | 55088.3064814815 | 2009-09-14 07:21:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040076 | The Tornado is an unusual and intense radio source located in the galactic center region. It has a polarized non-thermal radio spectrum. t has very unique morphology of elongated and loop-like structure. However, no crucial observational result determining the nature has been obtained. With the Suzaku AO3 observation of the Tornado (50ks), we found interesting signs of 2.45-keV He like S-K line, diffuse emission from the "tail" and the whole "head". The purpose of this observation is to obtain precise spectrum and spatial distribution. If the thermal S-K line is confirmed and it has a high metal abundance, the nature of the Tornado is an SNR. We also investigate the extreme structure of the tail and search for power-law component in spectra. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 4 | AO4 | REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504036010/ | Quick Look | ![]() |
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333 | GC_LARGEPROJECT1 | 266.4387 | -28.5683 | 265.646756 | -28.549082 | 266.850456 | -5.166114 | 0.32941305 | 0.16640393 | 260.8767 | 54711.4273958333 | 2008-09-02 10:15:27 | 54712.9530555556 | 2008-09-03 22:52:24 | 503007010 | 52.1523 | 50 | 52.1523 | 52.1523 | 0 | 52.1523 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1838 | 44.1838 | 131.7938 | 2 | PROCESSED | 57543.7627546296 | 2016-06-04 18:18:22 | 54557 | 2008-04-01 00:00:00 | 54780.6858796296 | 2008-11-10 16:27:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503007010/ | Quick Look | ![]() |
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334 | GC_LARGEPROJECT11 | 264.7183 | -31.3859 | 263.908606 | -31.358306 | 265.438625 | -8.028238 | 357.14965021 | -0.05250387 | 268.3335 | 54732.3390046296 | 2008-09-23 08:08:10 | 54733.3897337963 | 2008-09-24 09:21:13 | 503017010 | 51.2865 | 50 | 51.2945 | 51.2865 | 0 | 51.3025 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.5834 | 48.5834 | 90.7759 | 2 | PROCESSED | 57543.9868287037 | 2016-06-04 23:41:02 | 54557 | 2008-04-01 00:00:00 | 54780.6941550926 | 2008-11-10 16:39:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503017010/ | Quick Look | ![]() |
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335 | LOOP 1 L=356.00 | 263.2426 | -31.9466 | 262.429689 | -31.911872 | 264.194275 | -8.641352 | 356.00010804 | 0.70279756 | 93.3363 | 54908.96625 | 2009-03-18 23:11:24 | 54909.8933333333 | 2009-03-19 21:26:24 | 503022010 | 41.3193 | 40 | 41.3193 | 41.3193 | 0 | 41.3193 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3187 | 34.3187 | 80.0699 | 0 | PROCESSED | 57545.8730671296 | 2016-06-06 20:57:13 | 55330 | 2010-05-14 00:00:00 | 54923.2640162037 | 2009-04-02 06:20:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030023 | NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. | GALACTIC DIFFUSE EMISSION | 5 | C | SHIGEO YAMAUCHI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503022010/ | Quick Look | ![]() |
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336 | LOOP 2 L=356.33 | 263.4562 | -31.667 | 262.645073 | -31.633306 | 264.364444 | -8.35361 | 356.33349006 | 0.70266893 | 94.2779 | 54916.2757060185 | 2009-03-26 06:37:01 | 54917.0786921296 | 2009-03-27 01:53:19 | 503023010 | 31.1527 | 40 | 31.1527 | 31.1527 | 0 | 31.1527 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.2346 | 28.2346 | 69.3699 | 0 | PROCESSED | 57545.9012615741 | 2016-06-06 21:37:49 | 55330 | 2010-05-14 00:00:00 | 54930.234849537 | 2009-04-09 05:38:11 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030023 | NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. | GALACTIC DIFFUSE EMISSION | 5 | C | SHIGEO YAMAUCHI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503023010/ | Quick Look | ![]() |
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337 | CYGNUS LOOP (P11) | 312.4425 | 31.5127 | 311.927752 | 31.32576 | 327.295676 | 46.874223 | 74.4826992 | -7.83027866 | 49.9999 | 54595.9014814815 | 2008-05-09 21:38:08 | 54596.7391087963 | 2008-05-10 17:44:19 | 503055010 | 31.8947 | 25 | 31.9027 | 31.8947 | 0 | 31.9107 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0738 | 25.0738 | 72.3599 | 0 | PROCESSED | 57542.4981712963 | 2016-06-03 11:57:22 | 54972 | 2009-05-21 00:00:00 | 54606.1436342593 | 2008-05-20 03:26:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503055010/ | Quick Look | ![]() |
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338 | ASO0449 | 299.6429 | 28.7759 | 299.134977 | 28.639283 | 310.497072 | 48.135601 | 65.87759933 | -0.32938525 | 56.1427 | 54974.6386921296 | 2009-05-23 15:19:43 | 54975.5786342593 | 2009-05-24 13:53:14 | 504044010 | 38.7337 | 20 | 38.7337 | 38.7417 | 0 | 38.7417 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.22 | 35.22 | 81.1999 | 2 | PROCESSED | 57546.6654050926 | 2016-06-07 15:58:11 | 55356 | 2010-06-09 00:00:00 | 54987.4424652778 | 2009-06-05 10:37:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504044010/ | Quick Look | ![]() |
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339 | ASO0447 | 298.557 | 28.6365 | 298.049709 | 28.504502 | 309.068665 | 48.278589 | 65.2636943 | 0.41202338 | 90.516 | 54928.7514699074 | 2009-04-07 18:02:07 | 54929.253587963 | 2009-04-08 06:05:10 | 504046010 | 20.5457 | 20 | 20.5457 | 20.5457 | 0 | 20.5457 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.9071 | 16.9071 | 43.3779 | 1 | PROCESSED | 57546.0447106482 | 2016-06-07 01:04:23 | 55324 | 2010-05-08 00:00:00 | 54949.4485300926 | 2009-04-28 10:45:53 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504046010/ | Quick Look | ![]() |
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340 | CYGNUS LOOP (P24) | 312.134 | 32.2905 | 311.623759 | 32.104666 | 327.393235 | 47.692301 | 74.93132331 | -7.14055521 | 61.3941 | 54621.1479513889 | 2008-06-04 03:33:03 | 54621.6271875 | 2008-06-04 15:03:09 | 503060010 | 18.5046 | 15 | 18.5046 | 18.5046 | 0 | 18.5046 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.999 | 14.999 | 41.3979 | 1 | PROCESSED | 57542.7234027778 | 2016-06-03 17:21:42 | 55003 | 2009-06-21 00:00:00 | 54637.4594675926 | 2008-06-20 11:01:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503060010/ | Quick Look | ![]() |
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341 | (L,B)=(0.107,-1.425) | 267.8602 | -29.5833 | 267.06157 | -29.570962 | 268.118883 | -6.156195 | 0.10035042 | -1.42140103 | 68.0986 | 55261.1636226852 | 2010-03-06 03:55:37 | 55263.893275463 | 2010-03-08 21:26:19 | 504050010 | 100.3991 | 100 | 100.4311 | 100.3991 | 0 | 100.4231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.536 | 80.536 | 235.8218 | 1 | PROCESSED | 57550.8323726852 | 2016-06-11 19:58:37 | 55645 | 2011-03-25 00:00:00 | 55278.4832523148 | 2010-03-23 11:35:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040109 | In order to resolve origin of the Galactic bulge/ridge emission, we propose to observe the blank field 1.5 deg from the Galactic center where Chandra recently performed the deepest exposure (900 ksec) aiming to resolve the Galactic "diffuse" emission into point sources. Goals of the present observation are the following: (1) Resolve the three iron emission lines (6.41 keV, 6.67 keV and 6.97 keV) with Suzaku, and compare with the point source population determined by Chandra to clarify what kinds of sources are responsible for which emission line. (2) Study Galactic latitudinal variation of the three emission lines comparing with the existent Suzaku observation at (l,b)=(0.0, -2.0). (3) Constrain the hard-tail emission above 10 keV, and study its Galactic latitudinal variation. | GALACTIC DIFFUSE EMISSION | 5 | B | KEN EBISAWA | JAP | 4 | AO4 | RESOLVING ORIGIN OF THE IRON EMISSION LINES FROM THE GALACTIC BULGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504050010/ | Quick Look | ![]() |
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342 | GC(0,-1.6) | 268.0544 | -29.7594 | 267.254612 | -29.748002 | 268.29113 | -6.329868 | 0.03481768 | -1.65633011 | 65.7488 | 54899.6540509259 | 2009-03-09 15:41:50 | 54900.8168865741 | 2009-03-10 19:36:19 | 503081010 | 59.2233 | 50 | 59.2233 | 59.2233 | 0 | 59.2233 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.6018 | 57.6018 | 100.4538 | 1 | PROCESSED | 57545.7843402778 | 2016-06-06 18:49:27 | 55330 | 2010-05-14 00:00:00 | 54916.3813194444 | 2009-03-26 09:09:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030131 | We propose a 50 ksec observation of very enigmatic diffuse structure at 1.6 degree south from the Galactic center. We first discovered this structure with ROSAT. Then with ASCA, we found that the spectrum exhibits thin thermal emission accompanied with a hard tail which may be nonthermal radiation from high energy electrons. These results imply presence of a strong shock in this region, possibly due to a jet from Sgr A*. The diffuse emission may be a fossil of the past activities. With the observation of Suzaku, we obtain the richest statistics ever achieved. Then we will reveal the shock front from the image, and verify the past activities of the massive blackhole. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI MURAKAMI | JAP | 3 | AO3 | NEW EVIDENCE OF THE PAST ACTIVITY IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503081010/ | Quick Look | ![]() |
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343 | TYCHO SNR | 6.3115 | 64.1447 | 5.611508 | 63.867881 | 42.842768 | 53.765034 | 120.08050675 | 1.41805528 | 43.1557 | 54689.3425578704 | 2008-08-11 08:13:17 | 54690.918275463 | 2008-08-12 22:02:19 | 503085020 | 102.8556 | 100 | 102.8556 | 102.8556 | 0 | 102.8556 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.9078 | 91.9078 | 136.1039 | 1 | PROCESSED | 57543.2895717593 | 2016-06-04 06:56:59 | 54557 | 2008-04-01 00:00:00 | 54706.7896412037 | 2008-08-28 18:57:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503085020/ | Quick Look | ![]() |
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344 | GCL1 | 265.1726 | -28.5274 | 264.381201 | -28.50205 | 265.733071 | -5.157711 | 359.7799359 | 1.13423351 | 69.7267 | 54900.8188425926 | 2009-03-10 19:39:08 | 54901.4557175926 | 2009-03-11 10:56:14 | 503099010 | 29.706 | 25 | 29.7241 | 29.722 | 0 | 29.706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.5649 | 30.5649 | 55.02 | 1 | PROCESSED | 57545.7841782407 | 2016-06-06 18:49:13 | 55329 | 2010-05-13 00:00:00 | 54916.3706828704 | 2009-03-26 08:53:47 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503099010/ | Quick Look | ![]() |
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345 | HESSJ1616_PSRJ1617 | 244.3756 | -50.9175 | 243.427641 | -50.794985 | 251.811911 | -29.080089 | 332.50297445 | -0.27465368 | 270.0711 | 55059.1110763889 | 2009-08-16 02:39:57 | 55060.8328009259 | 2009-08-17 19:59:14 | 504056010 | 65.8331 | 50 | 65.8891 | 65.8331 | 0 | 65.8971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.7504 | 41.7504 | 148.7258 | 0 | PROCESSED | 57548.1892708333 | 2016-06-09 04:32:33 | 55437 | 2010-08-29 00:00:00 | 55071.2513425926 | 2009-08-28 06:01:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040115 | HESSJ1616-508 is one of the most energetic unidentified TeV object. Previously, we showed that there is no clear X-ray counterpart to this object with a Suzaku observation, and hence we argued that the object is a real dark particle accelerator. However, there is a young energetic pulsar PSRJ1617-5055 10 arcmin away from HESSJ1616, and another possibility has been proposed that HESSJ1616 is an offset pulsar wind nebula (PWN) driven by the pulsar. If this possibility is correct, a powerful X-ray PWN should be observed as HESSJ1825-137, but such PWN has not been reported. The lack of the detection may be due to small sensitivity of Chandra and XMM-Newton for a diffuse hard X-ray emission. We propose to observe PSRJ1617 to see if there is an extended PWN around this pulsar. | GALACTIC DIFFUSE EMISSION | 5 | A | HIRONORI MATSUMOTO | JAP | 4 | AO4 | IS THE MOST ENERGETIC UNIDENTIFIED TEV OBJECT HESSJ1616-508 A PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504056010/ | Quick Look | ![]() |
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346 | SLX 1737-282 | 265.2352 | -28.3094 | 264.445148 | -28.284356 | 265.781005 | -4.938001 | 359.99405573 | 1.20298654 | 69.9745 | 54901.4562384259 | 2009-03-11 10:56:59 | 54901.8035648148 | 2009-03-11 19:17:08 | 503103010 | 18.316 | 10 | 18.3324 | 18.332 | 0 | 18.316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.3659 | 16.3659 | 30.0019 | 0 | PROCESSED | 57545.7980208333 | 2016-06-06 19:09:09 | 55329 | 2010-05-13 00:00:00 | 54916.9907638889 | 2009-03-26 23:46:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | C | FARHAD YUSEF-ZADEH | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503103010/ | Quick Look | ![]() |
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347 | HESS J1745-303C | 266.3881 | -30.6242 | 265.582985 | -30.604704 | 266.857963 | -7.222423 | 358.55151469 | -0.86700864 | 101.7444 | 55252.1897800926 | 2010-02-25 04:33:17 | 55253.3842476852 | 2010-02-26 09:13:19 | 504003010 | 50.9065 | 50 | 50.9145 | 50.9145 | 0 | 50.9065 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2708 | 41.2708 | 103.1878 | 3 | PROCESSED | 57550.7231365741 | 2016-06-11 17:21:19 | 55632 | 2011-03-12 00:00:00 | 55264.3901157407 | 2010-03-09 09:21:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504003010/ | Quick Look | ![]() |
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348 | TYCHO SNR | 6.3244 | 64.1507 | 5.624265 | 63.873888 | 42.856632 | 53.765731 | 120.08671326 | 1.42345384 | 81.1044 | 53913.439224537 | 2006-06-27 10:32:29 | 53915.6530555556 | 2006-06-29 15:40:24 | 500024010 | 101.1274 | 100 | 101.1434 | 101.1274 | 101.1434 | 101.1434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94.5123 | 94.5123 | 191.2068 | 3 | PROCESSED | 57534.8252199074 | 2016-05-26 19:48:19 | 54289 | 2007-07-08 00:00:00 | 54052.7199884259 | 2006-11-13 17:16:47 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500024010/ | Quick Look | ![]() |
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349 | NEP #3 | 270.0483 | 66.5696 | 270.04982 | 66.569341 | 34.92017 | 89.983512 | 96.39421541 | 29.79223028 | 188.0738 | 55180.9320949074 | 2009-12-15 22:22:13 | 55182.0557638889 | 2009-12-17 01:20:18 | 504074010 | 50.1769 | 50 | 50.1769 | 50.1769 | 0 | 50.1769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.3374 | 33.3374 | 97.0499 | 1 | PROCESSED | 57549.895162037 | 2016-06-10 21:29:02 | 54922 | 2009-04-01 00:00:00 | 55200.4707291667 | 2010-01-04 11:17:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504074010/ | Quick Look | ![]() |
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350 | HESS J1809-193E | 272.0013 | -19.5033 | 271.261943 | -19.51123 | 271.881238 | 3.92439 | 10.71539243 | 0.332309 | 270.1011 | 55085.7498148148 | 2009-09-11 17:59:44 | 55087.1564351852 | 2009-09-13 03:45:16 | 504079010 | 51.0289 | 50 | 51.0289 | 51.0289 | 0 | 51.0289 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8753 | 41.8753 | 121.5198 | 2 | PROCESSED | 57548.5914699074 | 2016-06-09 14:11:43 | 55465 | 2010-09-26 00:00:00 | 55098.3372337963 | 2009-09-24 08:05:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | OLEG KARGALTSEV | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504079010/ | Quick Look | ![]() |
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351 | G156.2+5.7 (NW2) | 74.4322 | 52.0607 | 73.448956 | 51.983713 | 79.105505 | 29.208158 | 155.84514532 | 5.68920631 | 266.0115 | 55258.7553587963 | 2010-03-03 18:07:43 | 55259.9821643518 | 2010-03-04 23:34:19 | 504081010 | 52.8646 | 50 | 52.8678 | 52.8678 | 0 | 52.8646 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.3866 | 49.3866 | 105.991 | 1 | PROCESSED | 57550.7899189815 | 2016-06-11 18:57:29 | 55689 | 2011-05-08 00:00:00 | 55322.3173842593 | 2010-05-06 07:37:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504081010/ | Quick Look | ![]() |
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352 | 330.2+1.0 | 240.2338 | -51.588 | 239.290439 | -51.447752 | 249.06097 | -30.286548 | 330.14009051 | 0.98414205 | 285.0002 | 55078.1480671296 | 2009-09-04 03:33:13 | 55080.8126736111 | 2009-09-06 19:30:15 | 504083010 | 127.7746 | 150 | 127.7826 | 127.7746 | 0 | 127.7746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112.8484 | 112.8484 | 230.1578 | 1 | PROCESSED | 57548.4938657407 | 2016-06-09 11:51:10 | 55455 | 2010-09-16 00:00:00 | 55089.3295949074 | 2009-09-15 07:54:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | GLENN ALLEN | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083010/ | Quick Look | ![]() |
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353 | 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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354 | SGR_B2 | 266.8776 | -28.4437 | 266.086356 | -28.426612 | 267.234654 | -5.032575 | 0.63615824 | -0.0985299 | 266.3663 | 55095.6093518518 | 2009-09-21 14:37:28 | 55096.0418287037 | 2009-09-22 01:00:14 | 504004010 | 10.0572 | 200 | 10.0572 | 10.0572 | 0 | 10.0572 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.4328 | 9.4328 | 37.3409 | 0 | PROCESSED | 57548.6152314815 | 2016-06-09 14:45:56 | 55476 | 2010-10-07 00:00:00 | 55110.2035763889 | 2009-10-06 04:53:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040002 | The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504004010/ | Quick Look | ![]() |
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355 | RIM4 | 311.4678 | 31.0131 | 310.952491 | 30.829697 | 325.890411 | 46.737501 | 73.56601773 | -7.48621797 | 246.0303 | 55155.1210763889 | 2009-11-20 02:54:21 | 55155.3579166667 | 2009-11-20 08:35:24 | 504008010 | 12.1025 | 10 | 12.1025 | 12.1185 | 0 | 12.1105 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.666 | 8.666 | 20.4559 | 0 | PROCESSED | 57549.475462963 | 2016-06-10 11:24:40 | 55534 | 2010-12-04 00:00:00 | 55166.425787037 | 2009-12-01 10:13:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504008010/ | Quick Look | ![]() |
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356 | NEP | 272.8227 | 66.0165 | 272.806643 | 66.002812 | 335.593486 | 88.746745 | 95.79277142 | 28.663354 | 126.3033 | 53776.2556944445 | 2006-02-10 06:08:12 | 53778.0836111111 | 2006-02-12 02:00:24 | 500026010 | 88.5082 | 80 | 88.5322 | 88.5082 | 88.5242 | 88.5322 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 83.6728 | 83.6728 | 157.902 | 0 | PROCESSED | 57532.9856481482 | 2016-05-24 23:39:20 | 54247 | 2007-05-27 00:00:00 | 54041.1403703704 | 2006-11-02 03:22:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000042 | We propose a second Suzaku observation of the NEP region in order to constrain the long-term and short-term valiability of OVII and OIVVV emission line intensities.Short-term variability detected in the first Suzaku observation implies existence of a charge-exchange component in oVIII linem suggesting solar wind and geo corona interaction. First purpose is to confirm this with the second observtaion.Secondly, to search a long-term variability. If it is observed, it will place a further constraints on the solar wind and interplanetary medium near the Earth. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | JAP | 0 | SWG | NEP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500026010/ | Quick Look | ![]() |
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357 | BLOWOUT6 | 311.7638 | 30.9468 | 311.247593 | 30.762319 | 326.194522 | 46.578638 | 73.67127235 | -7.72686898 | 241.7587 | 55165.8330787037 | 2009-11-30 19:59:38 | 55166.2883449074 | 2009-12-01 06:55:13 | 504016010 | 21 | 19 | 21.008 | 21.016 | 0 | 21 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.7129 | 17.7129 | 39.3279 | 0 | PROCESSED | 57549.644849537 | 2016-06-10 15:28:35 | 55547 | 2010-12-17 00:00:00 | 55181.2630324074 | 2009-12-16 06:18:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504016010/ | Quick Look | ![]() |
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358 | GALACTIC_BULGE2 | 267.5552 | -29.599 | 266.756514 | -29.585181 | 267.852413 | -6.176134 | 359.95115697 | -1.20153587 | 277.9812 | 55113.1708217593 | 2009-10-09 04:05:59 | 55114.5903472222 | 2009-10-10 14:10:06 | 504089010 | 55.2601 | 50 | 55.2671 | 55.2601 | 0 | 55.2736 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.226 | 40.226 | 122.6338 | 1 | PROCESSED | 57548.8316666667 | 2016-06-09 19:57:36 | 54922 | 2009-04-01 00:00:00 | 55131.3309953704 | 2009-10-27 07:56:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504089010/ | Quick Look | ![]() |
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359 | HESS J1427-608 | 216.9609 | -60.8505 | 216.024633 | -60.626609 | 237.709544 | -43.214788 | 314.40487303 | -0.14444396 | 90.5578 | 55209.5761458333 | 2010-01-13 13:49:39 | 55212.1891666667 | 2010-01-16 04:32:24 | 504034010 | 104.1379 | 100 | 104.1379 | 104.1379 | 0 | 104.1379 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.2611 | 71.2611 | 225.7378 | 1 | PROCESSED | 57550.2389930556 | 2016-06-11 05:44:09 | 55594 | 2011-02-02 00:00:00 | 55225.4958449074 | 2010-01-29 11:54:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040066 | Pulsar wind nebula (PWN) has began to be recognized as the best candidate of a large fraction of the HESS-unidentified (unID) sources. It could be true for some sources like HESS J1825-137, while other PWN candidates are sometimes listed simply because they satisfy one or two of the necessary conditions (e.g., there is an energetic pulsar nearby). We then propose a Suzaku observation of HESS J1427-608, which is the most ``unlike'' HESS-unID source to be a PWN. The advantage that we can safely exclude a PWN for its candidate allows us to identify the emission mechanism/origin of HESS J1427-608 more unambiguously compared to other unID sources. We request a 150 ks exposure to constrain the ratio between X-ray and TeV fluxes, which is a good measure of the emission mechanism of TeV sources. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 4 | AO4 | A SUZAKU OBSERVATION OF HESS J1427-608 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504034010/ | Quick Look | ![]() |
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360 | ASO0402 | 273.3436 | -12.7608 | 272.639832 | -12.775336 | 273.308329 | 10.641449 | 17.24676471 | 2.45193699 | 68.9842 | 55277.3929513889 | 2010-03-22 09:25:51 | 55277.9793287037 | 2010-03-22 23:30:14 | 504042010 | 25.7125 | 20 | 25.7125 | 25.7125 | 0 | 25.7125 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.0152 | 16.0152 | 50.6559 | 1 | PROCESSED | 57550.9498958333 | 2016-06-11 22:47:51 | 55784 | 2011-08-11 00:00:00 | 55417.0893865741 | 2010-08-09 02:08:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504042010/ | Quick Look | ![]() |
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361 | 73P/SW3 | 18.0599 | -9.2267 | 17.433228 | -9.491881 | 13.014248 | -15.596574 | 139.25333623 | -71.43625621 | 59.4006 | 53894.0025 | 2006-06-08 00:03:36 | 53894.0689699074 | 2006-06-08 01:39:19 | 500014060 | 3.235 | 35 | 3.235 | 3.235 | 3.235 | 3.235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.49 | 2.49 | 5.7359 | 0 | PROCESSED | 57534.5883796296 | 2016-05-26 14:07:16 | 54267 | 2007-06-16 00:00:00 | 54052.5346759259 | 2006-11-13 12:49:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014060/ | Quick Look | ![]() |
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362 | 73P/SW3 | 18.338 | -9.3332 | 17.711705 | -9.597966 | 13.233056 | -15.802283 | 140.17356876 | -71.46762322 | 59.3974 | 53894.4024768518 | 2006-06-08 09:39:34 | 53894.4682986111 | 2006-06-08 11:14:21 | 500014120 | 1.5551 | 35 | 1.5551 | 1.5551 | 1.5551 | 1.5551 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.566 | 1.566 | 5.682 | 0 | PROCESSED | 57534.5988773148 | 2016-05-26 14:22:23 | 54267 | 2007-06-16 00:00:00 | 54052.5441782407 | 2006-11-13 13:03:37 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014120/ | Quick Look | ![]() |
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363 | SN1006 SE | 225.8656 | -42.0517 | 225.046486 | -41.856364 | 235.600187 | -23.734349 | 327.61589547 | 14.40537 | 115.0022 | 53765.3759259259 | 2006-01-30 09:01:20 | 53766.487662037 | 2006-01-31 11:42:14 | 500016010 | 51.6076 | 50 | 51.6132 | 51.6212 | 51.6212 | 51.6076 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55.6704 | 55.6704 | 96.0399 | 2 | PROCESSED | 57532.8333564815 | 2016-05-24 20:00:02 | 54247 | 2007-05-27 00:00:00 | 54040.6484259259 | 2006-11-01 15:33:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | JOHN HUGHES | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500016010/ | Quick Look | ![]() |
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364 | SGR C | 266.1523 | -29.4673 | 265.354719 | -29.446679 | 266.622211 | -6.071258 | 359.43182832 | -0.08906822 | 82.0001 | 53786.5315393518 | 2006-02-20 12:45:25 | 53789.4515509259 | 2006-02-23 10:50:14 | 500018010 | 106.9219 | 100 | 106.9219 | 106.9219 | 106.9219 | 106.9219 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46.6069 | 46.6069 | 252.2778 | 2 | PROCESSED | 57533.0732175926 | 2016-05-25 01:45:26 | 54247 | 2007-05-27 00:00:00 | 54041.6109375 | 2006-11-02 14:39:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI MURAKAMI | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500018010/ | Quick Look | ![]() |
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365 | VICINITY OF NGC 4051 | 180.4686 | 44.1146 | 179.828661 | 44.392934 | 159.283243 | 39.862026 | 150.13143213 | 70.30340869 | 109.3717 | 55184.3459606482 | 2009-12-19 08:18:11 | 55186.5140509259 | 2009-12-21 12:20:14 | 504062010 | 89.6305 | 80 | 89.6385 | 89.6465 | 0 | 89.6305 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 37.0758 | 37.0758 | 187.2819 | 2 | PROCESSED | 57549.977337963 | 2016-06-10 23:27:22 | 55581 | 2011-01-20 00:00:00 | 55209.4570833333 | 2010-01-13 10:58:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040120 | The highly ionized absorption lines of OVII and OVII at z = 0 have been unambiguously detected toward the bright AGN NGC 4051 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII and OVIII emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | C | TOSHISHIGE HAGIHARA | JAP | 4 | AO4 | STUDY OF WARM-HOT GAS TOWARD NGC 4051 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504062010/ | Quick Look | ![]() |
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366 | W51NW | 290.6858 | 14.2133 | 290.110894 | 14.116258 | 294.988251 | 35.876885 | 49.11550833 | -0.31636783 | 105.4558 | 55283.4893634259 | 2010-03-28 11:44:41 | 55284.555 | 2010-03-29 13:19:12 | 504066010 | 44.1125 | 40 | 44.1205 | 44.1205 | 0 | 44.1125 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.8961 | 8.8961 | 92.0639 | 0 | PROCESSED | 57551.0258217593 | 2016-06-12 00:37:11 | 55671 | 2011-04-20 00:00:00 | 55302.5003240741 | 2010-04-16 12:00:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDEAKI KATAGIRI | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504066010/ | Quick Look | ![]() |
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367 | SEP #3 | 89.9578 | -66.5683 | 89.959755 | -66.568521 | 317.285609 | -89.984917 | 276.39273536 | -29.82821774 | 172.4885 | 55179.5059259259 | 2009-12-14 12:08:32 | 55180.9169444444 | 2009-12-15 22:00:24 | 504073010 | 44.408 | 50 | 44.408 | 44.416 | 0 | 44.416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8784 | 23.8784 | 121.9018 | 1 | PROCESSED | 57549.8504282407 | 2016-06-10 20:24:37 | 54922 | 2009-04-01 00:00:00 | 55200.462337963 | 2010-01-04 11:05:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504073010/ | Quick Look | ![]() |
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368 | 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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369 | G156.2+5.7 (E2) | 75.2673 | 51.6789 | 74.287315 | 51.605827 | 79.638917 | 28.767744 | 156.46612231 | 5.86221802 | 271.6298 | 55248.7736574074 | 2010-02-21 18:34:04 | 55250.0369675926 | 2010-02-23 00:53:14 | 504082010 | 50.3308 | 50 | 50.3468 | 50.3308 | 0 | 50.3468 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1424 | 46.1424 | 109.1379 | 0 | PROCESSED | 57550.6943865741 | 2016-06-11 16:39:55 | 55632 | 2011-03-12 00:00:00 | 55266.2981597222 | 2010-03-11 07:09:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504082010/ | Quick Look | ![]() |
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370 | 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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371 | KEPLER_BG_GE | 263.5353 | -20.2634 | 262.792573 | -20.230259 | 263.918925 | 3.041235 | 5.99742641 | 6.79731937 | 272.7609 | 55087.1593171296 | 2009-09-13 03:49:25 | 55088.3606365741 | 2009-09-14 08:39:19 | 504101010 | 46.9895 | 60 | 46.9895 | 46.9895 | 0 | 46.9895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8993 | 40.8993 | 103.786 | 0 | PROCESSED | 57548.5758564815 | 2016-06-09 13:49:14 | 54922 | 2009-04-01 00:00:00 | 55099.2516782407 | 2009-09-25 06:02:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101010/ | Quick Look | ![]() |
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372 | IC443 NORTHWEST | 93.9975 | 22.7552 | 93.240341 | 22.772771 | 93.68801 | -0.634546 | 188.75644855 | 2.86235674 | 91.4819 | 55456.3191435185 | 2010-09-17 07:39:34 | 55458.2829050926 | 2010-09-19 06:47:23 | 505001010 | 83.1917 | 80 | 83.1917 | 83.1917 | 0 | 83.1917 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.6786 | 69.6786 | 169.6457 | 2 | PROCESSED | 57553.4791087963 | 2016-06-14 11:29:55 | 55836 | 2011-10-02 00:00:00 | 55469.4041087963 | 2010-09-30 09:41:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050001 | Suzaku discovered the radiative recombination continua (RRC) of Si and S from the supernova remnant IC443. This new phenomenon (the RRC) would be due to either pre-ionization by X-ray flash of gamma-ray burst, or adiabatic cooling in a rarefied ambient medium, or yet-unknown process. In any case, the RRC have essential and new clues for the mechanisms, evolution and/or even the cosmic-ray acceleration of IC443. Spectra of the rim regions provide key information for the RRC origin. We thus propose the East and West periphery of IC443 for total 200 ksec. | GALACTIC DIFFUSE EMISSION | 5 | C | MIDORI OZAWA | JAP | 5 | AO5 | EXPLORING THE ORIGIN OF THE RADIATIVE RECOMBINATION CONTINUUM OF IC443 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505001010/ | Quick Look | ![]() |
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373 | 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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374 | CYGNUS LOOP 7 | 313.929 | 31.0152 | 313.408854 | 30.822982 | 328.70395 | 45.915608 | 74.90122685 | -9.13052292 | 81.814 | 55306.459212963 | 2010-04-20 11:01:16 | 55306.7974189815 | 2010-04-20 19:08:17 | 505015010 | 13.5918 | 12 | 13.5918 | 13.5998 | 0 | 13.5998 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.682 | 12.682 | 29.1959 | 0 | PROCESSED | 57551.269212963 | 2016-06-12 06:27:40 | 55287 | 2010-04-01 00:00:00 | 55393.2216203704 | 2010-07-16 05:19:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505015010/ | Quick Look | ![]() |
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375 | CYGNUS LOOP 14 | 313.0411 | 29.9656 | 312.517703 | 29.77653 | 327.111212 | 45.248773 | 73.58742167 | -9.19932348 | 67.2195 | 55334.4727893518 | 2010-05-18 11:20:49 | 55335.1146759259 | 2010-05-19 02:45:08 | 505022010 | 29.2512 | 29 | 29.2512 | 29.2512 | 0 | 29.2512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.7832 | 24.7832 | 55.4519 | 0 | PROCESSED | 57551.5599305556 | 2016-06-12 13:26:18 | 55287 | 2010-04-01 00:00:00 | 55348.0488888889 | 2010-06-01 01:10:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505022010/ | Quick Look | ![]() |
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376 | FVW319.8+0.3 | 225.913 | -58.2332 | 224.953134 | -58.037768 | 241.861071 | -39.018553 | 319.61922846 | 0.28881447 | 278.3756 | 55413.1563888889 | 2010-08-05 03:45:12 | 55413.9307291667 | 2010-08-05 22:20:15 | 505029010 | 51.384 | 50 | 51.4 | 51.384 | 0 | 51.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.416 | 45.416 | 66.8939 | 2 | PROCESSED | 57552.8424421296 | 2016-06-13 20:13:07 | 55793 | 2011-08-20 00:00:00 | 55427.1529976852 | 2010-08-19 03:40:19 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050010 | Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 5 | AO5 | SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505029010/ | Quick Look | ![]() |
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377 | 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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378 | L139_B-32 | 28.093 | 28.6837 | 27.38183 | 28.437322 | 36.368533 | 16.024453 | 138.75887563 | -32.3084393 | 253.9538 | 55569.4091319444 | 2011-01-08 09:49:09 | 55571.3188541667 | 2011-01-10 07:39:09 | 505044010 | 84.0041 | 80 | 84.0041 | 84.0041 | 0 | 84.0041 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.0377 | 79.0377 | 164.9839 | 0 | PROCESSED | 57600.6057175926 | 2016-07-31 14:32:14 | 55962 | 2012-02-05 00:00:00 | 55595.2037615741 | 2011-02-03 04:53:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050064 | Suzaku measurements of the large scale variation of the Halo emission surrounding our Galaxy are proposed. To minimize the local emission and absorption structure, we selected three pointings toward the anti-center region (l=140) of the Galactic latitude between-20 and -40. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIKO YAMASAKI | JAP | 5 | AO5 | STRUCTURE OF THE GALACTIC HALO EMISSION TOWARD THE ANTI-CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505044010/ | Quick Look | ![]() |
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379 | 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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380 | DEM L238 | 83.8177 | -70.5927 | 83.963728 | -70.62236 | 296.31824 | -85.384034 | 281.24911245 | -31.77318091 | 307.401 | 55308.023125 | 2010-04-22 00:33:18 | 55312.9730902778 | 2010-04-26 23:21:15 | 505063010 | 199.7795 | 200 | 199.7795 | 199.7795 | 0 | 199.7795 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 167.8355 | 167.8355 | 427.6297 | 5 | PROCESSED | 57551.4910069444 | 2016-06-12 11:47:03 | 55287 | 2010-04-01 00:00:00 | 55326.6889699074 | 2010-05-10 16:32:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | KAZIMIERZ BORKOWSKI | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505063010/ | Quick Look | ![]() |
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381 | THE KEPLER SNR | 262.6737 | -21.5073 | 261.92432 | -21.469989 | 263.173689 | 1.760317 | 4.50532186 | 6.80830692 | 272.2663 | 55475.6914583333 | 2010-10-06 16:35:42 | 55478.2863194445 | 2010-10-09 06:52:18 | 505092020 | 111.1941 | 620 | 111.1941 | 111.2021 | 0 | 111.2021 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.8413 | 99.8413 | 224.1437 | 2 | PROCESSED | 57553.7268402778 | 2016-06-14 17:26:39 | 55287 | 2010-04-01 00:00:00 | 55488.3311689815 | 2010-10-19 07:56:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092020/ | Quick Look | ![]() |
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382 | THE KEPLER SNR | 262.671 | -21.4826 | 261.921758 | -21.445276 | 263.169925 | 1.784856 | 4.5248811 | 6.82377384 | 98.1034 | 55628.0376736111 | 2011-03-08 00:54:15 | 55632.2696643518 | 2011-03-12 06:28:19 | 505092050 | 84.5913 | 100 | 84.5913 | 85.6632 | 0 | 85.7192 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 122.4881 | 122.4881 | 365.616 | 3 | PROCESSED | 57601.284537037 | 2016-08-01 06:49:44 | 55287 | 2010-04-01 00:00:00 | 55648.4964699074 | 2011-03-28 11:54:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092050/ | Quick Look | ![]() |
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383 | 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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384 | HB21 SOUTH | 311.2512 | 50.6016 | 310.86516 | 50.418766 | 342.682858 | 64.005982 | 88.85305014 | 4.80482025 | 105.492 | 55660.3542361111 | 2011-04-09 08:30:06 | 55662.8155208333 | 2011-04-11 19:34:21 | 506005010 | 132.363 | 150 | 132.371 | 132.371 | 0 | 132.363 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 141.7887 | 141.7887 | 212.6359 | 1 | PROCESSED | 57601.4958564815 | 2016-08-01 11:54:02 | 56159 | 2012-08-20 00:00:00 | 55677.2811342593 | 2011-04-26 06:44:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060011 | Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 6 | AO6 | ORIGIN OF OVER-IONIZATION OF SNR PLASMAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506005010/ | Quick Look | ![]() |
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385 | CYGNUS LOOP BLOWOUT2 | 312.4423 | 29.4154 | 311.917417 | 29.228478 | 326.132278 | 44.939266 | 72.82314938 | -9.13589092 | 78.1524 | 55687.8500578704 | 2011-05-06 20:24:05 | 55688.6488310185 | 2011-05-07 15:34:19 | 506012010 | 35.655 | 35 | 35.655 | 35.655 | 0 | 35.655 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.4815 | 31.4815 | 68.9821 | 0 | PROCESSED | 57601.9748263889 | 2016-08-01 23:23:45 | 56066 | 2012-05-19 00:00:00 | 55700.4593865741 | 2011-05-19 11:01:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506012010/ | Quick Look | ![]() |
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386 | 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 | ![]() |
387 | G272.2-3.2 | 136.7067 | -52.1223 | 136.311595 | -51.920282 | 170.81242 | -63.078479 | 272.22054405 | -3.18534238 | 101.7643 | 55877.9477777778 | 2011-11-12 22:44:48 | 55878.6272916667 | 2011-11-13 15:03:18 | 506060020 | 25.5265 | 20 | 25.5345 | 25.5345 | 0 | 25.5265 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.028 | 27.028 | 58.706 | 0 | PROCESSED | 57603.7829282407 | 2016-08-03 18:47:25 | 55652 | 2011-04-01 00:00:00 | 55895.0737962963 | 2011-11-30 01:46:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060020/ | Quick Look | ![]() |
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388 | CYGNUS LOOP BLOWOUT6 | 312.8964 | 28.9665 | 312.36858 | 28.777954 | 326.408889 | 44.373591 | 72.71699713 | -9.72555156 | 78.1534 | 55691.9894791667 | 2011-05-10 23:44:51 | 55692.7710069445 | 2011-05-11 18:30:15 | 506016010 | 36.3744 | 35 | 36.3744 | 36.3744 | 0 | 36.3744 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.7568 | 32.7568 | 67.5039 | 0 | PROCESSED | 57602.0240277778 | 2016-08-02 00:34:36 | 56068 | 2012-05-21 00:00:00 | 55701.1981828704 | 2011-05-20 04:45:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506016010/ | Quick Look | ![]() |
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389 | GC23 | 266.578 | -28.0524 | 265.789256 | -28.033865 | 266.960919 | -4.647397 | 0.83380185 | 0.3300796 | 262.2345 | 54386.7855208333 | 2007-10-13 18:51:09 | 54387.2294444444 | 2007-10-14 05:30:24 | 502011010 | 23.013 | 20 | 23.013 | 23.021 | 0 | 23.029 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.0712 | 22.0712 | 38.3199 | 2 | PROCESSED | 57540.2674305556 | 2016-06-01 06:25:06 | 54777 | 2008-11-07 00:00:00 | 54402.5316898148 | 2007-10-29 12:45:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502011010/ | Quick Look | ![]() |
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390 | G23.5+0.1 | 278.489 | -8.375 | 277.807565 | -8.414468 | 278.678732 | 14.810155 | 23.49243074 | 0.03918587 | 261.7121 | 55489.5657291667 | 2010-10-20 13:34:39 | 55491.0730439815 | 2010-10-22 01:45:11 | 505026010 | 48.9761 | 50 | 48.9761 | 48.9761 | 0 | 48.9761 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7884 | 43.7884 | 130.1919 | 0 | PROCESSED | 57553.8193981482 | 2016-06-14 19:39:56 | 55868 | 2011-11-03 00:00:00 | 55502.1887962963 | 2010-11-02 04:31:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050009 | ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. | GALACTIC DIFFUSE EMISSION | 5 | B | SHIGEO YAMAUCHI | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505026010/ | Quick Look | ![]() |
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391 | 3C 59 VICINITY 2 | 31.4351 | 28.9234 | 30.715452 | 28.684984 | 39.296603 | 15.198203 | 141.95387958 | -31.18906496 | 250.3 | 55952.5116435185 | 2012-01-26 12:16:46 | 55957.4238773148 | 2012-01-31 10:10:23 | 506025010 | 173.347 | 50 | 173.347 | 173.355 | 0 | 173.355 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 0.5479 | 0.5479 | 86.854 | 0 | PROCESSED | 57604.5146759259 | 2016-08-04 12:21:08 | 56526 | 2013-08-22 00:00:00 | 56167.6426388889 | 2012-08-28 15:25:24 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060067 | We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed. | GALACTIC DIFFUSE EMISSION | 5 | C | KAZUHIRO SAKAI | JAP | 6 | AO6 | STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506025010/ | Quick Look | ![]() |
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392 | VELA PWN E3 | 129.9962 | -45.3672 | 129.571682 | -45.189023 | 154.98711 | -60.107857 | 264.19786494 | -2.25193357 | 304.5033 | 55712.1335069444 | 2011-05-31 03:12:15 | 55712.4099305556 | 2011-05-31 09:50:18 | 506046010 | 14.1787 | 15 | 14.2027 | 14.1947 | 0 | 14.1787 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6599 | 12.6599 | 23.8759 | 0 | PROCESSED | 57602.1638078704 | 2016-08-02 03:55:53 | 56093 | 2012-06-15 00:00:00 | 55725.9978240741 | 2011-06-13 23:56:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506046010/ | Quick Look | ![]() |
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393 | RADIO_ARC_S_W | 266.7778 | -29.3674 | 265.980729 | -29.349813 | 267.167421 | -5.95796 | 359.8007683 | -0.50226251 | 267.1999 | 56200.9358101852 | 2012-09-30 22:27:34 | 56202.0120601852 | 2012-10-02 00:17:22 | 507018010 | 51.0807 | 50 | 51.1047 | 51.0967 | 0 | 51.0807 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49.115 | 49.115 | 92.9799 | 0 | PROCESSED | 57607.2580324074 | 2016-08-07 06:11:34 | 56592 | 2013-10-27 00:00:00 | 56226.6169675926 | 2012-10-26 14:48:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070016 | The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. | GALACTIC DIFFUSE EMISSION | 5 | A | SYUKYO RYU | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507018010/ | Quick Look | ![]() |
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394 | G290.1-0.8 | 165.7447 | -60.8884 | 165.228717 | -60.618807 | 206.73964 | -58.122992 | 290.11957377 | -0.7436408 | 293.2659 | 55737.4551388889 | 2011-06-25 10:55:24 | 55740.5883333333 | 2011-06-28 14:07:12 | 506061010 | 110.5931 | 110 | 110.6091 | 110.5931 | 0 | 110.6011 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.3596 | 99.3596 | 270.6596 | 4 | PROCESSED | 57602.4993634259 | 2016-08-02 11:59:05 | 55652 | 2011-04-01 00:00:00 | 55775.3693287037 | 2011-08-02 08:51:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506061010/ | Quick Look | ![]() |
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395 | FERMI_BUBBLE_N5 | 233.6225 | 8.0718 | 233.013762 | 8.238094 | 228.991173 | 26.481108 | 14.37791019 | 47.00724717 | 287.4992 | 56146.9871990741 | 2012-08-07 23:41:34 | 56147.4320949074 | 2012-08-08 10:22:13 | 507005010 | 21.7222 | 20 | 21.7222 | 21.7222 | 0 | 21.7222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.5559 | 19.5559 | 38.4299 | 1 | PROCESSED | 57606.7961921296 | 2016-08-06 19:06:31 | 56535 | 2013-08-31 00:00:00 | 56169.0806944444 | 2012-08-30 01:56:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507005010/ | Quick Look | ![]() |
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396 | FERMI_BUBBLE_S3 | 327.8758 | -46.7423 | 327.0753 | -46.977097 | 312.913491 | -31.549758 | 351.52788223 | -49.77060768 | 44.0052 | 56035.6752777778 | 2012-04-18 16:12:24 | 56036.133587963 | 2012-04-19 03:12:22 | 507011010 | 21.2336 | 20 | 21.2336 | 21.2336 | 0 | 21.2336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.914 | 20.914 | 39.596 | 0 | PROCESSED | 57605.205787037 | 2016-08-05 04:56:20 | 56420 | 2013-05-08 00:00:00 | 56049.1986458333 | 2012-05-02 04:46:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507011010/ | Quick Look | ![]() |
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397 | VELA JR P3 | 132.1192 | -45.6039 | 131.689583 | -45.417926 | 157.761308 | -59.536255 | 265.30669647 | -1.23070071 | 347.0044 | 54285.9040162037 | 2007-07-04 21:41:47 | 54286.1057175926 | 2007-07-05 02:32:14 | 502025010 | 10.298 | 10 | 10.298 | 10.298 | 0 | 10.298 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.726 | 6.726 | 17.4239 | 0 | PROCESSED | 57539.0955902778 | 2016-05-31 02:17:39 | 54696 | 2008-08-18 00:00:00 | 54328.4516782407 | 2007-08-16 10:50:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502025010/ | Quick Look | ![]() |
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398 | IC 443 | 94.3024 | 22.7479 | 93.545319 | 22.766949 | 93.9693 | -0.633748 | 188.89613959 | 3.10659531 | 258.9994 | 56388.2234837963 | 2013-04-06 05:21:49 | 56390.0835763889 | 2013-04-08 02:00:21 | 507015040 | 75.6427 | 300 | 75.6428 | 75.6427 | 0 | 75.6427 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 68.7284 | 68.7284 | 160.6759 | 1 | PROCESSED | 57611.01125 | 2016-08-11 00:16:12 | 56018 | 2012-04-01 00:00:00 | 56401.615775463 | 2013-04-19 14:46:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015040/ | Quick Look | ![]() |
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399 | VELA JR P11 | 132.5986 | -45.8258 | 132.169014 | -45.638098 | 158.553222 | -59.54754 | 265.69032827 | -1.11165473 | 347.0024 | 54288.2314236111 | 2007-07-07 05:33:15 | 54288.6112731482 | 2007-07-07 14:40:14 | 502033010 | 11.2833 | 10 | 11.2833 | 11.2833 | 0 | 11.2833 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2079 | 12.2079 | 32.7901 | 1 | PROCESSED | 57539.1206828704 | 2016-05-31 02:53:47 | 54696 | 2008-08-18 00:00:00 | 54328.4031944445 | 2007-08-16 09:40:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502033010/ | Quick Look | ![]() |
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400 | VELA JR P22 | 132.4428 | -46.6127 | 132.019624 | -46.425546 | 159.213685 | -60.269437 | 266.23093455 | -1.69368029 | 346.9992 | 54652.0565625 | 2008-07-05 01:21:27 | 54652.3891087963 | 2008-07-05 09:20:19 | 503034010 | 15.2643 | 10 | 15.2643 | 15.2709 | 0 | 15.2709 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9717 | 14.9717 | 28.728 | 0 | PROCESSED | 57542.966099537 | 2016-06-03 23:11:11 | 55036 | 2009-07-24 00:00:00 | 54670.1353125 | 2008-07-23 03:14:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503034010/ | Quick Look | ![]() |
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401 | HESSJ1507-622_OFFSET | 227.1815 | -62.1646 | 226.158724 | -61.973493 | 244.511164 | -42.456937 | 318.2247639 | -3.44071412 | 303.001 | 56183.9562268518 | 2012-09-13 22:56:58 | 56185.1042939815 | 2012-09-15 02:30:11 | 507026010 | 40.9122 | 40 | 40.9122 | 40.9418 | 0 | 40.9338 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.0336 | 38.0336 | 99.1798 | 1 | PROCESSED | 57607.0490162037 | 2016-08-07 01:10:35 | 56582 | 2013-10-17 00:00:00 | 56212.7288078704 | 2012-10-12 17:29:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070033 | HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator. | GALACTIC DIFFUSE EMISSION | 5 | B | YUKIKATSU TERADA | HIRONORI MATSUMOTO | JAP | 7 | AO7 | SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507026010/ | Quick Look | ![]() |
402 | VELA JR P18 | 133.5064 | -46.0415 | 133.075299 | -45.850566 | 159.830487 | -59.392209 | 266.25968404 | -0.76370949 | 347.0006 | 54291.9244444444 | 2007-07-10 22:11:12 | 54292.1668634259 | 2007-07-11 04:00:17 | 502040010 | 15.0123 | 10 | 15.0123 | 15.0362 | 0 | 15.0203 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.8952 | 12.8952 | 20.9439 | 1 | PROCESSED | 57539.1482407407 | 2016-05-31 03:33:28 | 54696 | 2008-08-18 00:00:00 | 54328.4716666667 | 2007-08-16 11:19:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502040010/ | Quick Look | ![]() |
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403 | LOW_LATITUDE_86-21 | 332.3169 | 30.2173 | 331.751825 | 29.971433 | 347.602182 | 38.425077 | 86.0039952 | -20.78963339 | 82.7457 | 54229.0809259259 | 2007-05-09 01:56:32 | 54230.9966898148 | 2007-05-10 23:55:14 | 502047010 | 81.5486 | 80 | 81.5486 | 81.5486 | 0 | 81.5486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.2931 | 72.2931 | 165.5099 | 2 | PROCESSED | 57538.6557986111 | 2016-05-30 15:44:21 | 54744 | 2008-10-05 00:00:00 | 54244.7948032407 | 2007-05-24 19:04:31 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020061 | High galactic-latitude Suzaku observations of soft X-ray diffuse emission so far made show general tendency that the OVII emission line becomes stronger with decreasing abs(b). This suggests that the major part of the emission is originating from the halo of our galaxy. However, we cannot rule out the possibility that the data is contaminated by solar wind charge exchange emission from the entire heliosphere. In oder to confirm the abs(b) dependency and to constrain the spatial distribution of the halo emission, we propose to observe diffuse radiation at a low galactic latitude of abs(b) ~ 20 deg, where the galactic absorption still does not affect the line intensity significantly. | GALACTIC DIFFUSE EMISSION | 5 | B | TOMOTAKA YOSHINO | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502047010/ | Quick Look | ![]() |
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404 | HESS J1457-593 | 224.4524 | -59.4762 | 223.48511 | -59.275761 | 241.535779 | -40.451289 | 318.36335314 | -0.44487967 | 305.8997 | 56185.1060185185 | 2012-09-15 02:32:40 | 56186.0216782407 | 2012-09-16 00:31:13 | 507027010 | 31.0479 | 30 | 31.0479 | 31.0479 | 0 | 31.0479 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.0994 | 28.0994 | 79.1059 | 1 | PROCESSED | 57607.0753819445 | 2016-08-07 01:48:33 | 56584 | 2013-10-19 00:00:00 | 56218.5178009259 | 2012-10-18 12:25:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070037 | We propose an X-ray observation of the putative SNR-molecular cloud interaction HESS J1457-593 with the Suzaku XIS detector for 30 ks. The aim of the observation is to clarify whether the TeV gamma-ray emission is of a leptonic or hadronic origin by searching for an X-ray counterpart to a level down to $10^{-14}$~erg cm$^{-2}$ s$^{-1}$. A non-detection of an X-ray nebula would strongly disfavor a leptonic origin of the TeV emission and add to the already strong multi-wavelength data which all suggests a hadronic origin of the emission. Since the spectrum of this unique source extends above many tens of TeV this would mean that we see, for the first time, evidence for hadronic cosmic rays being accelerated up to PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROKAZU ODAKA | JAP | 7 | AO7 | INVESTIGATING A PUTATIVE COSMIC-RAY PEVATRON WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507027010/ | Quick Look | ![]() |
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405 | G298.6-0.0 | 183.3899 | -62.6356 | 182.720759 | -62.35751 | 219.490154 | -53.509251 | 298.59488766 | -0.08324812 | 319.8129 | 56150.8519097222 | 2012-08-11 20:26:45 | 56152.08625 | 2012-08-13 02:04:12 | 507037010 | 17.2388 | 50 | 17.2388 | 17.2388 | 0 | 17.2388 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.1746 | 19.1746 | 106.616 | 0 | PROCESSED | 57606.8422222222 | 2016-08-06 20:12:48 | 56721 | 2014-03-05 00:00:00 | 56291.7215162037 | 2012-12-30 17:18:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507037010/ | Quick Look | ![]() |
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406 | CYG_COCOON | 306.8026 | 40.9389 | 306.35518 | 40.773009 | 326.953221 | 57.33325 | 79.25133167 | 1.48664873 | 218.8996 | 56279.1800231482 | 2012-12-18 04:19:14 | 56280.1654976852 | 2012-12-19 03:58:19 | 507040010 | 51.0724 | 50 | 51.0724 | 51.0936 | 0 | 51.0804 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7833 | 42.7833 | 85.1439 | 0 | PROCESSED | 57608.3232291667 | 2016-08-08 07:45:27 | 56683 | 2014-01-26 00:00:00 | 56316.5705324074 | 2013-01-24 13:41:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070060 | The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507040010/ | Quick Look | ![]() |
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407 | SNR HB3 SE-B | 35.7593 | 62.192 | 34.815236 | 61.964819 | 57.837975 | 44.676486 | 133.39304715 | 1.19520932 | 247.4986 | 56323.4084259259 | 2013-01-31 09:48:08 | 56323.7710532407 | 2013-01-31 18:30:19 | 507057010 | 25.8366 | 20 | 25.8446 | 25.8366 | 0 | 25.8526 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.3092 | 19.3092 | 31.3279 | 1 | PROCESSED | 57608.6657638889 | 2016-08-08 15:58:42 | 56711 | 2014-02-23 00:00:00 | 56345.4750462963 | 2013-02-22 11:24:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNICHIRO KATSUTA | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507057010/ | Quick Look | ![]() |
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408 | SNR HB3 SE-C | 36.0358 | 62.4578 | 35.086232 | 62.23139 | 58.169094 | 44.855041 | 133.42083063 | 1.4890972 | 247.4994 | 56323.7716666667 | 2013-01-31 18:31:12 | 56324.1585532407 | 2013-02-01 03:48:19 | 507058010 | 24.142 | 20 | 24.1616 | 24.142 | 0 | 24.1696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.4547 | 23.4547 | 33.4239 | 0 | PROCESSED | 57608.6786342593 | 2016-08-08 16:17:14 | 56711 | 2014-02-23 00:00:00 | 56345.4779976852 | 2013-02-22 11:28:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNICHIRO KATSUTA | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507058010/ | Quick Look | ![]() |
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409 | COMET_8P_TUTTLE-P1-10 | 28.408 | 5.7525 | 27.75444 | 5.506869 | 28.446793 | -5.529035 | 149.8061723 | -53.84230192 | 248.5015 | 54471.1158333333 | 2008-01-06 02:46:48 | 54471.1820717593 | 2008-01-06 04:22:11 | 502062100 | 3.2196 | 3.2 | 3.2196 | 3.2196 | 0 | 3.2196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.166 | 2.166 | 5.6799 | 0 | PROCESSED | 57541.2676967593 | 2016-06-02 06:25:29 | 54908 | 2009-03-18 00:00:00 | 54542.2429513889 | 2008-03-17 05:49:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062100/ | Quick Look | ![]() |
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410 | G278.0+12.4 | 158.151 | -43.7043 | 157.610146 | -43.446336 | 182.388463 | -47.807278 | 278.01040448 | 12.3478226 | 304.0284 | 56102.6152199074 | 2012-06-24 14:45:55 | 56102.9842476852 | 2012-06-24 23:37:19 | 507067010 | 18.996 | 17.5 | 19.004 | 18.996 | 0 | 19.004 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.442 | 16.442 | 31.8799 | 0 | PROCESSED | 57605.7438078704 | 2016-08-05 17:51:05 | 56582 | 2013-10-17 00:00:00 | 56219.6572916667 | 2012-10-19 15:46:30 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | TOBIAS PRINZ | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507067010/ | Quick Look | ![]() |
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411 | GRXE_E_4 | 267.9068 | -26.8159 | 267.125467 | -26.803832 | 268.119163 | -3.388548 | 2.50111874 | -0.04382328 | 104.4995 | 56371.1118518518 | 2013-03-20 02:41:04 | 56373.3049421296 | 2013-03-22 07:19:07 | 507071010 | 101.2086 | 100 | 101.2166 | 101.2086 | 0 | 101.2166 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105.6491 | 105.6491 | 189.4519 | 1 | PROCESSED | 57610.9065625 | 2016-08-10 21:45:27 | 56018 | 2012-04-01 00:00:00 | 56384.6094560185 | 2013-04-02 14:37:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507071010/ | Quick Look | ![]() |
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412 | COMET_8P_TUTTLE-P2_09 | 40.126 | -36.804 | 39.619449 | -37.017725 | 21.006365 | -49.022029 | 242.56232387 | -65.03879756 | 253.3121 | 54491.0963773148 | 2008-01-26 02:18:47 | 54491.2292824074 | 2008-01-26 05:30:10 | 502063090 | 4.3979 | 4 | 4.3979 | 4.3979 | 0 | 4.3979 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.752 | 4.752 | 11.4439 | 0 | PROCESSED | 57541.402662037 | 2016-06-02 09:39:50 | 54912 | 2009-03-22 00:00:00 | 54546.2142592593 | 2008-03-21 05:08:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063090/ | Quick Look | ![]() |
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413 | W44_NORTH | 283.9599 | 1.4928 | 283.326032 | 1.427124 | 285.320102 | 24.193967 | 34.76225024 | -0.29835298 | 254.9998 | 56584.8902083333 | 2013-10-19 21:21:54 | 56586.2084837963 | 2013-10-21 05:00:13 | 508005010 | 55.6459 | 60 | 55.7019 | 55.6459 | 0 | 55.7008 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 47.4531 | 47.4531 | 113.8958 | 1 | PROCESSED | 57613.0578356482 | 2016-08-13 01:23:17 | 56967 | 2014-11-06 00:00:00 | 56597.6717824074 | 2013-11-01 16:07:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508005010/ | Quick Look | ![]() |
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414 | HESS J1534-571 4 | 233.6872 | -56.8979 | 232.705572 | -56.731059 | 246.296725 | -36.40404 | 323.85352453 | -0.81317458 | 295.9989 | 56545.1801157407 | 2013-09-10 04:19:22 | 56545.8042708333 | 2013-09-10 19:18:09 | 508016010 | 42.1696 | 40 | 42.1696 | 42.1936 | 0 | 42.1776 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.9419 | 39.9419 | 53.9199 | 0 | PROCESSED | 57612.5878587963 | 2016-08-12 14:06:31 | 56990 | 2014-11-29 00:00:00 | 56625.6134953704 | 2013-11-29 14:43:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508016010/ | Quick Look | ![]() |
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415 | G355.6-0.0 | 263.7798 | -32.6083 | 262.962219 | -32.576152 | 264.68406 | -9.281685 | 355.69106204 | -0.03789327 | 90.0013 | 55246.5249074074 | 2010-02-19 12:35:52 | 55247.6293287037 | 2010-02-20 15:06:14 | 504098010 | 52.5044 | 50 | 52.5275 | 52.5204 | 0 | 52.5044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.7346 | 43.7346 | 95.4118 | 0 | PROCESSED | 57550.6569560185 | 2016-06-11 15:46:01 | 54922 | 2009-04-01 00:00:00 | 55257.1119444444 | 2010-03-02 02:41:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504098010/ | Quick Look | ![]() |
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416 | G21.5-0.9 | 278.4038 | -10.5066 | 277.711815 | -10.545632 | 278.460388 | 12.687474 | 21.56207071 | -0.86897985 | 103.5553 | 54190.0674074074 | 2007-03-31 01:37:04 | 54191.7405671296 | 2007-04-01 17:46:25 | 502065020 | 53.5261 | 100 | 53.5261 | 53.551 | 0 | 53.5661 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 48.618 | 48.618 | 144.5418 | 0 | PROCESSED | 57538.0817013889 | 2016-05-30 01:57:39 | 54695 | 2008-08-17 00:00:00 | 54200.5054861111 | 2007-04-10 12:07:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | ILANA HARRUS | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502065020/ | Quick Look | ![]() |
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417 | JUPITER | 103.7993 | 23.1163 | 103.042955 | 23.180911 | 102.674134 | 0.280458 | 192.50244401 | 11.09547038 | 264.3793 | 56762.0858912037 | 2014-04-15 02:03:41 | 56762.3890277778 | 2014-04-15 09:20:12 | 508023010 | 13.0905 | 160 | 13.0905 | 13.0905 | 0 | 13.0905 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.005 | 13.005 | 26.1839 | 0 | PROCESSED | 57614.2446527778 | 2016-08-14 05:52:18 | 57212 | 2015-07-09 00:00:00 | 56778.6117708333 | 2014-05-01 14:40:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023010/ | Quick Look | ![]() |
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418 | JUPITER | 104.0402 | 23.0972 | 103.284076 | 23.16295 | 102.896521 | 0.28265 | 192.61518388 | 11.28841687 | 264.4641 | 56764.0628125 | 2014-04-17 01:30:27 | 56764.1911805556 | 2014-04-17 04:35:18 | 508023070 | 4.5577 | 160 | 4.5577 | 4.5577 | 0 | 4.5737 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9502777778 | 2016-08-14 22:48:24 | 57212 | 2015-07-09 00:00:00 | 56782.4904976852 | 2014-05-05 11:46:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023070/ | Quick Look | ![]() |
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419 | JUPITER | 104.5088 | 23.0594 | 103.753114 | 23.127361 | 103.329251 | 0.287317 | 192.8346306 | 11.66394816 | 267.1301 | 56767.4497106482 | 2014-04-20 10:47:35 | 56767.7814583333 | 2014-04-20 18:45:18 | 508023120 | 11.1894 | 160 | 11.1894 | 11.1961 | 0 | 11.1974 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.962974537 | 2016-08-14 23:06:41 | 57212 | 2015-07-09 00:00:00 | 56789.8021759259 | 2014-05-12 19:15:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023120/ | Quick Look | ![]() |
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420 | RCW86_SE | 221.3859 | -62.671 | 220.394052 | -62.460463 | 241.394031 | -43.97094 | 315.61056381 | -2.64231092 | 96.79 | 54863.365787037 | 2009-02-01 08:46:44 | 54864.7550115741 | 2009-02-02 18:07:13 | 503004010 | 53.3274 | 50 | 53.3594 | 53.3274 | 0 | 53.3594 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.8136 | 47.8136 | 119.9879 | 0 | PROCESSED | 57545.4381481482 | 2016-06-06 10:30:56 | 55329 | 2010-05-13 00:00:00 | 54880.5420138889 | 2009-02-18 13:00:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503004010/ | Quick Look | ![]() |
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421 | GC_LARGEPROJECT4 | 266.0398 | -29.5556 | 265.241679 | -29.534433 | 266.526203 | -6.162189 | 359.30535174 | -0.05184233 | 261.05 | 54715.6640393518 | 2008-09-06 15:56:13 | 54717.0690277778 | 2008-09-08 01:39:24 | 503010010 | 53.1056 | 50 | 53.1216 | 53.1056 | 0 | 53.1136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.0646 | 37.0646 | 121.366 | 1 | PROCESSED | 57543.7725694444 | 2016-06-04 18:32:30 | 54557 | 2008-04-01 00:00:00 | 54780.6585648148 | 2008-11-10 15:48:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503010010/ | Quick Look | ![]() |
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422 | VELA PWN W2 | 127.3498 | -45.1919 | 126.932022 | -45.023781 | 151.542711 | -60.896813 | 262.94388066 | -3.64107383 | 303.5006 | 56439.0351851852 | 2013-05-27 00:50:40 | 56439.4696643518 | 2013-05-27 11:16:19 | 508043010 | 19.5844 | 15 | 19.5924 | 19.5844 | 0 | 19.6004 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.6266 | 15.6266 | 37.5339 | 1 | PROCESSED | 57611.391875 | 2016-08-11 09:24:18 | 56816 | 2014-06-08 00:00:00 | 56450.7935532407 | 2013-06-07 19:02:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508043010/ | Quick Look | ![]() |
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423 | GC_LARGEPROJECT10 | 264.8736 | -31.1751 | 264.065254 | -31.148261 | 265.564785 | -7.81275 | 357.39875369 | -0.05245192 | 268.5898 | 54731.2832060185 | 2008-09-22 06:47:49 | 54732.3383912037 | 2008-09-23 08:07:17 | 503016010 | 52.1712 | 50 | 52.1712 | 52.1792 | 0 | 52.1792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.2913 | 49.2913 | 91.1639 | 1 | PROCESSED | 57543.9863425926 | 2016-06-04 23:40:20 | 54557 | 2008-04-01 00:00:00 | 54780.6078935185 | 2008-11-10 14:35:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503016010/ | Quick Look | ![]() |
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424 | VELA PWN W3 | 126.9052 | -45.2087 | 126.488861 | -45.042306 | 150.998783 | -61.06652 | 262.77480933 | -3.90558145 | 95.0008 | 56590.9784606482 | 2013-10-25 23:28:59 | 56591.4343055556 | 2013-10-26 10:25:24 | 508044010 | 13.871 | 15 | 13.871 | 13.871 | 0 | 13.871 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.3448 | 11.3448 | 39.3799 | 1 | PROCESSED | 57613.1197106482 | 2016-08-13 02:52:23 | 57009 | 2014-12-18 00:00:00 | 56643.6595949074 | 2013-12-17 15:49:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508044010/ | Quick Look | ![]() |
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425 | GC_LARGEPROJECT15 | 265.2338 | -30.2129 | 264.431646 | -30.187819 | 265.84334 | -6.840443 | 358.37855715 | 0.19604348 | 267.777 | 54743.1555902778 | 2008-10-04 03:44:03 | 54744.4565277778 | 2008-10-05 10:57:24 | 503021010 | 53.826 | 50 | 53.834 | 53.834 | 0 | 53.826 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.6405 | 49.6405 | 112.3781 | 0 | PROCESSED | 57544.0429861111 | 2016-06-05 01:01:54 | 54557 | 2008-04-01 00:00:00 | 54780.430150463 | 2008-11-10 10:19:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503021010/ | Quick Look | ![]() |
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426 | SGR A | 266.5133 | -28.9285 | 265.71907 | -28.909638 | 266.925006 | -5.524591 | 0.05589981 | -0.0769322 | 266.9997 | 56555.4484490741 | 2013-09-20 10:45:46 | 56556.6446875 | 2013-09-21 15:28:21 | 508064010 | 50.4569 | 50 | 50.4569 | 50.4569 | 0 | 50.4569 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.2248 | 45.2248 | 103.308 | 0 | PROCESSED | 57612.6971527778 | 2016-08-12 16:43:54 | 56956 | 2014-10-26 00:00:00 | 56588.757025463 | 2013-10-23 18:10:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080143 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | YOSHITOMO MAEDA | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508064010/ | Quick Look | ![]() |
427 | 0509-67.5 | 77.4191 | -67.5347 | 77.43679 | -67.59534 | 342.967322 | -85.012032 | 278.15520093 | -34.57404921 | 36.9172 | 56491.0670601852 | 2013-07-18 01:36:34 | 56495.4689583333 | 2013-07-22 11:15:18 | 508072020 | 152.6517 | 150 | 152.6997 | 152.6517 | 0 | 152.6997 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 139.7536 | 139.7536 | 380.2994 | 7 | PROCESSED | 57612.009537037 | 2016-08-12 00:13:44 | 56383 | 2013-04-01 00:00:00 | 56509.8769097222 | 2013-08-05 21:02:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072020/ | Quick Look | ![]() |
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428 | MBM36 | 238.3604 | -4.7951 | 237.700156 | -4.647695 | 237.207526 | 15.116261 | 4.00027103 | 35.69642682 | 294.5973 | 56525.2685300926 | 2013-08-21 06:26:41 | 56526.5655092593 | 2013-08-22 13:34:20 | 508079010 | 49.6555 | 80 | 49.6555 | 49.6555 | 0 | 49.6555 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8799 | 42.8799 | 112.0458 | 2 | PROCESSED | 57612.3808912037 | 2016-08-12 09:08:29 | 56383 | 2013-04-01 00:00:00 | 56587.6359027778 | 2013-10-22 15:15:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079010/ | Quick Look | ![]() |
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429 | HESS_J1825-137_2 | 276.1969 | -13.7002 | 275.488545 | -13.728547 | 276.096187 | 9.609358 | 17.73170044 | -0.43977824 | 271.0001 | 54756.4591666667 | 2008-10-17 11:01:12 | 54758.1953009259 | 2008-10-19 04:41:14 | 503029010 | 57.1993 | 50 | 57.1993 | 57.1993 | 0 | 57.1993 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.185 | 51.185 | 149.9858 | 0 | PROCESSED | 57544.2276157407 | 2016-06-05 05:27:46 | 55148 | 2009-11-13 00:00:00 | 54780.5081365741 | 2008-11-10 12:11:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAAKI TANAKA | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503029010/ | Quick Look | ![]() |
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430 | HESSJ1614-A | 243.5214 | -52.1022 | 242.56254 | -51.975946 | 251.486678 | -30.347435 | 331.29897546 | -0.76107386 | 283.3889 | 54729.7629050926 | 2008-09-20 18:18:35 | 54730.562662037 | 2008-09-21 13:30:14 | 503073010 | 53.6494 | 50 | 53.6574 | 53.6494 | 0 | 53.6654 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.8713 | 40.8713 | 69.0719 | 0 | PROCESSED | 57543.9752662037 | 2016-06-04 23:24:23 | 55148 | 2009-11-13 00:00:00 | 54780.4246990741 | 2008-11-10 10:11:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030088 | The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503073010/ | Quick Look | ![]() |
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431 | HESSJ1832 | 278.156 | -8.4222 | 277.474303 | -8.460064 | 278.335703 | 14.782649 | 23.29856204 | 0.30967904 | 88.1963 | 55659.2543518518 | 2011-04-08 06:06:16 | 55660.3454282407 | 2011-04-09 08:17:25 | 506021010 | 40.3432 | 40 | 40.3432 | 40.3432 | 0 | 40.3432 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8513 | 34.8513 | 94.2578 | 1 | PROCESSED | 57601.464224537 | 2016-08-01 11:08:29 | 56043 | 2012-04-26 00:00:00 | 55673.2950925926 | 2011-04-22 07:04:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506021010/ | Quick Look | ![]() |
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432 | MBM20 | 68.9307 | -14.6229 | 68.358009 | -14.724304 | 64.461829 | -36.216174 | 211.39181931 | -36.56844204 | 64.9904 | 56520.8174074074 | 2013-08-16 19:37:04 | 56522.5001967593 | 2013-08-18 12:00:17 | 508081010 | 56.4905 | 80 | 56.4905 | 56.4905 | 0 | 56.4905 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.086 | 55.086 | 145.38 | 1 | PROCESSED | 57612.3311111111 | 2016-08-12 07:56:48 | 56383 | 2013-04-01 00:00:00 | 56587.6432291667 | 2013-10-22 15:26:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508081010/ | Quick Look | ![]() |
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433 | CYGNUS LOOP (P25) | 311.8608 | 32.1678 | 311.350497 | 31.982956 | 327.005863 | 47.670937 | 74.68970828 | -7.03578766 | 60.8878 | 54621.6278472222 | 2008-06-04 15:04:06 | 54622.1488888889 | 2008-06-05 03:34:24 | 503061010 | 25.9959 | 20 | 25.9959 | 25.9959 | 0 | 25.9959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.8791 | 23.8791 | 45.01 | 0 | PROCESSED | 57542.7242476852 | 2016-06-03 17:22:55 | 55003 | 2009-06-21 00:00:00 | 54636.2508217593 | 2008-06-19 06:01:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503061010/ | Quick Look | ![]() |
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434 | VELA PWN GEV3 | 128.0196 | -44.9062 | 127.597638 | -44.735505 | 152.091567 | -60.413918 | 262.99085627 | -3.09029782 | 119.9755 | 56986.5006481482 | 2014-11-25 12:00:56 | 56986.9105439815 | 2014-11-25 21:51:11 | 509013010 | 18.4893 | 15 | 18.4893 | 18.4969 | 0 | 18.4893 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8178009259 | 2016-08-16 19:37:38 | 57366 | 2015-12-10 00:00:00 | 57002.4411226852 | 2014-12-11 10:35:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509013010/ | Quick Look | ![]() |
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435 | VELA PWN GEV4 | 127.5996 | -44.9062 | 127.17888 | -44.73712 | 151.566964 | -60.561222 | 262.81539743 | -3.33071285 | 121.1346 | 56986.9114814815 | 2014-11-25 21:52:32 | 56987.558587963 | 2014-11-26 13:24:22 | 509014010 | 17.9817 | 15 | 17.9817 | 17.9897 | 0 | 17.9977 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8244328704 | 2016-08-16 19:47:11 | 57368 | 2015-12-12 00:00:00 | 57002.4392824074 | 2014-12-11 10:32:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509014010/ | Quick Look | ![]() |
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436 | G166.0+4.3_NE | 81.7715 | 42.9863 | 80.874617 | 42.944315 | 83.616156 | 19.728231 | 166.13139999 | 4.39632756 | 84.8097 | 56922.0215740741 | 2014-09-22 00:31:04 | 56923.3544444444 | 2014-09-23 08:30:24 | 509022020 | 58.5598 | 60 | 58.5598 | 61.5039 | 0 | 61.4879 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2.207 | 2.207 | 5.696 | 0 | PROCESSED | 57616.5872685185 | 2016-08-16 14:05:40 | 57312 | 2015-10-17 00:00:00 | 56945.1963657407 | 2014-10-15 04:42:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509022020/ | Quick Look | ![]() |
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437 | CIZA J1358.9-4750_NW | 209.4473 | -47.6057 | 208.659126 | -47.362265 | 225.512998 | -33.070935 | 314.36323033 | 13.78794346 | 293.0002 | 56880.8612615741 | 2014-08-11 20:40:13 | 56881.8265972222 | 2014-08-12 19:50:18 | 509028010 | 41.501 | 40 | 41.501 | 41.525 | 0 | 41.509 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.9918 | 7.9918 | 20.64 | 0 | PROCESSED | 57616.4817939815 | 2016-08-16 11:33:47 | 57267 | 2015-09-02 00:00:00 | 56898.4888657407 | 2014-08-29 11:43:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509028010/ | Quick Look | ![]() |
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438 | G189 EAST | 95.4705 | 22.4826 | 94.715097 | 22.507311 | 95.056054 | -0.862354 | 189.63783855 | 3.93426331 | 258.2106 | 57096.5099652778 | 2015-03-15 12:14:21 | 57098.6780324074 | 2015-03-17 16:16:22 | 509036010 | 66.0529 | 85 | 66.0529 | 86.2237 | 0 | 86.2397 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8236226852 | 2016-08-17 19:46:01 | 57524 | 2016-05-16 00:00:00 | 57157.5685416667 | 2015-05-15 13:38:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091314 | We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars. | GALACTIC DIFFUSE EMISSION | 5 | B | BRIAN WILLIAMS | USA | 9 | AO9 | OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509036010/ | Quick Look | ![]() |
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439 | RADIO_ARC_SOUTH | 266.9853 | -29.0688 | 266.190093 | -29.052225 | 267.342882 | -5.6555 | 0.15000746 | -0.5026703 | 267.1998 | 56186.0290509259 | 2012-09-16 00:41:50 | 56188.8203472222 | 2012-09-18 19:41:18 | 507016010 | 103.472 | 100 | 103.472 | 103.472 | 0 | 103.472 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.1906 | 89.1906 | 241.1319 | 4 | PROCESSED | 57607.146875 | 2016-08-07 03:31:30 | 56668 | 2014-01-11 00:00:00 | 56303.6234490741 | 2013-01-11 14:57:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070016 | The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. | GALACTIC DIFFUSE EMISSION | 5 | A | SYUKYO RYU | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507016010/ | Quick Look | ![]() |
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440 | VELA JR SE1 | 133.9641 | -46.7818 | 133.536852 | -46.589245 | 161.150153 | -59.841767 | 267.02895458 | -1.00032542 | 109.9994 | 56621.589525463 | 2013-11-25 14:08:55 | 56622.3175462963 | 2013-11-26 07:37:16 | 508060010 | 40.5996 | 40 | 40.5996 | 40.5996 | 0 | 40.6057 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6535 | 46.6535 | 62.8959 | 0 | PROCESSED | 57613.4271990741 | 2016-08-13 10:15:10 | 56998 | 2014-12-07 00:00:00 | 56632.5928240741 | 2013-12-06 14:13:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | TARO FUKUYAMA | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508060010/ | Quick Look | ![]() |
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441 | KES 69 | 278.2575 | -10.136 | 277.567341 | -10.174332 | 278.335469 | 13.065931 | 21.8245316 | -0.57033928 | 267.6495 | 56927.2830902778 | 2014-09-27 06:47:39 | 56929.1391435185 | 2014-09-29 03:20:22 | 509037010 | 77.3795 | 80 | 77.3795 | 77.9708 | 0 | 77.9953 | 2 | 2 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5892361111 | 2016-08-16 14:08:30 | 57345 | 2015-11-19 00:00:00 | 56979.4056944444 | 2014-11-18 09:44:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091315 | We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509037010/ | Quick Look | ![]() |
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442 | RXJ1713-3946_ID1 | 257.9616 | -39.5166 | 257.09684 | -39.456462 | 260.331165 | -16.477991 | 347.33828294 | -0.06271892 | 87.0007 | 55242.129375 | 2010-02-15 03:06:18 | 55243.2502199074 | 2010-02-16 06:00:19 | 504027010 | 61.5331 | 60 | 61.5578 | 61.5331 | 0 | 61.5738 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46.7259 | 46.7259 | 96.8238 | 0 | PROCESSED | 57550.6101273148 | 2016-06-11 14:38:35 | 55622 | 2011-03-02 00:00:00 | 55253.4734259259 | 2010-02-26 11:21:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504027010/ | Quick Look | ![]() |
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443 | FERMI_JET_COCOON_2 | 320.2279 | -29.504 | 319.485138 | -29.716859 | 313.416673 | -13.31861 | 17.00065384 | -44.00205209 | 255.063 | 56981.4053356482 | 2014-11-20 09:43:41 | 56981.8683217593 | 2014-11-20 20:50:23 | 509048010 | 19.9032 | 20 | 19.9032 | 19.9032 | 0 | 19.9032 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7951736111 | 2016-08-16 19:05:03 | 57362 | 2015-12-06 00:00:00 | 56995.5937268518 | 2014-12-04 14:14:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509048010/ | Quick Look | ![]() |
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444 | DIFFUSE1E | 200.6072 | 7.3824 | 199.979251 | 7.643505 | 196.163547 | 14.87503 | 324.76377809 | 68.9302329 | 123.5311 | 57011.0086458333 | 2014-12-20 00:12:27 | 57011.5252083333 | 2014-12-20 12:36:18 | 509062010 | 23.9762 | 20 | 23.9762 | 24.5362 | 0 | 24.5362 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5495023148 | 2016-08-17 13:11:17 | 57475 | 2016-03-28 00:00:00 | 57107.4289583333 | 2015-03-26 10:17:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509062010/ | Quick Look | ![]() |
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445 | MBM16 | 49.7641 | 11.5835 | 49.080496 | 11.40241 | 50.44037 | -6.504342 | 170.59835317 | -37.27294118 | 77.8263 | 56867.2632638889 | 2014-07-29 06:19:06 | 56869.0606018518 | 2014-07-31 01:27:16 | 509073010 | 78.81 | 80 | 78.818 | 78.818 | 0 | 78.81 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4583449074 | 2016-08-16 11:00:01 | 56748 | 2014-04-01 00:00:00 | 56902.6996180556 | 2014-09-02 16:47:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073010/ | Quick Look | ![]() |
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446 | VELA FRAGMENT C | 136.2696 | -44.691 | 135.819541 | -44.490549 | 161.57955 | -57.213344 | 266.51473212 | 1.58715492 | 269.3614 | 54580.6978703704 | 2008-04-24 16:44:56 | 54582.3056481482 | 2008-04-26 07:20:08 | 503095010 | 84.1167 | 70 | 84.1167 | 84.1167 | 0 | 84.1167 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.3547 | 91.3547 | 138.9018 | 2 | PROCESSED | 57542.4305439815 | 2016-06-03 10:19:59 | 54960 | 2009-05-09 00:00:00 | 54594.2480324074 | 2008-05-08 05:57:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | TERRANCE GAETZ | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503095010/ | Quick Look | ![]() |
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447 | GB_NORTH_1 | 266.1004 | -28.3619 | 265.30982 | -28.341045 | 266.546613 | -4.967513 | 0.35022505 | 0.52781175 | 106.0661 | 57104.6393981482 | 2015-03-23 15:20:44 | 57106.6752777778 | 2015-03-25 16:12:24 | 509077010 | 98.2407 | 100 | 98.2407 | 98.4407 | 0 | 98.4407 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8715277778 | 2016-08-17 20:55:00 | 56748 | 2014-04-01 00:00:00 | 57120.4153125 | 2015-04-08 09:58:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509077010/ | Quick Look | ![]() |
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448 | HESS J1745-303A | 265.7791 | -30.3241 | 264.976083 | -30.301658 | 266.320995 | -6.936807 | 358.53258375 | -0.26269922 | 103.33 | 55253.3854166667 | 2010-02-26 09:15:00 | 55254.6758796296 | 2010-02-27 16:13:16 | 504001010 | 51.1538 | 50 | 51.1618 | 51.1538 | 0 | 51.1685 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.2196 | 42.2196 | 111.4581 | 1 | PROCESSED | 57550.7381134259 | 2016-06-11 17:42:53 | 55636 | 2011-03-16 00:00:00 | 55267.2568634259 | 2010-03-12 06:09:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504001010/ | Quick Look | ![]() |
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449 | RADIO_ARC_S_E | 267.1914 | -28.7693 | 266.398054 | -28.753729 | 267.517971 | -5.352408 | 0.49965543 | -0.50260843 | 267.4999 | 56199.7928125 | 2012-09-29 19:01:39 | 56200.9349652778 | 2012-09-30 22:26:21 | 507017010 | 54.1782 | 50 | 54.2022 | 54.1782 | 0 | 54.202 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51.7936 | 51.7936 | 98.6799 | 0 | PROCESSED | 57607.2277777778 | 2016-08-07 05:28:00 | 56592 | 2013-10-27 00:00:00 | 56226.621400463 | 2012-10-26 14:54:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070016 | The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. | GALACTIC DIFFUSE EMISSION | 5 | A | SYUKYO RYU | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507017010/ | Quick Look | ![]() |
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450 | BLOWOUT2 | 311.9515 | 31.5359 | 311.437845 | 31.350733 | 326.744585 | 47.059417 | 74.23825049 | -7.48819964 | 243.427 | 55158.9662615741 | 2009-11-23 23:11:25 | 55159.5106944444 | 2009-11-24 12:15:24 | 504012010 | 26.5494 | 23 | 26.5654 | 26.5494 | 0 | 26.5734 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.9401 | 19.9401 | 47.0319 | 1 | PROCESSED | 57549.5397800926 | 2016-06-10 12:57:17 | 55545 | 2010-12-15 00:00:00 | 55176.2336921296 | 2009-12-11 05:36:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504012010/ | Quick Look | ![]() |
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451 | W49B | 287.7847 | 9.1153 | 287.186342 | 9.031642 | 290.654992 | 31.289584 | 43.2812159 | -0.18378496 | 89.2674 | 54921.5302662037 | 2009-03-31 12:43:35 | 54923.0613425926 | 2009-04-02 01:28:20 | 504035010 | 61.7825 | 100 | 61.7905 | 61.7845 | 0 | 61.7825 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 55.1556 | 55.1556 | 132.2739 | 3 | PROCESSED | 57546.0146412037 | 2016-06-07 00:21:05 | 55324 | 2010-05-08 00:00:00 | 54949.4493287037 | 2009-04-28 10:47:02 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040075 | Observation of the W49B supernova remnant for 100 ksec is proposed to detect Ti emission line at the 3 sigma confidence level. In order to reveal whether it is a remnant of Type Ia supernova or not, detailed measurement of the rare metal elements such as Cr, Mn, Ni, and Ti is essential. We determine the type by Ti to Cr, Mn to Cr, and Ni to Fe ratios. Furthermore, we investigate whether its plasma is in the overionized status or not. | GALACTIC DIFFUSE EMISSION | 5 | B | MIDORI OZAWA | JAP | 4 | AO4 | UNMASK THE NATURE OF W49B ! | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504035010/ | Quick Look | ![]() |
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452 | FESI2 | 313.183 | 30.3797 | 312.661298 | 30.190122 | 327.500793 | 45.583083 | 73.99193661 | -9.03499466 | 225.2405 | 55174.9860300926 | 2009-12-09 23:39:53 | 55175.7904398148 | 2009-12-10 18:58:14 | 504018010 | 34.5904 | 34 | 34.5904 | 34.5904 | 0 | 34.5904 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.318 | 30.318 | 69.4939 | 0 | PROCESSED | 57549.7573032407 | 2016-06-10 18:10:31 | 55555 | 2010-12-25 00:00:00 | 55189.1622916667 | 2009-12-24 03:53:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504018010/ | Quick Look | ![]() |
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453 | GALACTIC_BULGE7 | 266.6764 | -30.8281 | 265.869887 | -30.809998 | 267.112733 | -7.42025 | 358.50617228 | -1.18471698 | 274.4326 | 55117.1787037037 | 2009-10-13 04:17:20 | 55118.4785416667 | 2009-10-14 11:29:06 | 504090010 | 41.2607 | 50 | 41.2607 | 52.9033 | 0 | 52.9033 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 34.964 | 34.964 | 112.2938 | 2 | PROCESSED | 57548.8825694444 | 2016-06-09 21:10:54 | 54922 | 2009-04-01 00:00:00 | 55133.2421643518 | 2009-10-29 05:48:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504090010/ | Quick Look | ![]() |
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454 | HESS J1809-193B | 272.6789 | -19.1585 | 271.941455 | -19.169725 | 272.527802 | 4.258732 | 11.32661741 | -0.06027609 | 269.0544 | 55084.4838773148 | 2009-09-10 11:36:47 | 55085.7488310185 | 2009-09-11 17:58:19 | 504078010 | 52.4748 | 50 | 52.4748 | 52.4748 | 0 | 52.4748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.3733 | 43.3733 | 109.2758 | 1 | PROCESSED | 57548.5486226852 | 2016-06-09 13:10:01 | 55475 | 2010-10-06 00:00:00 | 55109.4280555556 | 2009-10-05 10:16:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | OLEG KARGALTSEV | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504078010/ | Quick Look | ![]() |
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455 | 330.2+1.0 | 240.2384 | -51.525 | 239.295706 | -51.384773 | 249.047523 | -30.224565 | 330.18352169 | 1.02987491 | 98.9027 | 55239.832025463 | 2010-02-12 19:58:07 | 55242.125150463 | 2010-02-15 03:00:13 | 504083030 | 92.505 | 30 | 92.513 | 92.505 | 0 | 92.521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.0965 | 86.0965 | 198.0897 | 4 | PROCESSED | 57550.6564699074 | 2016-06-11 15:45:19 | 55622 | 2011-03-02 00:00:00 | 55253.5397685185 | 2010-02-26 12:57:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | GLENN ALLEN | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504083030/ | Quick Look | ![]() |
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456 | 3C_397 | 286.9038 | 7.1223 | 286.296185 | 7.042755 | 289.336416 | 29.435283 | 41.11064468 | -0.32936267 | 256.5108 | 55493.8258449074 | 2010-10-24 19:49:13 | 55495.8022337963 | 2010-10-26 19:15:13 | 505008010 | 69.3266 | 70 | 69.3266 | 69.3266 | 0 | 69.3266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62.1653 | 62.1653 | 170.7319 | 0 | PROCESSED | 57553.8922800926 | 2016-06-14 21:24:53 | 55287 | 2010-04-01 00:00:00 | 55505.3393981482 | 2010-11-05 08:08:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505008010/ | Quick Look | ![]() |
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457 | CYGNUS LOOP 5 | 312.0188 | 31.9594 | 311.507127 | 31.773986 | 327.066622 | 47.426634 | 74.60885135 | -7.27014396 | 81.8368 | 55305.8645833333 | 2010-04-19 20:45:00 | 55306.4578125 | 2010-04-20 10:59:15 | 505013010 | 26.8452 | 26 | 26.8452 | 26.8452 | 0 | 26.8452 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.277 | 21.277 | 51.232 | 2 | PROCESSED | 57551.2602083333 | 2016-06-12 06:14:42 | 55287 | 2010-04-01 00:00:00 | 55364.2036458333 | 2010-06-17 04:53:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505013010/ | Quick Look | ![]() |
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458 | CYGNUS LOOP 11 | 313.8693 | 30.5587 | 313.347105 | 30.366695 | 328.378211 | 45.516461 | 74.51088669 | -9.3807208 | 82.002 | 55328.698587963 | 2010-05-12 16:45:58 | 55329.1251736111 | 2010-05-13 03:00:15 | 505019010 | 18.8976 | 18 | 18.9056 | 18.8976 | 0 | 18.9136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9048 | 14.9048 | 36.8539 | 1 | PROCESSED | 57551.490150463 | 2016-06-12 11:45:49 | 55287 | 2010-04-01 00:00:00 | 55393.3619791667 | 2010-07-16 08:41:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505019010/ | Quick Look | ![]() |
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459 | WESTERLUND1_4 | 253.5509 | -45.3005 | 252.641306 | -45.219522 | 257.53427 | -22.567529 | 340.7711384 | -1.01287357 | 288.2868 | 55463.3974652778 | 2010-09-24 09:32:21 | 55464.5203587963 | 2010-09-25 12:29:19 | 505052010 | 49.627 | 50 | 49.627 | 49.627 | 0 | 49.627 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2137 | 40.2137 | 97.0079 | 1 | PROCESSED | 57553.5510416667 | 2016-06-14 13:13:30 | 55840 | 2011-10-06 00:00:00 | 55474.1080208333 | 2010-10-05 02:35:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505052010/ | Quick Look | ![]() |
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460 | VELA SNR CB-LBG | 130.6266 | -44.6167 | 130.194556 | -44.436193 | 154.988854 | -59.23497 | 263.87788945 | -1.43970243 | 293.482 | 55319.3460648148 | 2010-05-03 08:18:20 | 55319.7940046296 | 2010-05-03 19:03:22 | 505071010 | 27.1799 | 20 | 27.1799 | 27.1799 | 0 | 27.1799 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0945 | 25.0945 | 38.6939 | 1 | PROCESSED | 57551.3691203704 | 2016-06-12 08:51:32 | 55696 | 2011-05-15 00:00:00 | 55330.1543981482 | 2010-05-14 03:42:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505071010/ | Quick Look | ![]() |
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461 | GALACTIC_BULGE4 | 269.1417 | -30.4015 | 268.337633 | -30.395373 | 269.244618 | -6.962713 | 359.95546853 | -2.79264334 | 69.3552 | 55632.2752314815 | 2011-03-12 06:36:20 | 55633.4287152778 | 2011-03-13 10:17:21 | 505079010 | 50.2193 | 50 | 50.2273 | 50.2193 | 0 | 50.2273 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.375 | 43.375 | 99.648 | 1 | PROCESSED | 57601.1540277778 | 2016-08-01 03:41:48 | 55287 | 2010-04-01 00:00:00 | 55645.5706134259 | 2011-03-25 13:41:41 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505079010/ | Quick Look | ![]() |
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462 | GALACTIC_BULGE5 | 270.1525 | -30.903 | 269.345086 | -30.901777 | 270.122341 | -7.462063 | 359.95222621 | -3.79644913 | 86.7823 | 55293.7188657407 | 2010-04-07 17:15:10 | 55295.8849074074 | 2010-04-09 21:14:16 | 505080010 | 56.1396 | 50 | 56.1396 | 56.1396 | 0 | 56.1396 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.1498 | 55.1498 | 185.0058 | 1 | PROCESSED | 57553.0630439815 | 2016-06-14 01:30:47 | 55287 | 2010-04-01 00:00:00 | 55441.4355555556 | 2010-09-02 10:27:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505080010/ | Quick Look | ![]() |
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463 | JUPITER | 29.0345 | 10.6283 | 28.369064 | 10.38411 | 30.736601 | -1.177073 | 147.65759499 | -49.11229838 | 249.1849 | 55938.2087962963 | 2012-01-12 05:00:40 | 55939.2481944444 | 2012-01-13 05:57:24 | 506006040 | 38.6289 | 160 | 38.6289 | 38.6367 | 0 | 38.6369 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.7692 | 31.7692 | 89.7859 | 0 | PROCESSED | 57604.3463657407 | 2016-08-04 08:18:46 | 56388 | 2013-04-06 00:00:00 | 56020.1680208333 | 2012-04-03 04:01:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006040/ | Quick Look | ![]() |
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464 | THE KEPLER SNR | 262.6707 | -21.4823 | 261.92146 | -21.444975 | 263.169631 | 1.785142 | 4.52498329 | 6.82417088 | 98.3356 | 55620.8079166667 | 2011-02-28 19:23:24 | 55624.797337963 | 2011-03-04 19:08:10 | 505092040 | 146.2337 | 250 | 146.2337 | 146.2541 | 0 | 146.2577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113.8022 | 113.8022 | 344.6577 | 6 | PROCESSED | 57601.192337963 | 2016-08-01 04:36:58 | 55287 | 2010-04-01 00:00:00 | 55642.4090046296 | 2011-03-22 09:48:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092040/ | Quick Look | ![]() |
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465 | CYGNUS LOOP BLOWOUT1 | 312.1499 | 29.2487 | 311.624762 | 29.062833 | 325.710057 | 44.881262 | 72.53069275 | -9.03908096 | 78.1532 | 55686.7775578704 | 2011-05-05 18:39:41 | 55687.8494907407 | 2011-05-06 20:23:16 | 506011010 | 48.5641 | 50 | 48.5641 | 48.5641 | 0 | 48.5641 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.0429 | 42.0429 | 92.5799 | 1 | PROCESSED | 57601.954224537 | 2016-08-01 22:54:05 | 56066 | 2012-05-19 00:00:00 | 55698.3278472222 | 2011-05-17 07:52:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506011010/ | Quick Look | ![]() |
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466 | GAMMACYGNI_NWSHELL2 | 304.652 | 40.6975 | 304.208167 | 40.540107 | 324.021819 | 57.820534 | 78.12229495 | 2.68416641 | 82.9982 | 55665.3027430556 | 2011-04-14 07:15:57 | 55666.2688657407 | 2011-04-15 06:27:10 | 506018010 | 39.712 | 40 | 39.712 | 39.712 | 0 | 39.712 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.1165 | 36.1165 | 83.4379 | 0 | PROCESSED | 57601.5048032407 | 2016-08-01 12:06:55 | 56058 | 2012-05-11 00:00:00 | 55690.9818402778 | 2011-05-09 23:33:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060059 | We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band. | GALACTIC DIFFUSE EMISSION | 5 | B | YASUYUKI TANAKA | JAP | 6 | AO6 | SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506018010/ | Quick Look | ![]() |
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467 | S147_N | 87.0463 | 27.5187 | 86.260987 | 27.502453 | 87.375766 | 4.104837 | 181.50494456 | -0.25223067 | 273.8998 | 55997.2930324074 | 2012-03-11 07:01:58 | 55998.555787037 | 2012-03-12 13:20:20 | 506031010 | 54.8833 | 55 | 54.8913 | 54.8833 | 0 | 54.8913 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.1919 | 52.1919 | 109.054 | 1 | PROCESSED | 57604.8728472222 | 2016-08-04 20:56:54 | 56385 | 2013-04-03 00:00:00 | 56016.6668287037 | 2012-03-30 16:00:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060080 | We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it. | GALACTIC DIFFUSE EMISSION | 5 | C | YOSHITAKA HANABATA | JAP | 6 | AO6 | STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506031010/ | Quick Look | ![]() |
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468 | VELA PWN E6 | 131.2685 | -45.4809 | 130.840764 | -45.298021 | 156.629635 | -59.743456 | 264.83769354 | -1.61837696 | 304.5065 | 55712.9576273148 | 2011-05-31 22:58:59 | 55713.2292939815 | 2011-06-01 05:30:11 | 506049010 | 18.1968 | 15 | 18.2048 | 18.1968 | 0 | 18.2128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.209 | 14.209 | 23.4699 | 0 | PROCESSED | 57602.1814699074 | 2016-08-02 04:21:19 | 56103 | 2012-06-25 00:00:00 | 55735.9387268518 | 2011-06-23 22:31:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506049010/ | Quick Look | ![]() |
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469 | ERIDANUS_ARCB_SPOT | 53.3104 | -9.6904 | 52.708102 | -9.857933 | 48.180187 | -27.963294 | 196.20250346 | -48.10218961 | 67.1761 | 56138.1083101852 | 2012-07-30 02:35:58 | 56139.0792476852 | 2012-07-31 01:54:07 | 507032010 | 40.6186 | 40 | 40.6186 | 40.6186 | 0 | 40.6186 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.171 | 35.171 | 83.8699 | 1 | PROCESSED | 57606.7122337963 | 2016-08-06 17:05:37 | 56528 | 2013-08-24 00:00:00 | 56162.0431018518 | 2012-08-23 01:02:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070046 | We propose Suzaku spectroscopic observations of the Edinanus Super Bubble, the nearest super bubble in our Galaxy. This is a good site to study the density, temperature, metalicity, and ionization status etc. at the rim of super bubbles which might be sources of the Galactic halo or fountains. A series of observations will reveal how the hot plasma is heated and expands as a bubble. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIKO YAMASAKI | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE ERIDANUS SUPER BUBBLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507032010/ | Quick Look | ![]() |
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470 | G299.5-0.6 | 184.8049 | -63.1515 | 184.121711 | -62.873858 | 220.875708 | -53.463768 | 299.30360744 | -0.50694599 | 313.6989 | 56144.5663773148 | 2012-08-05 13:35:35 | 56144.9523032407 | 2012-08-05 22:51:19 | 507064010 | 13.8351 | 10 | 13.8431 | 13.8351 | 0 | 13.8431 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2722 | 13.2722 | 33.3359 | 0 | PROCESSED | 57606.7635763889 | 2016-08-06 18:19:33 | 56630 | 2013-12-04 00:00:00 | 56264.5463541667 | 2012-12-03 13:06:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | TOBIAS PRINZ | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507064010/ | Quick Look | ![]() |
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471 | G350.1-0.3 | 260.2697 | -37.4549 | 259.419167 | -37.405796 | 262.032562 | -14.282003 | 350.06545974 | -0.33871818 | 266.4234 | 55821.2580787037 | 2011-09-17 06:11:38 | 55822.9126388889 | 2011-09-18 21:54:12 | 506065010 | 70.1813 | 70 | 70.1973 | 70.1813 | 0 | 70.1973 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.0704 | 60.0704 | 142.9159 | 0 | PROCESSED | 57603.2088541667 | 2016-08-03 05:00:45 | 55652 | 2011-04-01 00:00:00 | 55865.2679282407 | 2011-10-31 06:25:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506065010/ | Quick Look | ![]() |
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472 | FERMI_BUBBLE_S1 | 329.068 | -46.6182 | 328.273423 | -46.856069 | 313.852963 | -31.76179 | 351.41726681 | -50.59485428 | 44.0071 | 56034.6949884259 | 2012-04-17 16:40:47 | 56035.2070717593 | 2012-04-18 04:58:11 | 507009010 | 25.3149 | 20 | 25.3149 | 25.3229 | 0 | 25.3229 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.7973 | 24.7973 | 44.2399 | 0 | PROCESSED | 57605.1828703704 | 2016-08-05 04:23:20 | 56420 | 2013-05-08 00:00:00 | 56049.2134722222 | 2012-05-02 05:07:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507009010/ | Quick Look | ![]() |
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473 | IC 443 | 94.3026 | 22.7461 | 93.545529 | 22.76515 | 93.969538 | -0.635542 | 188.89781567 | 3.10590753 | 258.9991 | 56382.4892824074 | 2013-03-31 11:44:34 | 56385.8835763889 | 2013-04-03 21:12:21 | 507015030 | 131.1823 | 300 | 131.1823 | 131.1823 | 0 | 131.1823 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113.8514 | 113.8514 | 293.2478 | 1 | PROCESSED | 57611.0338194444 | 2016-08-11 00:48:42 | 56018 | 2012-04-01 00:00:00 | 56394.7872337963 | 2013-04-12 18:53:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507015030/ | Quick Look | ![]() |
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474 | G337.2-0.7 | 249.8782 | -47.8314 | 248.950154 | -47.733478 | 255.175293 | -25.419144 | 337.20769447 | -0.7291284 | 280.8005 | 56172.5530439815 | 2012-09-02 13:16:23 | 56181.2598263889 | 2012-09-11 06:14:09 | 507068010 | 304.1484 | 300 | 304.1564 | 304.1484 | 0 | 304.1484 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 275.8448 | 275.8448 | 461.2638 | 9 | PROCESSED | 57607.2211111111 | 2016-08-07 05:18:24 | 56018 | 2012-04-01 00:00:00 | 56271.4641203704 | 2012-12-10 11:08:20 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 7 | Ao7 | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507068010/ | Quick Look | ![]() |
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475 | CYG_BGD2 | 306.9576 | 42.391 | 306.519882 | 42.224487 | 328.379789 | 58.578032 | 80.50042704 | 2.23726855 | 218.3998 | 56280.6304166667 | 2012-12-19 15:07:48 | 56281.1313888889 | 2012-12-20 03:09:12 | 507042010 | 25.6249 | 25 | 25.6249 | 25.6249 | 0 | 25.6489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.025 | 25.025 | 43.2739 | 1 | PROCESSED | 57608.3181018518 | 2016-08-08 07:38:04 | 56683 | 2014-01-26 00:00:00 | 56316.5346990741 | 2013-01-24 12:49:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070060 | The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507042010/ | Quick Look | ![]() |
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476 | VELA PWN N5 | 128.8386 | -43.7507 | 128.405645 | -43.5769 | 151.977516 | -59.119722 | 262.41040878 | -1.9318018 | 327.6005 | 56110.3470717593 | 2012-07-02 08:19:47 | 56110.6620138889 | 2012-07-02 15:53:18 | 507052010 | 18.1486 | 15 | 18.1566 | 18.1486 | 0 | 18.1566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.4582 | 17.4582 | 27.208 | 1 | PROCESSED | 57606.5339930556 | 2016-08-06 12:48:57 | 56493 | 2013-07-20 00:00:00 | 56127.126712963 | 2012-07-19 03:02:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507052010/ | Quick Look | ![]() |
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477 | JUPITER | 104.3277 | 23.0738 | 103.571845 | 23.140907 | 103.162022 | 0.285142 | 192.75008442 | 11.51865374 | 264.5662 | 56766.1211111111 | 2014-04-19 02:54:24 | 56766.4481365741 | 2014-04-19 10:45:19 | 508023080 | 15.9616 | 160 | 15.9776 | 15.9616 | 0 | 15.9806 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9566782407 | 2016-08-14 22:57:37 | 57212 | 2015-07-09 00:00:00 | 56782.5045486111 | 2014-05-05 12:06:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023080/ | Quick Look | ![]() |
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478 | GRXE_E_6 | 268.1913 | -26.3855 | 267.412548 | -26.37482 | 268.368065 | -2.954748 | 3.00107417 | -0.0433749 | 104.9996 | 56375.3653125 | 2013-03-24 08:46:03 | 56377.4119444445 | 2013-03-26 09:53:12 | 507073010 | 101.6745 | 100 | 101.6745 | 101.6745 | 0 | 101.6745 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100.2473 | 100.2473 | 176.8078 | 1 | PROCESSED | 57610.9396296296 | 2016-08-10 22:33:04 | 56018 | 2012-04-01 00:00:00 | 56387.5561574074 | 2013-04-05 13:20:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507073010/ | Quick Look | ![]() |
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479 | JUPITER | 103.925 | 23.1078 | 103.168762 | 23.173006 | 102.79003 | 0.283016 | 192.55993514 | 11.19674467 | 264.4254 | 56763.06625 | 2014-04-16 01:35:24 | 56763.3890162037 | 2014-04-16 09:20:11 | 508023040 | 14.5693 | 160 | 14.5773 | 14.5693 | 0 | 14.5847 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9505902778 | 2016-08-14 22:48:51 | 57212 | 2015-07-09 00:00:00 | 56839.6932175926 | 2014-07-01 16:38:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023040/ | Quick Look | ![]() |
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480 | HESS J1534-571 3 | 234.1055 | -57.4189 | 233.115127 | -57.253673 | 246.756574 | -36.836074 | 323.73309574 | -1.36851406 | 296.0043 | 56544.6705787037 | 2013-09-09 16:05:38 | 56545.1793171296 | 2013-09-10 04:18:13 | 508015010 | 38.7487 | 40 | 38.7727 | 38.7647 | 0 | 38.7487 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29.947 | 29.947 | 43.9439 | 0 | PROCESSED | 57612.5739814815 | 2016-08-12 13:46:32 | 56956 | 2014-10-26 00:00:00 | 56588.8303125 | 2013-10-23 19:55:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508015010/ | Quick Look | ![]() |
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481 | HESSJ1858-A | 284.5878 | 2.0823 | 283.956685 | 2.013656 | 286.075284 | 24.712449 | 35.57325236 | -0.58765875 | 251.7991 | 56592.8339467593 | 2013-10-27 20:00:53 | 56593.9759027778 | 2013-10-28 23:25:18 | 508021010 | 51.6531 | 50 | 51.6611 | 51.6691 | 0 | 51.6531 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.7792 | 48.7792 | 98.6558 | 1 | PROCESSED | 57613.1533796296 | 2016-08-13 03:40:52 | 56975 | 2014-11-14 00:00:00 | 56608.6801388889 | 2013-11-12 16:19:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080052 | HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 8 | AO8 | DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508021010/ | Quick Look | ![]() |
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482 | HESS J1534-571 1 | 234.0464 | -57.1146 | 233.060336 | -56.949151 | 246.608003 | -36.554258 | 323.88573784 | -1.10331415 | 295.9997 | 56543.4345138889 | 2013-09-08 10:25:42 | 56544.0210300926 | 2013-09-09 00:30:17 | 508013010 | 36.891 | 40 | 36.899 | 36.891 | 0 | 36.899 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36.0704 | 36.0704 | 50.6719 | 0 | PROCESSED | 57612.5616319444 | 2016-08-12 13:28:45 | 56990 | 2014-11-29 00:00:00 | 56622.6022569444 | 2013-11-26 14:27:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508013010/ | Quick Look | ![]() |
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483 | SGR C | 266.1575 | -29.4721 | 265.359887 | -29.451505 | 266.626891 | -6.075935 | 359.43010365 | -0.09543697 | 265.018 | 56559.2657060185 | 2013-09-24 06:22:37 | 56561.8960763889 | 2013-09-26 21:30:21 | 508019010 | 104.2256 | 100 | 104.2495 | 104.2415 | 0 | 104.2256 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.1975 | 91.1975 | 227.2419 | 1 | PROCESSED | 57612.8165277778 | 2016-08-12 19:35:48 | 56956 | 2014-10-26 00:00:00 | 56588.6596643518 | 2013-10-23 15:49:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080043 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508019010/ | Quick Look | ![]() |
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484 | 0509-67.5 | 77.4163 | -67.5163 | 77.433384 | -67.576954 | 343.17919 | -85.012675 | 278.13367069 | -34.57909379 | 302.8449 | 56393.0595949074 | 2013-04-11 01:25:49 | 56397.1258912037 | 2013-04-15 03:01:17 | 508072010 | 175.9192 | 320 | 175.9352 | 175.9192 | 0 | 175.9432 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 166.6668 | 166.6668 | 351.2916 | 3 | PROCESSED | 57611.1504513889 | 2016-08-11 03:36:39 | 56383 | 2013-04-01 00:00:00 | 56425.6930439815 | 2013-05-13 16:37:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508072010/ | Quick Look | ![]() |
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485 | MBM16-OFF | 46.1075 | 13.1563 | 45.420617 | 12.96209 | 47.406639 | -4.032974 | 165.8625544 | -38.38773927 | 69.5985 | 56513.919849537 | 2013-08-09 22:04:35 | 56515.9119791667 | 2013-08-11 21:53:15 | 508073010 | 83.0565 | 80 | 83.0565 | 83.0565 | 0 | 83.0565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.1386 | 81.1386 | 172.0979 | 2 | PROCESSED | 57612.2143981482 | 2016-08-12 05:08:44 | 56953 | 2014-10-23 00:00:00 | 56587.5588541667 | 2013-10-22 13:24:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081322 | We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission. | GALACTIC DIFFUSE EMISSION | 5 | A | EUGENIO URSINO | USA | 8 | AO8 | PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508073010/ | Quick Look | ![]() |
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486 | GRXE_E_8 | 268.4708 | -25.9492 | 267.69465 | -25.939883 | 268.614118 | -2.515578 | 3.50431952 | -0.037979 | 86.7223 | 56718.7089236111 | 2014-03-02 17:00:51 | 56720.9585069445 | 2014-03-04 23:00:15 | 508077010 | 103.132 | 100 | 103.14 | 103.132 | 0 | 103.14 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.8538 | 94.8538 | 194.3449 | 2 | PROCESSED | 57613.971712963 | 2016-08-13 23:19:16 | 56383 | 2013-04-01 00:00:00 | 56775.6980787037 | 2014-04-28 16:45:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086001 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508077010/ | Quick Look | ![]() |
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487 | VELA PWN GEV2 | 128.4409 | -44.9066 | 128.017684 | -44.734295 | 152.61498 | -60.265788 | 263.16834954 | -2.85026128 | 119.7193 | 56985.851099537 | 2014-11-24 20:25:35 | 56986.5001273148 | 2014-11-25 12:00:11 | 509012010 | 19.1078 | 15 | 19.1398 | 19.1238 | 0 | 19.1078 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8168981482 | 2016-08-16 19:36:20 | 57366 | 2015-12-10 00:00:00 | 57009.4112268518 | 2014-12-18 09:52:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509012010/ | Quick Look | ![]() |
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488 | HESS J1641-463 | 250.2616 | -46.3013 | 249.347836 | -46.205158 | 255.208281 | -23.867274 | 338.52580532 | 0.09066192 | 282.4572 | 56900.1342939815 | 2014-08-31 03:13:23 | 56902.1166435185 | 2014-09-02 02:47:58 | 509010020 | 0 | 40 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5303356482 | 2016-08-16 12:43:41 | 56748 | 2014-04-01 00:00:00 | 57122.3887268518 | 2015-04-10 09:19:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090045 | The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 9 | AO9 | IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509010020/ | Quick Look | ![]() |
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489 | CIZA J1358.9-4750_SE | 209.9655 | -47.9267 | 209.17324 | -47.684492 | 226.050091 | -33.219593 | 314.62109256 | 13.3860264 | 293 | 56881.8273032407 | 2014-08-12 19:51:19 | 56882.7188773148 | 2014-08-13 17:15:11 | 509026010 | 41.3601 | 40 | 41.3601 | 41.3601 | 0 | 41.3601 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5.8509 | 5.8509 | 14.04 | 0 | PROCESSED | 57616.4947800926 | 2016-08-16 11:52:29 | 57270 | 2015-09-05 00:00:00 | 56902.1901273148 | 2014-09-02 04:33:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509026010/ | Quick Look | ![]() |
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490 | G93.3+6.9 NW RIM | 312.9527 | 55.5354 | 312.608547 | 55.346344 | 352.30712 | 67.106977 | 93.368132 | 7.08938459 | 52.0991 | 56814.8070023148 | 2014-06-06 19:22:05 | 56817.24125 | 2014-06-09 05:47:24 | 509040010 | 107.8986 | 100 | 107.9066 | 107.9066 | 0 | 107.8986 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2100115741 | 2016-08-15 05:02:25 | 57236 | 2015-08-02 00:00:00 | 56869.6106481482 | 2014-07-31 14:39:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | MICHAEL STAGE | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509040010/ | Quick Look | ![]() |
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491 | OFF-FIELD4 | 173.7625 | -36.8508 | 173.145535 | -36.574162 | 191.286304 | -35.787139 | 286.33839516 | 23.54732297 | 109.4045 | 57008.1600925926 | 2014-12-17 03:50:32 | 57009.6814699074 | 2014-12-18 16:21:19 | 509045010 | 81.321 | 80 | 81.321 | 81.321 | 0 | 81.321 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5308680556 | 2016-08-17 12:44:27 | 56748 | 2014-04-01 00:00:00 | 57112.4059490741 | 2015-03-31 09:44:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | C | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509045010/ | Quick Look | ![]() |
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492 | FERMI_JET_COCOON_5 | 306.4609 | -33.261 | 305.672059 | -33.424933 | 300.742491 | -13.631284 | 9.28791468 | -33.23258901 | 260.3818 | 56968.8506481482 | 2014-11-07 20:24:56 | 56969.3612847222 | 2014-11-08 08:40:15 | 509051010 | 22.0438 | 20 | 22.0518 | 22.0438 | 0 | 22.0573 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7478125 | 2016-08-16 17:56:51 | 57358 | 2015-12-02 00:00:00 | 56982.4350694445 | 2014-11-21 10:26:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509051010/ | Quick Look | ![]() |
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493 | 3C400.2 SW | 294.5545 | 17.147 | 293.991762 | 17.032549 | 300.267467 | 38.043132 | 53.47817432 | -2.17482828 | 81.5886 | 56761.5284375 | 2014-04-14 12:40:57 | 56762.0730555556 | 2014-04-15 01:45:12 | 509069010 | 24.1528 | 20 | 24.1528 | 24.1528 | 0 | 24.1537 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.915 | 23.915 | 47.0479 | 3 | PROCESSED | 57614.2434027778 | 2016-08-14 05:50:30 | 57138 | 2015-04-26 00:00:00 | 56772.6111226852 | 2014-04-25 14:40:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | JACCO VINK | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509069010/ | Quick Look | ![]() |
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494 | GB_NORTH_2 | 265.5401 | -28.4005 | 264.749404 | -28.376931 | 266.05313 | -5.020438 | 0.05846164 | 0.92703829 | 108.0199 | 57106.6765856482 | 2015-03-25 16:14:17 | 57108.7243634259 | 2015-03-27 17:23:05 | 509078010 | 95.3893 | 100 | 95.3893 | 99.8284 | 0 | 99.8124 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8717361111 | 2016-08-17 20:55:18 | 56748 | 2014-04-01 00:00:00 | 57119.4143981482 | 2015-04-07 09:56:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509078010/ | Quick Look | ![]() |
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495 | GB_NORTH_3 | 265.8335 | -28.3716 | 265.042917 | -28.349452 | 266.311245 | -4.983802 | 0.21886292 | 0.72273612 | 108.0564 | 57108.7249074074 | 2015-03-27 17:23:52 | 57110.9703703704 | 2015-03-29 23:17:20 | 509079010 | 106.9674 | 100 | 106.9674 | 108.1889 | 0 | 108.1889 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8792939815 | 2016-08-17 21:06:11 | 56748 | 2014-04-01 00:00:00 | 57119.4192708333 | 2015-04-07 10:03:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509079010/ | Quick Look | ![]() |
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496 | SN1006_BGD4 | 226.2633 | -42.7499 | 225.438524 | -42.555935 | 236.137627 | -24.311137 | 327.5160888 | 13.6541367 | 286.3809 | 56889.2090740741 | 2014-08-20 05:01:04 | 56889.7793865741 | 2014-08-20 18:42:19 | 509086010 | 33.5116 | 30 | 33.5156 | 33.5116 | 0 | 33.5196 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5076851852 | 2016-08-16 12:11:04 | 56748 | 2014-04-01 00:00:00 | 56910.6440162037 | 2014-09-10 15:27:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509086010/ | Quick Look | ![]() |
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497 | 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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498 | 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 | ![]() |
499 | COMET_8P_TUTTLE-P2_11 | 40.2448 | -37.071 | 39.739892 | -37.284352 | 20.945205 | -49.302594 | 243.11250517 | -64.87732742 | 253.5002 | 54491.3630439815 | 2008-01-26 08:42:47 | 54491.4959953704 | 2008-01-26 11:54:14 | 502063110 | 6.3822 | 6.7 | 6.3902 | 6.3822 | 0 | 6.3902 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.8385 | 6.8385 | 11.4799 | 0 | PROCESSED | 57541.406712963 | 2016-06-02 09:45:40 | 54912 | 2009-03-22 00:00:00 | 54546.1994097222 | 2008-03-21 04:47:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063110/ | Quick Look | ![]() |
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500 | RXJ1713-3946_ID2 | 258.3083 | -40.2394 | 257.437413 | -40.180894 | 260.672603 | -17.175399 | 346.91054647 | -0.70324775 | 87.0013 | 55243.7284722222 | 2010-02-16 17:29:00 | 55244.1258564815 | 2010-02-17 03:01:14 | 504028010 | 19.0093 | 20 | 19.0093 | 19.0173 | 0 | 19.0173 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.8263 | 11.8263 | 34.3319 | 0 | PROCESSED | 57550.6004976852 | 2016-06-11 14:24:43 | 55622 | 2011-03-02 00:00:00 | 55256.0518171296 | 2010-03-01 01:14:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504028010/ | Quick Look | ![]() |
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501 | CTB109 NORTHEAST | 345.764 | 59.0015 | 345.238644 | 58.732029 | 24.240732 | 56.810585 | 109.36320905 | -0.98507066 | 252.0025 | 55910.0815393518 | 2011-12-15 01:57:25 | 55910.7522106482 | 2011-12-15 18:03:11 | 506039010 | 30.4058 | 30 | 30.4058 | 30.4058 | 0 | 30.4058 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.7473 | 30.7473 | 57.9219 | 1 | PROCESSED | 57604.1437268518 | 2016-08-04 03:26:58 | 56289 | 2012-12-28 00:00:00 | 55921.9865277778 | 2011-12-26 23:40:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506039010/ | Quick Look | ![]() |
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502 | 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 | ![]() |
503 | VERJ2019_P3 | 304.792 | 36.828 | 304.322431 | 36.670095 | 321.385407 | 54.239801 | 74.98489793 | 0.41476969 | 250.4389 | 56971.0428009259 | 2014-11-10 01:01:38 | 56972.0349537037 | 2014-11-11 00:50:20 | 509030010 | 41.0715 | 40 | 41.0795 | 41.0715 | 0 | 41.0875 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7632175926 | 2016-08-16 18:19:02 | 57352 | 2015-11-26 00:00:00 | 56982.4314467593 | 2014-11-21 10:21:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090120 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 9 | AO9 | SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509030010/ | Quick Look | ![]() |
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504 | VELA PWN NE3 | 131.0442 | -44.0836 | 130.607036 | -43.901563 | 154.967747 | -58.624056 | 263.64329985 | -0.87547181 | 123.9937 | 55895.188900463 | 2011-11-30 04:32:01 | 55895.621724537 | 2011-11-30 14:55:17 | 506043010 | 17.7999 | 15 | 17.8066 | 17.7999 | 0 | 17.8066 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.012 | 13.012 | 37.3959 | 0 | PROCESSED | 57604.0129050926 | 2016-08-04 00:18:35 | 56274 | 2012-12-13 00:00:00 | 55907.1603703704 | 2011-12-12 03:50:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506043010/ | Quick Look | ![]() |
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505 | VELA PWN E1 | 129.1398 | -45.2732 | 128.71724 | -45.098238 | 153.84788 | -60.334335 | 263.75797839 | -2.67419196 | 142.334 | 55916.0561226852 | 2011-12-21 01:20:49 | 55916.622337963 | 2011-12-21 14:56:10 | 506044010 | 17.718 | 15 | 17.718 | 17.718 | 0 | 17.718 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6284 | 16.6284 | 48.8959 | 0 | PROCESSED | 57604.1814814815 | 2016-08-04 04:21:20 | 56305 | 2013-01-13 00:00:00 | 55937.7696527778 | 2012-01-11 18:28:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506044010/ | Quick Look | ![]() |
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506 | HB9-WEST | 74.7057 | 46.2322 | 73.785793 | 46.156635 | 78.534376 | 23.399217 | 160.54700874 | 2.22396757 | 74.7402 | 56930.7930671296 | 2014-09-30 19:02:01 | 56931.9168518518 | 2014-10-01 22:00:16 | 509032010 | 49.7688 | 50 | 49.7688 | 49.7688 | 0 | 49.7688 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5952662037 | 2016-08-16 14:17:11 | 57345 | 2015-11-19 00:00:00 | 56979.4048611111 | 2014-11-18 09:43:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091312 | We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509032010/ | Quick Look | ![]() |
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507 | WESTERLUND1_3 | 252.0931 | -46.1953 | 251.177246 | -46.107555 | 256.5618 | -23.584825 | 339.43313351 | -0.79934014 | 282.1087 | 55462.25625 | 2010-09-23 06:09:00 | 55463.3946296296 | 2010-09-24 09:28:16 | 505051010 | 50.2046 | 50 | 50.2046 | 50.2046 | 0 | 50.2046 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.7966 | 40.7966 | 98.3438 | 1 | PROCESSED | 57553.5465162037 | 2016-06-14 13:06:59 | 55840 | 2011-10-06 00:00:00 | 55474.0771180556 | 2010-10-05 01:51:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505051010/ | Quick Look | ![]() |
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508 | LDN1563 | 75.5225 | 13.8674 | 74.815655 | 13.796139 | 75.781481 | -8.861998 | 187.1486738 | -16.70848186 | 83.2339 | 56902.1301041667 | 2014-09-02 03:07:21 | 56904.0071643518 | 2014-09-04 00:10:19 | 509075010 | 41.1155 | 80 | 41.1396 | 41.1395 | 0 | 41.1155 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5646296296 | 2016-08-16 13:33:04 | 56748 | 2014-04-01 00:00:00 | 56926.5705439815 | 2014-09-26 13:41:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509075010/ | Quick Look | ![]() |
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509 | 73P/SW3 | 18.1606 | -9.2654 | 17.534064 | -9.530431 | 13.093401 | -15.671197 | 139.58635244 | -71.44823165 | 59.3999 | 53894.1358333333 | 2006-06-08 03:15:36 | 53894.2085416667 | 2006-06-08 05:00:18 | 500014080 | 1.8637 | 35 | 1.8637 | 1.8637 | 1.8637 | 1.8637 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1.9212 | 1.9212 | 6.2779 | 0 | PROCESSED | 57534.5937731482 | 2016-05-26 14:15:02 | 54267 | 2007-06-16 00:00:00 | 54052.5243171296 | 2006-11-13 12:35:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014080/ | Quick Look | ![]() |
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510 | SN1006_BGD1 | 225.9444 | -42.5002 | 225.122216 | -42.305131 | 235.809577 | -24.144105 | 327.43636425 | 13.98792654 | 286.4314 | 56887.5218171296 | 2014-08-18 12:31:25 | 56888.0141203704 | 2014-08-19 00:20:20 | 509083010 | 32.1009 | 30 | 32.1089 | 32.1089 | 0 | 32.1009 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5011111111 | 2016-08-16 12:01:36 | 56748 | 2014-04-01 00:00:00 | 56910.6401736111 | 2014-09-10 15:21:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509083010/ | Quick Look | ![]() |
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511 | 73P/SW3 | 18.3869 | -9.3535 | 17.760674 | -9.618192 | 13.270909 | -15.839893 | 140.33698221 | -71.47421859 | 59.3991 | 53894.4684490741 | 2006-06-08 11:14:34 | 53894.5356365741 | 2006-06-08 12:51:19 | 500014130 | 1.6939 | 35 | 1.6939 | 1.6939 | 1.6939 | 1.6939 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.694 | 1.694 | 5.804 | 0 | PROCESSED | 57534.6023611111 | 2016-05-26 14:27:24 | 54267 | 2007-06-16 00:00:00 | 54052.5234722222 | 2006-11-13 12:33:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014130/ | Quick Look | ![]() |
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512 | ASO0147 | 98.4346 | 6.5402 | 97.762331 | 6.579413 | 98.750752 | -16.644923 | 205.09585789 | -0.932863 | 292.0552 | 54931.9181481482 | 2009-04-10 22:02:08 | 54932.5036921296 | 2009-04-11 12:05:19 | 504047010 | 24.0413 | 20 | 24.0413 | 24.0413 | 0 | 24.0413 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.2409 | 23.2409 | 50.562 | 1 | PROCESSED | 57546.1122685185 | 2016-06-07 02:41:40 | 55324 | 2010-05-08 00:00:00 | 54949.5271180556 | 2009-04-28 12:39:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504047010/ | Quick Look | ![]() |
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513 | G25.5+0.0 | 279.4506 | -6.6057 | 278.777895 | -6.649808 | 279.78518 | 16.514382 | 25.50196825 | 0.00652115 | 74.2354 | 54927.1234490741 | 2009-04-06 02:57:46 | 54928.7446064815 | 2009-04-07 17:52:14 | 504099010 | 52.7375 | 50 | 52.7375 | 52.7375 | 0 | 52.7375 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.5703 | 44.5703 | 140.042 | 3 | PROCESSED | 57546.0819675926 | 2016-06-07 01:58:02 | 54922 | 2009-04-01 00:00:00 | 54949.4845023148 | 2009-04-28 11:37:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504099010/ | Quick Look | ![]() |
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514 | SN1006_BGD2 | 226.2226 | -42.2202 | 225.40133 | -42.0261 | 235.931519 | -23.815123 | 327.76465581 | 14.12663913 | 286.4366 | 56888.0146875 | 2014-08-19 00:21:09 | 56888.6460416667 | 2014-08-19 15:30:18 | 509084010 | 34.8497 | 30 | 34.8793 | 34.8817 | 0 | 34.8497 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5054050926 | 2016-08-16 12:07:47 | 56748 | 2014-04-01 00:00:00 | 56910.6406365741 | 2014-09-10 15:22:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509084010/ | Quick Look | ![]() |
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515 | 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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516 | 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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517 | (L,B)=(0.25,-0.27) | 266.8068 | -28.8823 | 266.012807 | -28.864862 | 267.181973 | -5.472426 | 0.22878525 | -0.27253682 | 265.3343 | 54343.5232986111 | 2007-08-31 12:33:33 | 54346.7919560185 | 2007-09-03 19:00:25 | 502022010 | 134.7904 | 133 | 134.7984 | 134.8064 | 0 | 134.7904 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116.8425 | 116.8425 | 282.3759 | 1 | PROCESSED | 57539.9810185185 | 2016-05-31 23:32:40 | 54724 | 2008-09-15 00:00:00 | 54356.5238657407 | 2007-09-13 12:34:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020044 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma with kT=6-7keV (GCDX). The comparison of Suzaku and VLA 90cm images show a hit for special correlation, suggest a magnetic confinement of GCDX. Thus, in order to search for new SNRs and investigate the galactic latitude dependency of the GCDX, we make a GC observation with the aiming point of (l,b)=(0.25, -0.27). We also see the correlation of GCDX with the radio. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKESHI TSURU | JAP | 2 | AO2 | GLOBAL STRUCTURES OF THE GALACTIC CENTER DIFFUSE X-RAY PLASMA (GCDX) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502022010/ | Quick Look | ![]() |
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518 | GC16 | 267.4868 | -29.3131 | 266.689954 | -29.298954 | 267.787562 | -5.891312 | 0.16607902 | -1.00376926 | 260.5335 | 54383.6397800926 | 2007-10-10 15:21:17 | 54384.0419444444 | 2007-10-11 01:00:24 | 502004010 | 19.873 | 20 | 19.873 | 19.8903 | 0 | 19.8743 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.8321 | 18.8321 | 34.736 | 0 | PROCESSED | 57540.2356597222 | 2016-06-01 05:39:21 | 54771 | 2008-11-01 00:00:00 | 54402.5680208333 | 2007-10-29 13:37:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502004010/ | Quick Look | ![]() |
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519 | 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 | ![]() |
520 | COMET_8P_TUTTLE-P2_17 | 40.6015 | -37.8518 | 40.101512 | -38.064027 | 20.766573 | -50.125126 | 244.68288405 | -64.39021906 | 254.0645 | 54492.1630439815 | 2008-01-27 03:54:47 | 54492.2959953704 | 2008-01-27 07:06:14 | 502063170 | 5.1495 | 5 | 5.1495 | 5.1495 | 0 | 5.1495 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.4142 | 5.4142 | 11.432 | 0 | PROCESSED | 57541.4188425926 | 2016-06-02 10:03:08 | 54912 | 2009-03-22 00:00:00 | 54546.2465509259 | 2008-03-21 05:55:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063170/ | Quick Look | ![]() |
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521 | HESS J1841-55 1 | 279.8307 | -5.8897 | 279.161498 | -5.93564 | 280.231092 | 17.202355 | 26.31151486 | -0.00077944 | 87.7391 | 55645.2916782407 | 2011-03-25 07:00:01 | 55646.4446180556 | 2011-03-26 10:40:15 | 505088010 | 49.652 | 50 | 49.652 | 49.652 | 0 | 49.652 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.8604 | 39.8604 | 99.5978 | 0 | PROCESSED | 57601.3329976852 | 2016-08-01 07:59:31 | 55287 | 2010-04-01 00:00:00 | 55658.1566087963 | 2011-04-07 03:45:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505088010/ | Quick Look | ![]() |
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522 | GC_LARGEPROJECT7 | 265.6744 | -30.0704 | 264.873054 | -30.047455 | 266.222278 | -6.685926 | 358.7007591 | -0.05229538 | 265.9998 | 54725.0356365741 | 2008-09-16 00:51:19 | 54727.1975 | 2008-09-18 04:44:24 | 503013010 | 104.769 | 100 | 104.777 | 104.777 | 0 | 104.769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.9013 | 93.9013 | 186.7098 | 3 | PROCESSED | 57543.8883564815 | 2016-06-04 21:19:14 | 54557 | 2008-04-01 00:00:00 | 54780.5885532407 | 2008-11-10 14:07:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503013010/ | Quick Look | ![]() |
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523 | RXJ_0852-4622_NW_offset | 135.1284 | -47.9102 | 134.705364 | -47.713589 | 163.727844 | -60.335158 | 268.39892579 | -1.13950817 | 140.267 | 53727.3040393518 | 2005-12-23 07:17:49 | 53728.368912037 | 2005-12-24 08:51:14 | 500010020 | 59.1784 | 50 | 59.1784 | 59.1925 | 59.2026 | 59.1925 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63.4821 | 63.4821 | 91.9959 | 0 | PROCESSED | 57532.4967708333 | 2016-05-24 11:55:21 | 54247 | 2007-05-27 00:00:00 | 54039.2486226852 | 2006-10-31 05:58:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | UNA HWANG | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500010020/ | Quick Look | ![]() |
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524 | VELA JR P4 | 132.5157 | -45.5453 | 132.084337 | -45.3579 | 158.164513 | -59.340232 | 265.43667302 | -0.97855833 | 347.0031 | 54286.1062847222 | 2007-07-05 02:33:03 | 54286.4480787037 | 2007-07-05 10:45:14 | 502026010 | 10.9724 | 10 | 10.9724 | 10.9724 | 0 | 10.9724 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.2959 | 11.2959 | 29.5119 | 1 | PROCESSED | 57539.0994791667 | 2016-05-31 02:23:15 | 54759 | 2008-10-20 00:00:00 | 54328.4405787037 | 2007-08-16 10:34:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502026010/ | Quick Look | ![]() |
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525 | GC_LARGEPROJECT12 | 264.5602 | -31.5978 | 263.749148 | -31.569439 | 265.310572 | -8.245043 | 356.8985011 | -0.05173107 | 288.0843 | 54733.394375 | 2008-09-24 09:27:54 | 54733.9377777778 | 2008-09-24 22:30:24 | 503018010 | 29.4012 | 50 | 29.4125 | 29.4125 | 0 | 29.4012 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.6716 | 26.6716 | 46.942 | 0 | PROCESSED | 57543.9951851852 | 2016-06-04 23:53:04 | 54557 | 2008-04-01 00:00:00 | 54780.4814583333 | 2008-11-10 11:33:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018010/ | Quick Look | ![]() |
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526 | GC_LARGEPROJECT14 | 264.2413 | -32.0163 | 263.427554 | -31.98639 | 265.053396 | -8.67384 | 356.39993487 | -0.04727305 | 95.7088 | 54883.0527199074 | 2009-02-21 01:15:55 | 54884.7911342593 | 2009-02-22 18:59:14 | 503020010 | 61.0441 | 50 | 61.0681 | 61.0441 | 0 | 61.0601 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.7185 | 51.7185 | 150.1319 | 1 | PROCESSED | 57545.6307175926 | 2016-06-06 15:08:14 | 54557 | 2008-04-01 00:00:00 | 54895.6029166667 | 2009-03-05 14:28:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503020010/ | Quick Look | ![]() |
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527 | VELA JR P21 | 133.1972 | -46.3295 | 132.769289 | -46.139656 | 159.781258 | -59.750169 | 266.34323773 | -1.11269222 | 347.0005 | 54651.5833680556 | 2008-07-04 14:00:03 | 54652.0557175926 | 2008-07-05 01:20:14 | 503033010 | 14.2872 | 10 | 14.2952 | 14.2872 | 0 | 14.3032 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.0665 | 12.0665 | 40.8019 | 1 | PROCESSED | 57542.9629398148 | 2016-06-03 23:06:38 | 55036 | 2009-07-24 00:00:00 | 54665.3234375 | 2008-07-18 07:45:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503033010/ | Quick Look | ![]() |
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528 | VELA JR P36 | 133.0606 | -47.2239 | 132.639922 | -47.034529 | 160.606122 | -60.550234 | 266.97132611 | -1.75647675 | 346.9998 | 54656.5145833333 | 2008-07-09 12:21:00 | 54656.9168634259 | 2008-07-09 22:00:17 | 503048010 | 11.1226 | 10 | 11.1306 | 11.1226 | 0 | 11.1386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.3838 | 9.3838 | 34.7499 | 1 | PROCESSED | 57543.0132175926 | 2016-06-04 00:19:02 | 55037 | 2009-07-25 00:00:00 | 54670.2692361111 | 2008-07-23 06:27:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503048010/ | Quick Look | ![]() |
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529 | CYGNUS LOOP (P23) | 312.4772 | 32.3587 | 311.966597 | 32.171629 | 327.828669 | 47.6396 | 75.1675214 | -7.32455162 | 61.8892 | 54620.7530439815 | 2008-06-03 18:04:23 | 54621.1473842593 | 2008-06-04 03:32:14 | 503059010 | 19.457 | 15 | 19.457 | 19.457 | 0 | 19.457 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.2771 | 17.2771 | 34.0639 | 0 | PROCESSED | 57542.7106944444 | 2016-06-03 17:03:24 | 55003 | 2009-06-21 00:00:00 | 54636.2328240741 | 2008-06-19 05:35:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503059010/ | Quick Look | ![]() |
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530 | CYGNUS LOOP (P28) | 313.4797 | 29.8934 | 312.955126 | 29.702774 | 327.568716 | 45.03529 | 73.77252886 | -9.54040793 | 49.1005 | 54600.0501273148 | 2008-05-14 01:12:11 | 54600.5334953704 | 2008-05-14 12:48:14 | 503064010 | 18.1693 | 15 | 18.1773 | 18.1853 | 0 | 18.1693 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.443 | 16.443 | 41.756 | 0 | PROCESSED | 57542.5291898148 | 2016-06-03 12:42:02 | 54975 | 2009-05-24 00:00:00 | 54609.1904282407 | 2008-05-23 04:34:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503064010/ | Quick Look | ![]() |
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531 | G18.0-0.7 | 276.56 | -13.5781 | 275.85231 | -13.608204 | 276.459314 | 9.715522 | 18.00442084 | -0.69482715 | 92.0001 | 54909.8982060185 | 2009-03-19 21:33:25 | 54911.080775463 | 2009-03-21 01:56:19 | 503086010 | 52.0592 | 50 | 52.0592 | 52.0672 | 0 | 52.0672 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3036 | 46.3036 | 102.1458 | 2 | PROCESSED | 57547.7369560185 | 2016-06-08 17:41:13 | 55329 | 2010-05-13 00:00:00 | 54923.3684490741 | 2009-04-02 08:50:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | JOSEPH GELFAND | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503086010/ | Quick Look | ![]() |
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532 | GALACTIC_BULGE12 | 270.5539 | -32.7559 | 269.734001 | -32.756597 | 270.462385 | -9.315774 | 358.50046577 | -5.00243267 | 271.4834 | 55119.6475462963 | 2009-10-15 15:32:28 | 55120.7502199074 | 2009-10-16 18:00:19 | 504095010 | 48.2622 | 50 | 48.2622 | 48.2622 | 0 | 48.2622 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 38.358 | 38.358 | 95.2619 | 1 | PROCESSED | 57548.9040856482 | 2016-06-09 21:41:53 | 54922 | 2009-04-01 00:00:00 | 55133.2742824074 | 2009-10-29 06:34:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504095010/ | Quick Look | ![]() |
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533 | 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 | ![]() |
534 | HESS J1718-385 | 259.5578 | -38.4584 | 258.700067 | -38.405877 | 261.528277 | -15.323293 | 348.92137939 | -0.45364037 | 266.9006 | 54706.233599537 | 2008-08-28 05:36:23 | 54706.9286342593 | 2008-08-28 22:17:14 | 503108010 | 23.5097 | 20 | 23.5097 | 23.5097 | 0 | 23.5097 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.4402 | 19.4402 | 60.0479 | 1 | PROCESSED | 57543.4301851852 | 2016-06-04 10:19:28 | 55093 | 2009-09-19 00:00:00 | 54720.4386689815 | 2008-09-11 10:31:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032026 | HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum. | GALACTIC DIFFUSE EMISSION | 5 | A | GERD PUEHLHOFER | EUR | 3 | AO3 | SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503108010/ | Quick Look | ![]() |
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535 | ASO0431 | 286.9632 | 6.0295 | 286.350421 | 5.949691 | 289.23811 | 28.344266 | 40.16756672 | -0.88470452 | 90.0004 | 54936.153287037 | 2009-04-15 03:40:44 | 54936.8141666667 | 2009-04-15 19:32:24 | 504043010 | 24.5222 | 20 | 24.5222 | 24.5222 | 0 | 24.5222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.105 | 18.105 | 57.0739 | 0 | PROCESSED | 57546.1491087963 | 2016-06-07 03:34:43 | 55324 | 2010-05-08 00:00:00 | 54949.5652777778 | 2009-04-28 13:34:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504043010/ | Quick Look | ![]() |
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536 | 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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537 | RIM5 | 311.5286 | 30.6813 | 311.011535 | 30.497677 | 325.775502 | 46.411023 | 73.33464134 | -7.73161485 | 255.8951 | 55155.3611689815 | 2009-11-20 08:40:05 | 55155.7953356482 | 2009-11-20 19:05:17 | 504009010 | 15.8502 | 15 | 15.8502 | 15.8502 | 0 | 15.8502 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2891 | 12.2891 | 37.5039 | 0 | PROCESSED | 57549.4934259259 | 2016-06-10 11:50:32 | 55534 | 2010-12-04 00:00:00 | 55166.4265277778 | 2009-12-01 10:14:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504009010/ | Quick Look | ![]() |
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538 | ASO0304 | 213.3355 | -62.0808 | 212.410984 | -61.846899 | 236.335934 | -45.096122 | 312.3597658 | -0.71761471 | 280.2937 | 55036.9044907407 | 2009-07-24 21:42:28 | 55038.1453935185 | 2009-07-26 03:29:22 | 504054010 | 44.2485 | 40 | 44.2485 | 44.2485 | 0 | 44.2485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0839 | 41.0839 | 107.2018 | 1 | PROCESSED | 57547.9369791667 | 2016-06-08 22:29:15 | 55415 | 2010-08-07 00:00:00 | 55048.3203819444 | 2009-08-05 07:41:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504054010/ | Quick Look | ![]() |
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539 | G346.6-0.2 | 257.5822 | -40.1827 | 256.712432 | -40.120751 | 260.089291 | -17.167114 | 346.62898747 | -0.22219097 | 278.7363 | 55111.704525463 | 2009-10-07 16:54:31 | 55113.1668287037 | 2009-10-09 04:00:14 | 504096010 | 56.7543 | 50 | 56.7543 | 56.7623 | 0 | 56.7703 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4121 | 42.4121 | 126.3239 | 0 | PROCESSED | 57548.806724537 | 2016-06-09 19:21:41 | 54922 | 2009-04-01 00:00:00 | 55127.3766898148 | 2009-10-23 09:02:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504096010/ | Quick Look | ![]() |
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540 | 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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541 | 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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542 | 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 | ![]() |
543 | 73P/SW3 | 317.9167 | 24.1666 | 317.359719 | 23.9609 | 329.535722 | 38.234901 | 71.86402338 | -16.24383714 | 72.7109 | 53868.3425 | 2006-05-13 08:13:12 | 53868.4085532407 | 2006-05-13 09:48:19 | 500013040 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.677 | 2.677 | 5.7039 | 0 | PROCESSED | 57534.2934143518 | 2016-05-26 07:02:31 | 54256 | 2007-06-05 00:00:00 | 54042.2977430556 | 2006-11-03 07:08:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013040/ | Quick Look | ![]() |
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544 | 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 | ![]() |
545 | W44 | 284.0351 | 1.3886 | 283.400736 | 1.32257 | 285.389988 | 24.082424 | 34.70383121 | -0.41279271 | 90.6817 | 55296.8229513889 | 2010-04-10 19:45:03 | 55298.1591898148 | 2010-04-12 03:49:14 | 505004010 | 61.1433 | 60 | 61.1513 | 61.1433 | 0 | 61.1513 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53.7129 | 53.7129 | 115.3999 | 2 | PROCESSED | 57551.2065625 | 2016-06-12 04:57:27 | 55287 | 2010-04-01 00:00:00 | 55313.4281597222 | 2010-04-27 10:16:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505004010/ | Quick Look | ![]() |
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546 | 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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547 | CYGNUS LOOP 8 | 313.6776 | 30.8178 | 313.157016 | 30.626468 | 328.307341 | 45.819556 | 74.60811536 | -9.08900254 | 81.5524 | 55306.7979398148 | 2010-04-20 19:09:02 | 55307.2786689815 | 2010-04-21 06:41:17 | 505016010 | 23.5534 | 21 | 23.5614 | 23.5534 | 0 | 23.5694 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.1989 | 20.1989 | 41.5279 | 0 | PROCESSED | 57551.2800462963 | 2016-06-12 06:43:16 | 55287 | 2010-04-01 00:00:00 | 55364.2401967593 | 2010-06-17 05:45:53 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505016010/ | Quick Look | ![]() |
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548 | L168_B53 | 153.7378 | 48.0763 | 152.957538 | 48.325063 | 136.571096 | 34.402104 | 167.64470811 | 53.18666692 | 109.5667 | 55519.8069328704 | 2010-11-19 19:21:59 | 55521.5828356482 | 2010-11-21 13:59:17 | 505058010 | 79.4999 | 80 | 79.4999 | 79.4999 | 0 | 79.4999 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.6619 | 35.6619 | 153.4218 | 1 | PROCESSED | 57554.2060763889 | 2016-06-15 04:56:45 | 55898 | 2011-12-03 00:00:00 | 55530.2748842593 | 2010-11-30 06:35:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050106 | A dark patch extending degrees scale was found in the R4-band ROSAT All Sky Survey data from our re-analysis of the map based on the recent Suzaku results. The deficiency is small in R5 band . Strikingly the area well coincides with the dark patch in the 408 MHz emission. This indicates the low cosmic-ray and magnetic pressure of this area. We propose to observe this area to determine the temperature of the halo emission using Oxygen lines and to constrain the thermal pressure of hot interstellar medium. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIO SEKIYA | JAP | 5 | AO5 | DARK PATCH IN THE GALACTIC HALO X-RAY EMISSION AND ITS POSSIBLE RELATION TO RADIO SYNCHROTRON RADIATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505058010/ | Quick Look | ![]() |
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549 | DEM L 199 | 81.6473 | -68.8371 | 81.71922 | -68.877404 | 320.411618 | -86.105475 | 279.33316137 | -32.78488249 | 187.7916 | 55551.3246759259 | 2010-12-21 07:47:32 | 55552.146099537 | 2010-12-22 03:30:23 | 505042010 | 51.7434 | 50 | 51.7564 | 51.7434 | 0 | 51.7564 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.2079 | 48.2079 | 70.9659 | 0 | PROCESSED | 57554.4832523148 | 2016-06-15 11:35:53 | 55961 | 2012-02-04 00:00:00 | 55593.2050231482 | 2011-02-01 04:55:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050061 | Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles. | GALACTIC DIFFUSE EMISSION | 5 | C | HIROSHI NAKAJIMA | JAP | 5 | AO5 | UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505042010/ | Quick Look | ![]() |
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550 | 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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551 | VELA SNR CB3 | 129.7826 | -44.6964 | 129.353744 | -44.51903 | 154.049323 | -59.60688 | 263.57338638 | -1.96329272 | 278.1748 | 55318.927974537 | 2010-05-02 22:16:17 | 55319.3418402778 | 2010-05-03 08:12:15 | 505070010 | 18.1718 | 20 | 18.1718 | 18.1718 | 0 | 18.1718 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.1544 | 17.1544 | 35.7539 | 1 | PROCESSED | 57551.3562847222 | 2016-06-12 08:33:03 | 55696 | 2011-05-15 00:00:00 | 55330.1275925926 | 2010-05-14 03:03:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505070010/ | Quick Look | ![]() |
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552 | G12.0-0.1 | 273.0232 | -18.6277 | 272.288654 | -18.640604 | 272.865066 | 4.782958 | 11.94868379 | -0.09019508 | 259.2908 | 54375.5953819444 | 2007-10-02 14:17:21 | 54376.9863310185 | 2007-10-03 23:40:19 | 502001010 | 53.7521 | 53 | 53.7521 | 53.7521 | 0 | 53.7521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.183 | 47.183 | 120.172 | 1 | PROCESSED | 57540.1741898148 | 2016-06-01 04:10:50 | 54751 | 2008-10-12 00:00:00 | 54403.1207986111 | 2007-10-30 02:53:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020010 | We propose an observation of a supernova remnant (SNR) G12.0-0.1 with Suzaku. ASCA discovered X-ray emission from this SNR. The X-ray spectrum exhibit a power-law shape, and the radius and X-ray luminosity estimated from the ASCA results are similar to those of SN 1006, which suggests that it is a SN 1006-like SNR. However, due to the poor statistics, we could not conclude that G12.0-0.1 is SN 1006-like SNR. Precise measurements of the X-ray spectrum with the XIS will provide us with understanding the physical process in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | SHIGEO YAMAUCHI | JAP | 2 | AO2 | SUZAKU OBSERVATION OF G12.0-0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502001010/ | Quick Look | ![]() |
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553 | HESS J1841-55 4 | 280.4555 | -5.2917 | 279.789233 | -5.340638 | 280.927287 | 17.753088 | 27.12788601 | -0.27973073 | 86.6744 | 55648.7926273148 | 2011-03-28 19:01:23 | 55649.9633449074 | 2011-03-29 23:07:13 | 505091010 | 51.2539 | 50 | 51.2539 | 51.2539 | 0 | 51.2539 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.0078 | 45.0078 | 101.142 | 1 | PROCESSED | 57601.3663310185 | 2016-08-01 08:47:31 | 55287 | 2010-04-01 00:00:00 | 55666.3000115741 | 2011-04-15 07:12:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505091010/ | Quick Look | ![]() |
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554 | RCW86_SOUTH | 220.8315 | -62.6734 | 219.843557 | -62.461116 | 241.073682 | -44.079198 | 315.37853465 | -2.53716675 | 96.1597 | 54862.1182291667 | 2009-01-31 02:50:15 | 54863.3647569445 | 2009-02-01 08:45:15 | 503003010 | 54.8181 | 50 | 54.8181 | 54.8181 | 0 | 54.8341 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.3483 | 47.3483 | 107.6848 | 1 | PROCESSED | 57545.4382175926 | 2016-06-06 10:31:02 | 55329 | 2010-05-13 00:00:00 | 54880.5892361111 | 2009-02-18 14:08:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503003010/ | Quick Look | ![]() |
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555 | THE KEPLER SNR | 262.671 | -21.485 | 261.921744 | -21.447676 | 263.170047 | 1.78246 | 4.52284766 | 6.82247636 | 99.4153 | 55649.9685416667 | 2011-03-29 23:14:42 | 55653.0828356482 | 2011-04-02 01:59:17 | 505092070 | 133.3906 | 90 | 133.3986 | 133.3986 | 0 | 133.3906 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112.2172 | 112.2172 | 269.0278 | 1 | PROCESSED | 57601.4459490741 | 2016-08-01 10:42:10 | 55287 | 2010-04-01 00:00:00 | 55666.5226736111 | 2011-04-15 12:32:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092070/ | Quick Look | ![]() |
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556 | VELA JR P20 | 133.6175 | -46.3272 | 133.188109 | -46.13587 | 160.261964 | -59.591088 | 266.52787238 | -0.88873335 | 346.9997 | 54651.2368402778 | 2008-07-04 05:41:03 | 54651.5828009259 | 2008-07-04 13:59:14 | 503032010 | 16.8237 | 10 | 16.8237 | 16.8317 | 0 | 16.8317 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.7982 | 14.7982 | 29.8879 | 0 | PROCESSED | 57542.9499074074 | 2016-06-03 22:47:52 | 55036 | 2009-07-24 00:00:00 | 54665.3228125 | 2008-07-18 07:44:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503032010/ | Quick Look | ![]() |
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557 | W49B | 287.7847 | 9.1157 | 287.186344 | 9.032042 | 290.655059 | 31.28998 | 43.28157058 | -0.18360003 | 89.2671 | 54919.1063888889 | 2009-03-29 02:33:12 | 54920.4689583333 | 2009-03-30 11:15:18 | 503084010 | 52.1549 | 40 | 52.1549 | 52.1549 | 0 | 52.1549 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9512 | 43.9512 | 117.7099 | 2 | PROCESSED | 57547.7422685185 | 2016-06-08 17:48:52 | 55330 | 2010-05-14 00:00:00 | 54931.3622106482 | 2009-04-10 08:41:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030142 | Observations of the W49B supernova remnant for 40 ks is proposed to reveal whether it is a remnant of an anomalous Type Ia supernova or not. To determine the type of the supernova, detailed measurement of less abundand elements such as Cr and Mn will be performed, and abundance of Ni and Ti will be examined. The abundance pattern of those elements in W49B will be compared to that of Tycho's SNR we measured by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | C | TORU TAMAGAWA | JAP | 3 | AO3 | IS W49B A REMNANT OF AN ANOMALOUS TYPE IA SUPERNOVA? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503084010/ | Quick Look | ![]() |
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558 | GAMMACYGNI_NWSHELL1 | 304.9359 | 40.8711 | 304.492598 | 40.71257 | 324.526393 | 57.885883 | 78.38707497 | 2.60425327 | 82.9977 | 55664.4219675926 | 2011-04-13 10:07:38 | 55665.3022222222 | 2011-04-14 07:15:12 | 506017010 | 39.0271 | 40 | 39.0271 | 39.0271 | 0 | 39.0271 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.6965 | 37.6965 | 76.052 | 0 | PROCESSED | 57601.5010416667 | 2016-08-01 12:01:30 | 56058 | 2012-05-11 00:00:00 | 55690.9556597222 | 2011-05-09 22:56:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060059 | We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band. | GALACTIC DIFFUSE EMISSION | 5 | B | YASUYUKI TANAKA | JAP | 6 | AO6 | SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506017010/ | Quick Look | ![]() |
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559 | VELA JR P6 | 133.325 | -45.4847 | 132.890485 | -45.294415 | 159.041125 | -58.989018 | 265.75161327 | -0.50306307 | 347.0024 | 54286.7508449074 | 2007-07-05 18:01:13 | 54286.9863888889 | 2007-07-05 23:40:24 | 502028010 | 11.5072 | 10 | 11.5312 | 11.5232 | 0 | 11.5072 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.2579 | 8.2579 | 20.3439 | 0 | PROCESSED | 57539.1055324074 | 2016-05-31 02:31:58 | 54696 | 2008-08-18 00:00:00 | 54328.3854166667 | 2007-08-16 09:15:00 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502028010/ | Quick Look | ![]() |
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560 | CTB1_SW | 359.716 | 62.4332 | 359.080854 | 62.154888 | 37.143182 | 54.514989 | 116.89133919 | 0.1796486 | 252.1748 | 55924.1262037037 | 2011-12-29 03:01:44 | 55924.6251736111 | 2011-12-29 15:00:15 | 506034010 | 28.9419 | 50 | 28.9419 | 28.9499 | 0 | 28.9499 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.385 | 25.385 | 43.108 | 0 | PROCESSED | 57604.2594675926 | 2016-08-04 06:13:38 | 56313 | 2013-01-21 00:00:00 | 55972.6473958333 | 2012-02-15 15:32:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060086 | CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1. | GALACTIC DIFFUSE EMISSION | 5 | C | SHINYA NAKASHIMA | JAP | 6 | AO6 | NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506034010/ | Quick Look | ![]() |
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561 | MONOGEM RING W1 | 100.4191 | 15.2834 | 99.703498 | 15.332031 | 100.143287 | -7.791413 | 198.20484712 | 4.79777248 | 269.9998 | 55998.5603356482 | 2012-03-12 13:26:53 | 56000.0002314815 | 2012-03-14 00:00:20 | 506053010 | 61.1266 | 60 | 61.1267 | 61.1266 | 0 | 61.1266 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 59.074 | 59.074 | 124.3739 | 1 | PROCESSED | 57604.899849537 | 2016-08-04 21:35:47 | 56382 | 2013-03-31 00:00:00 | 56016.6737152778 | 2012-03-30 16:10:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061316 | We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. | GALACTIC DIFFUSE EMISSION | 5 | C | PAUL PLUCINSKY | USA | 6 | AO6 | STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506053010/ | Quick Look | ![]() |
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562 | G236+38 ON | 146.5345 | 0.5057 | 145.892219 | 0.737078 | 148.588681 | -12.195052 | 235.93345442 | 38.21375915 | 307.3884 | 55713.4761574074 | 2011-06-01 11:25:40 | 55715.0002314815 | 2011-06-03 00:00:20 | 506055010 | 69.8025 | 70 | 69.8025 | 69.8025 | 0 | 69.8025 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.3488 | 64.3488 | 131.674 | 0 | PROCESSED | 57602.2264351852 | 2016-08-02 05:26:04 | 56127 | 2012-07-19 00:00:00 | 55757.6954050926 | 2011-07-15 16:41:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061321 | Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. | GALACTIC DIFFUSE EMISSION | 5 | B | DAVID HENLEY | USA | 6 | AO6 | UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506055010/ | Quick Look | ![]() |
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563 | RXJ1713-3946_ID4 | 258.9125 | -40.0131 | 258.042933 | -39.957471 | 261.134722 | -16.911926 | 347.36417887 | -0.94594655 | 86.0017 | 55244.4787384259 | 2010-02-17 11:29:23 | 55244.8903587963 | 2010-02-17 21:22:07 | 504030010 | 22.1534 | 20 | 22.1774 | 22.1694 | 0 | 22.1534 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.7193 | 19.7193 | 35.5579 | 1 | PROCESSED | 57550.6146412037 | 2016-06-11 14:45:05 | 55622 | 2011-03-02 00:00:00 | 55256.0824768518 | 2010-03-01 01:58:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TADAYUKI TAKAHASHI | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504030010/ | Quick Look | ![]() |
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564 | G292.0+1.8 | 171.1489 | -59.2723 | 170.582246 | -58.997353 | 208.114622 | -55.074076 | 292.03159099 | 1.74911685 | 309.5957 | 55764.9604050926 | 2011-07-22 23:02:59 | 55765.6883449074 | 2011-07-23 16:31:13 | 506062010 | 43.6592 | 40 | 43.6592 | 43.6592 | 0 | 43.6592 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2364 | 40.2364 | 62.8859 | 1 | PROCESSED | 57602.6430902778 | 2016-08-02 15:26:03 | 55652 | 2011-04-01 00:00:00 | 55785.0141782407 | 2011-08-12 00:20:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506062010/ | Quick Look | ![]() |
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565 | FERMI_BUBBLE_S4 | 331.467 | -46.3468 | 330.684504 | -46.590536 | 315.761845 | -32.186623 | 351.15250978 | -52.26066971 | 44.0063 | 56036.1354976852 | 2012-04-19 03:15:07 | 56036.5905324074 | 2012-04-19 14:10:22 | 507012010 | 21.1637 | 20 | 21.1717 | 21.1637 | 0 | 21.1718 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.3816 | 15.3816 | 39.3039 | 0 | PROCESSED | 57605.2132291667 | 2016-08-05 05:07:03 | 56434 | 2013-05-22 00:00:00 | 56068.6280671296 | 2012-05-21 15:04:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507012010/ | Quick Look | ![]() |
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566 | GC_SOUTH_3 | 268.18 | -29.2061 | 267.383741 | -29.195321 | 268.393759 | -5.775192 | 0.56701913 | -1.46906711 | 273.9841 | 56205.6096412037 | 2012-10-05 14:37:53 | 56206.6341898148 | 2012-10-06 15:13:14 | 507030010 | 51.7418 | 50 | 51.7498 | 51.7498 | 0 | 51.7418 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.1911 | 52.1911 | 88.5159 | 0 | PROCESSED | 57607.309537037 | 2016-08-07 07:25:44 | 56595 | 2013-10-30 00:00:00 | 56226.549212963 | 2012-10-26 13:10:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507030010/ | Quick Look | ![]() |
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567 | G32.8-0.1 SOUTH | 282.8163 | -0.2514 | 282.174201 | -0.311644 | 283.889842 | 22.573278 | 32.68848527 | -0.07620379 | 74.5004 | 56038.7902430556 | 2012-04-21 18:57:57 | 56039.916087963 | 2012-04-22 21:59:10 | 507036010 | 52.2324 | 50 | 52.2404 | 52.2324 | 0 | 52.2484 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2432 | 50.2432 | 97.268 | 1 | PROCESSED | 57605.2444560185 | 2016-08-05 05:52:01 | 56421 | 2013-05-09 00:00:00 | 56055.0208564815 | 2012-05-08 00:30:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507036010/ | Quick Look | ![]() |
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568 | COMET_8P_TUTTLE-P1-3 | 28.0473 | 7.5049 | 27.389882 | 7.258447 | 28.728614 | -3.762405 | 148.10975305 | -52.37174422 | 248.4997 | 54470.6493055556 | 2008-01-05 15:35:00 | 54470.7154861111 | 2008-01-05 17:10:18 | 502062030 | 1.9633 | 2 | 1.9633 | 1.9633 | 0 | 1.9633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.905 | 1.905 | 5.718 | 0 | PROCESSED | 57540.9903935185 | 2016-06-01 23:46:10 | 54908 | 2009-03-18 00:00:00 | 54542.2294791667 | 2008-03-17 05:30:27 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062030/ | Quick Look | ![]() |
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569 | SNR HB3 SE-A | 35.6022 | 61.9246 | 34.662678 | 61.696985 | 57.575576 | 44.47157 | 133.41628397 | 0.91883689 | 247.499 | 56322.7203935185 | 2013-01-30 17:17:22 | 56323.4079050926 | 2013-01-31 09:47:23 | 507056010 | 46.748 | 40 | 46.748 | 46.7517 | 0 | 46.7597 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9628 | 43.9628 | 59.3939 | 0 | PROCESSED | 57608.6541666667 | 2016-08-08 15:42:00 | 56709 | 2014-02-21 00:00:00 | 56342.6336921296 | 2013-02-19 15:12:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | JUNICHIRO KATSUTA | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507056010/ | Quick Look | ![]() |
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570 | SGR B | 266.8769 | -28.4429 | 266.085661 | -28.425809 | 267.234018 | -5.031789 | 0.6365241 | -0.09758916 | 267.0001 | 56556.6453472222 | 2013-09-21 15:29:18 | 56559.2640740741 | 2013-09-24 06:20:16 | 508018010 | 101.9558 | 100 | 101.9558 | 101.9558 | 0 | 101.9558 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.894 | 87.894 | 226.2438 | 0 | PROCESSED | 57612.7499768518 | 2016-08-12 17:59:58 | 56956 | 2014-10-26 00:00:00 | 56588.5828125 | 2013-10-23 13:59:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080043 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | MASAYOSHI NOBUKAWA | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508018010/ | Quick Look | ![]() |
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571 | JUPITER | 104.5549 | 23.0543 | 103.799265 | 23.122478 | 103.371966 | 0.286476 | 192.85746904 | 11.70034918 | 267.1462 | 56767.7816087963 | 2014-04-20 18:45:31 | 56768.1147916667 | 2014-04-21 02:45:18 | 508023130 | 10.0906 | 160 | 10.0986 | 10.0986 | 0 | 10.0906 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9649652778 | 2016-08-14 23:09:33 | 57212 | 2015-07-09 00:00:00 | 56782.5091782407 | 2014-05-05 12:13:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023130/ | Quick Look | ![]() |
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572 | G359.0-0.9 S | 266.8698 | -30.3116 | 266.066627 | -30.294444 | 267.268772 | -6.900137 | 359.03431589 | -1.05952932 | 101.9997 | 56724.8167013889 | 2014-03-08 19:36:03 | 56726.0627662037 | 2014-03-10 01:30:23 | 508059010 | 53.4961 | 50 | 53.4961 | 53.5031 | 0 | 53.5201 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 47.9921 | 47.9921 | 107.6559 | 1 | PROCESSED | 57614.0007175926 | 2016-08-14 00:01:02 | 57106 | 2015-03-25 00:00:00 | 56740.7217013889 | 2014-03-24 17:19:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508059010/ | Quick Look | ![]() |
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573 | RX J1713 CENTER | 258.5686 | -39.6657 | 257.702123 | -39.608442 | 260.830462 | -16.587092 | 347.49241435 | -0.52884605 | 86.0002 | 56713.2203125 | 2014-02-25 05:17:15 | 56714.6669212963 | 2014-02-26 16:00:22 | 508068010 | 82.0615 | 80 | 82.0695 | 82.0695 | 0 | 82.0615 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8059 | 34.8059 | 50.3319 | 0 | PROCESSED | 57613.9125231482 | 2016-08-13 21:54:02 | 57089 | 2015-03-08 00:00:00 | 56723.6064699074 | 2014-03-07 14:33:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081313 | Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield. | GALACTIC DIFFUSE EMISSION | 5 | B | FABIO ACERO | USA | 8 | AO8 | STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508068010/ | Quick Look | ![]() |
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574 | COMET_8P_TUTTLE-P2_BGD-1 | 40.599 | -37.8517 | 40.099004 | -38.063935 | 20.76393 | -50.124108 | 244.68396515 | -64.39213957 | 254.2787 | 54492.4296643518 | 2008-01-27 10:18:43 | 54492.562662037 | 2008-01-27 13:30:14 | 502064010 | 6.5707 | 5 | 6.5707 | 6.6024 | 0 | 6.5867 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.6293 | 6.6293 | 11.4879 | 0 | PROCESSED | 57541.4243518518 | 2016-06-02 10:11:04 | 54912 | 2009-03-22 00:00:00 | 54546.2413888889 | 2008-03-21 05:47:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502064010/ | Quick Look | ![]() |
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575 | CTB109 SOUTHWEST | 345.0971 | 58.7572 | 344.575762 | 58.488555 | 23.478605 | 56.879692 | 108.94859975 | -1.06655489 | 252.0045 | 55909.1993287037 | 2011-12-14 04:47:02 | 55910.0807407407 | 2011-12-15 01:56:16 | 506038010 | 41.3824 | 40 | 41.3904 | 41.3824 | 0 | 41.3984 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.779 | 38.779 | 76.1358 | 0 | PROCESSED | 57604.1454282407 | 2016-08-04 03:29:25 | 56289 | 2012-12-28 00:00:00 | 55921.9811574074 | 2011-12-26 23:32:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | TOSHIO NAKANO | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506038010/ | Quick Look | ![]() |
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576 | ARC1 | 40.8605 | -42.0069 | 40.383748 | -42.218277 | 17.737941 | -53.844666 | 253.28744097 | -62.75503946 | 235.1247 | 54480.7980787037 | 2008-01-15 19:09:14 | 54482.7640509259 | 2008-01-17 18:20:14 | 502070010 | 104.3694 | 100 | 104.3774 | 104.3854 | 0 | 104.3694 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 115.4202 | 115.4202 | 169.8377 | 3 | PROCESSED | 57541.3640277778 | 2016-06-02 08:44:12 | 54860 | 2009-01-29 00:00:00 | 54490.7270717593 | 2008-01-25 17:26:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBIN SHELTON | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502070010/ | Quick Look | ![]() |
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577 | W49B | 287.784 | 9.1149 | 287.185641 | 9.031245 | 290.654125 | 31.289286 | 43.28054167 | -0.18335704 | 82.0063 | 57131.6619444445 | 2015-04-19 15:53:12 | 57133.5779513889 | 2015-04-21 13:52:15 | 509001040 | 67.3182 | 400 | 67.3182 | 67.3182 | 0 | 67.3262 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0264699074 | 2016-08-18 00:38:07 | 56748 | 2014-04-01 00:00:00 | 57224.4531481482 | 2015-07-21 10:52:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001040/ | Quick Look | ![]() |
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578 | VELA PWN GEV1 | 127.6995 | -44.6062 | 127.276202 | -44.43674 | 151.392903 | -60.265182 | 262.61398048 | -3.09706524 | 119.7191 | 56985.3954282407 | 2014-11-24 09:29:25 | 56985.8502546296 | 2014-11-24 20:24:22 | 509011010 | 19.1492 | 15 | 19.1572 | 19.1652 | 0 | 19.1492 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8102893518 | 2016-08-16 19:26:49 | 57365 | 2015-12-09 00:00:00 | 57009.4123726852 | 2014-12-18 09:53:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509011010/ | Quick Look | ![]() |
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579 | G166.0+4.3_NW | 81.4339 | 42.9094 | 80.537947 | 42.865797 | 83.349134 | 19.666732 | 166.05797128 | 4.14809941 | 85.1436 | 56920.3100347222 | 2014-09-20 07:26:27 | 56921.2397106482 | 2014-09-21 05:45:11 | 509023010 | 39.7982 | 40 | 39.7982 | 42.0339 | 0 | 42.0259 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5613078704 | 2016-08-16 13:28:17 | 57298 | 2015-10-03 00:00:00 | 56940.6722569444 | 2014-10-10 16:08:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509023010/ | Quick Look | ![]() |
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580 | CIZA J1358.9-4750_SW | 209.5053 | -47.9232 | 208.715208 | -47.679899 | 225.712458 | -33.34381 | 314.31638856 | 13.47131455 | 293 | 56882.719537037 | 2014-08-13 17:16:08 | 56883.5528356482 | 2014-08-14 13:16:05 | 509027010 | 42.0308 | 40 | 42.0308 | 42.0548 | 0 | 42.0388 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.0109 | 7.0109 | 14.276 | 0 | PROCESSED | 57616.4982175926 | 2016-08-16 11:57:26 | 57267 | 2015-09-02 00:00:00 | 56898.5152662037 | 2014-08-29 12:21:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | YUICHI KATO | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509027010/ | Quick Look | ![]() |
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581 | ARC_BACKGROUND | 39.8321 | -35.8483 | 39.320146 | -36.062945 | 21.353527 | -48.064568 | 240.48423372 | -65.50115915 | 257.6627 | 54496.6274537037 | 2008-01-31 15:03:32 | 54499.812662037 | 2008-02-03 19:30:14 | 502072010 | 0 | 100 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 105.161 | 105.161 | 275.1537 | 4 | PROCESSED | 57541.5227314815 | 2016-06-02 12:32:44 | 54883 | 2009-02-21 00:00:00 | 54515.6371875 | 2008-02-19 15:17:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | ROBIN SHELTON | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502072010/ | Quick Look | ![]() |
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582 | MBM20 | 68.9409 | -14.6227 | 68.368213 | -14.724058 | 64.473913 | -36.217726 | 211.39642208 | -36.55928879 | 252.4258 | 54507.612025463 | 2008-02-11 14:41:19 | 54510.6980439815 | 2008-02-14 16:45:11 | 502075010 | 107.0668 | 100 | 107.0668 | 107.0668 | 0 | 107.0668 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.8036 | 92.8036 | 266.6036 | 2 | PROCESSED | 57541.6362847222 | 2016-06-02 15:16:15 | 54889 | 2009-02-27 00:00:00 | 54522.4496527778 | 2008-02-26 10:47:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | MASSIMILIANO GALEAZZI | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502075010/ | Quick Look | ![]() |
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583 | 3C 396 | 285.987 | 5.4347 | 285.37156 | 5.359452 | 288.059681 | 27.878529 | 39.1930056 | -0.29514711 | 64.6066 | 56773.2792592593 | 2014-04-26 06:42:08 | 56775.1223726852 | 2014-04-28 02:56:13 | 509038010 | 82.7922 | 80 | 82.7922 | 82.7922 | 0 | 82.7922 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1.0111 | 1.0111 | 1.744 | 0 | PROCESSED | 57614.9978703704 | 2016-08-14 23:56:56 | 57157 | 2015-05-15 00:00:00 | 56789.6241782407 | 2014-05-12 14:58:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091315 | We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | B | THOMAS PANNUTI | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509038010/ | Quick Look | ![]() |
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584 | MBM20 | 68.9408 | -14.6235 | 68.368117 | -14.724858 | 64.47362 | -36.218496 | 211.39729046 | -36.55969232 | 255.8156 | 57069.9923842593 | 2015-02-16 23:49:02 | 57071.9654050926 | 2015-02-18 23:10:11 | 509076010 | 81.154 | 80 | 81.154 | 81.162 | 0 | 81.162 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.624537037 | 2016-08-17 14:59:20 | 56748 | 2014-04-01 00:00:00 | 57083.4173032407 | 2015-03-02 10:00:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509076010/ | Quick Look | ![]() |
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585 | VELA JR P34 | 132.1138 | -46.9499 | 131.694344 | -46.763927 | 159.20149 | -60.674913 | 266.35035002 | -2.0812575 | 347.0005 | 54656.0096990741 | 2008-07-09 00:13:58 | 54656.2634143518 | 2008-07-09 06:19:19 | 503046010 | 11.0421 | 10 | 11.0581 | 11.0421 | 0 | 11.0581 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.1306 | 11.1306 | 21.916 | 0 | PROCESSED | 57543.0076967593 | 2016-06-04 00:11:05 | 55037 | 2009-07-25 00:00:00 | 54670.2236342593 | 2008-07-23 05:22:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503046010/ | Quick Look | ![]() |
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586 | VELA JR P37 | 132.6136 | -47.1701 | 132.194095 | -46.982326 | 160.029329 | -60.672793 | 266.73640279 | -1.95651055 | 346.9993 | 54656.9174768518 | 2008-07-09 22:01:10 | 54657.2418287037 | 2008-07-10 05:48:14 | 503049010 | 12.5294 | 10 | 12.5414 | 12.5294 | 0 | 12.5454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.8527 | 12.8527 | 28.02 | 0 | PROCESSED | 57543.0205671296 | 2016-06-04 00:29:37 | 55037 | 2009-07-25 00:00:00 | 54670.278900463 | 2008-07-23 06:41:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503049010/ | Quick Look | ![]() |
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587 | WESTERLUND 2 | 156.0088 | -57.7448 | 155.54834 | -57.490842 | 195.724597 | -59.560466 | 284.2643696 | -0.3172737 | 343.7602 | 54687.6527199074 | 2008-08-09 15:39:55 | 54689.327962963 | 2008-08-11 07:52:16 | 503053010 | 73.67 | 100 | 73.67 | 73.67 | 0 | 73.67 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5776 | 86.5776 | 144.7298 | 0 | PROCESSED | 57543.2480555556 | 2016-06-04 05:57:12 | 55252 | 2010-02-25 00:00:00 | 54706.476412037 | 2008-08-28 11:26:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030059 | Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. | GALACTIC DIFFUSE EMISSION | 5 | A | YUTAKA FUJITA | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503053010/ | Quick Look | ![]() |
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588 | WESTERLUND 2 | 155.9878 | -57.7462 | 155.527496 | -57.492284 | 195.71117 | -59.569482 | 284.25564056 | -0.32444098 | 166.5036 | 54866.5949189815 | 2009-02-04 14:16:41 | 54867.1669444444 | 2009-02-05 04:00:24 | 503053020 | 33.4924 | 30 | 33.5004 | 33.4924 | 0 | 33.5004 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.073 | 32.073 | 49.4159 | 1 | PROCESSED | 57545.4584606482 | 2016-06-06 11:00:11 | 55329 | 2010-05-13 00:00:00 | 54880.5574189815 | 2009-02-18 13:22:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030059 | Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. | GALACTIC DIFFUSE EMISSION | 5 | A | YUTAKA FUJITA | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503053020/ | Quick Look | ![]() |
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589 | HESS J1745-303B | 266.0577 | -30.545 | 265.253177 | -30.523904 | 266.569275 | -7.150762 | 358.47050833 | -0.58308172 | 102.2921 | 55254.6768634259 | 2010-02-27 16:14:41 | 55255.9515509259 | 2010-02-28 22:50:14 | 504002010 | 53.0609 | 50 | 53.0609 | 53.0609 | 0 | 53.0609 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.585 | 46.585 | 110.1219 | 1 | PROCESSED | 57550.7606481482 | 2016-06-11 18:15:20 | 55636 | 2011-03-16 00:00:00 | 55267.2715856482 | 2010-03-12 06:31:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504002010/ | Quick Look | ![]() |
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590 | ASO0218 | 157.1332 | -58.313 | 156.668691 | -58.056852 | 197.346686 | -59.525927 | 285.06973918 | -0.48663651 | 315.2825 | 55020.3423148148 | 2009-07-08 08:12:56 | 55020.9467476852 | 2009-07-08 22:43:19 | 504045010 | 22.8449 | 20 | 22.8449 | 22.8449 | 0 | 22.8449 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1544 | 21.1544 | 52.2179 | 1 | PROCESSED | 57547.7933680556 | 2016-06-08 19:02:27 | 55400 | 2010-07-23 00:00:00 | 55034.2716898148 | 2009-07-22 06:31:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504045010/ | Quick Look | ![]() |
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591 | GALACTIC_BULGE13 | 264.5912 | -32.1955 | 263.77613 | -32.167278 | 265.360141 | -8.841295 | 356.40747371 | -0.39354159 | 92.0351 | 55635.5794907407 | 2011-03-15 13:54:28 | 55636.621099537 | 2011-03-16 14:54:23 | 505082010 | 48.4969 | 50 | 48.5129 | 48.5129 | 0 | 48.4969 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.255 | 41.255 | 89.9798 | 0 | PROCESSED | 57601.201412037 | 2016-08-01 04:50:02 | 55287 | 2010-04-01 00:00:00 | 55648.3385763889 | 2011-03-28 08:07:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505082010/ | Quick Look | ![]() |
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592 | CYGNUS LOOP 6 | 314.1656 | 31.2305 | 313.646001 | 31.037451 | 329.094604 | 46.032553 | 75.19999907 | -9.14964477 | 81.8988 | 55301.8924189815 | 2010-04-15 21:25:05 | 55302.1398148148 | 2010-04-16 03:21:20 | 505014010 | 12.4623 | 10 | 12.4783 | 12.4623 | 0 | 12.4783 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.0683 | 12.0683 | 21.3599 | 0 | PROCESSED | 57551.2257060185 | 2016-06-12 05:25:01 | 55287 | 2010-04-01 00:00:00 | 55362.3410532407 | 2010-06-15 08:11:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505014010/ | Quick Look | ![]() |
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593 | SNR G106.3+2.7 P3 | 336.5055 | 60.7692 | 336.063779 | 60.514367 | 20.620799 | 61.417005 | 106.0859109 | 2.74547808 | 12.2692 | 55424.0215509259 | 2010-08-16 00:31:02 | 55424.9841782407 | 2010-08-16 23:37:13 | 505073010 | 50.4548 | 50 | 50.4628 | 50.4548 | 0 | 50.4632 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2105 | 50.2105 | 83.1639 | 1 | PROCESSED | 57553.1155439815 | 2016-06-14 02:46:23 | 55805 | 2011-09-01 00:00:00 | 55439.1312037037 | 2010-08-31 03:08:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051305 | After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. | GALACTIC DIFFUSE EMISSION | 5 | C | ESTER ALIU | USA | 5 | AO5 | ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505073010/ | Quick Look | ![]() |
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594 | CYGNUS LOOP 12 | 313.6077 | 30.3526 | 313.085044 | 30.161518 | 327.967179 | 45.415269 | 74.20451075 | -9.33661335 | 82.0022 | 55329.1256944444 | 2010-05-13 03:01:00 | 55329.8391666667 | 2010-05-13 20:08:24 | 505020010 | 27.8427 | 28 | 27.8507 | 27.8507 | 0 | 27.8427 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0522 | 21.0522 | 61.64 | 0 | PROCESSED | 57551.5093055556 | 2016-06-12 12:13:24 | 55287 | 2010-04-01 00:00:00 | 55393.4203009259 | 2010-07-16 10:05:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505020010/ | Quick Look | ![]() |
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595 | FVW319.8+0.3_BGD | 225.4141 | -58.3766 | 224.455219 | -58.179449 | 241.611855 | -39.24635 | 319.32044374 | 0.28957352 | 278.3765 | 55413.9313888889 | 2010-08-05 22:21:12 | 55414.6724768518 | 2010-08-06 16:08:22 | 505030010 | 51.6262 | 50 | 51.6262 | 51.6636 | 0 | 51.6476 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.0503 | 40.0503 | 64.0179 | 1 | PROCESSED | 57552.8534837963 | 2016-06-13 20:29:01 | 55793 | 2011-08-20 00:00:00 | 55427.2012152778 | 2010-08-19 04:49:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050010 | Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 5 | AO5 | SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505030010/ | Quick Look | ![]() |
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596 | DEM L 86 | 77.4674 | -68.8946 | 77.532288 | -68.954899 | 328.060855 | -84.723884 | 279.75652902 | -34.25087364 | 194.4731 | 55552.1478703704 | 2010-12-22 03:32:56 | 55552.9495601852 | 2010-12-22 22:47:22 | 505041010 | 51.4681 | 50 | 51.4997 | 51.4997 | 0 | 51.4681 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.2589 | 44.2589 | 69.2579 | 0 | PROCESSED | 57554.4839236111 | 2016-06-15 11:36:51 | 55973 | 2012-02-16 00:00:00 | 55607.0926851852 | 2011-02-15 02:13:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050061 | Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles. | GALACTIC DIFFUSE EMISSION | 5 | C | HIROSHI NAKAJIMA | JAP | 5 | AO5 | UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505041010/ | Quick Look | ![]() |
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597 | VELA SNR CB1 | 130.2067 | -44.4709 | 129.774891 | -44.291952 | 154.339696 | -59.260079 | 263.57895082 | -1.58638955 | 294.2634 | 55318.1574074074 | 2010-05-02 03:46:40 | 55318.5738425926 | 2010-05-02 13:46:20 | 505068010 | 23.6665 | 20 | 23.6665 | 23.678 | 0 | 23.6665 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.818 | 18.818 | 35.9759 | 1 | PROCESSED | 57551.3448842593 | 2016-06-12 08:16:38 | 55696 | 2011-05-15 00:00:00 | 55330.1358449074 | 2010-05-14 03:15:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505068010/ | Quick Look | ![]() |
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598 | HESS J1841-55 2 | 280.1473 | -5.9564 | 279.477798 | -6.003856 | 280.554771 | 17.113097 | 26.39650339 | -0.31125339 | 87.3564 | 55646.4452777778 | 2011-03-26 10:41:12 | 55647.6391550926 | 2011-03-27 15:20:23 | 505089010 | 50.0053 | 50 | 50.0304 | 50.0053 | 0 | 50.0304 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43.1789 | 43.1789 | 103.1139 | 0 | PROCESSED | 57601.3264236111 | 2016-08-01 07:50:03 | 55287 | 2010-04-01 00:00:00 | 55658.2084606482 | 2011-04-07 05:00:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505089010/ | Quick Look | ![]() |
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599 | JUPITER | 28.7092 | 10.4688 | 28.044402 | 10.223855 | 30.381154 | -1.215152 | 147.29554938 | -49.38035583 | 249.1847 | 55930.8245717593 | 2012-01-04 19:47:23 | 55931.8508564815 | 2012-01-05 20:25:14 | 506006020 | 35.518 | 160 | 35.522 | 35.518 | 0 | 35.526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.367 | 34.367 | 88.6599 | 0 | PROCESSED | 57604.3110185185 | 2016-08-04 07:27:52 | 56316 | 2013-01-24 00:00:00 | 55946.2294097222 | 2012-01-20 05:30:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006020/ | Quick Look | ![]() |
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600 | CTB1_NE | 0.2869 | 62.6043 | 359.6465 | 62.325973 | 37.675416 | 54.459267 | 117.18345572 | 0.29518062 | 253.7193 | 55923.0281134259 | 2011-12-28 00:40:29 | 55924.1251736111 | 2011-12-29 03:00:15 | 506035010 | 52.666 | 50 | 52.666 | 52.666 | 0 | 52.666 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3108 | 48.3108 | 94.7759 | 3 | PROCESSED | 57604.2722569444 | 2016-08-04 06:32:03 | 56313 | 2013-01-21 00:00:00 | 55972.6734490741 | 2012-02-15 16:09:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060086 | CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1. | GALACTIC DIFFUSE EMISSION | 5 | C | SHINYA NAKASHIMA | JAP | 6 | AO6 | NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506035010/ | Quick Look | ![]() |
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601 | W28WEST | 269.8372 | -23.6072 | 269.074768 | -23.604556 | 269.841247 | -0.166403 | 6.15250357 | 0.06606197 | 270.1135 | 55844.0583217593 | 2011-10-10 01:23:59 | 55848.1342708333 | 2011-10-14 03:13:21 | 506036010 | 151.0892 | 150 | 151.0972 | 151.0892 | 0 | 151.0923 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 128.9797 | 128.9797 | 352.1259 | 2 | PROCESSED | 57603.4758449074 | 2016-08-03 11:25:13 | 56240 | 2012-11-09 00:00:00 | 55872.5113425926 | 2011-11-07 12:16:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060095 | W28 is a mixed-morphology supernova remnant (MM SNR). Recently, GeV and TeV gamma-ray emission have been detected from the eastern edge of W28. On the other hand, we have observed the central region of W28 and have detected an over-ionized plasma, which can not be produced in the canonical evolution of SNRs. Several SNRs have been turned out to host a over-ionized plasma. All of them are MM SNR and are showing GeV and/or TeV emission. This indicates that there are some physical connections between the existence of high-energy cosmic rays and over-ionized plasma. W28 is the best place to study this possible connection due to the large apparent size. Thus, we propose Suzaku observation of western region of W28, which has not been covered by the previous mapping observations. | GALACTIC DIFFUSE EMISSION | 5 | A | MAKOTO SAWADA | JAP | 6 | AO6 | THE SNR W28 - SEARCHING FOR THE PHYSICAL CONNECTION BETWEEN HIGH-ENERGY COSMIC RAYS AND OVER-IONIZED PLASMA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506036010/ | Quick Look | ![]() |
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602 | MONOGEM RING W2 | 97.483 | 17.0349 | 96.757694 | 17.069404 | 97.197447 | -6.219287 | 195.35325463 | 3.08684005 | 270 | 56001.1430439815 | 2012-03-15 03:25:59 | 56002.5487384259 | 2012-03-16 13:10:11 | 506054010 | 62.5933 | 60 | 62.5933 | 62.5933 | 0 | 62.5933 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.9669 | 59.9669 | 121.4439 | 1 | PROCESSED | 57604.9251967593 | 2016-08-04 22:12:17 | 56385 | 2013-04-03 00:00:00 | 56019.3467592593 | 2012-04-02 08:19:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061316 | We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. | GALACTIC DIFFUSE EMISSION | 5 | C | PAUL PLUCINSKY | USA | 6 | AO6 | STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506054010/ | Quick Look | ![]() |
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603 | FERMI_BUBBLE_S2 | 330.2693 | -46.4894 | 329.48073 | -46.73026 | 314.804008 | -31.978019 | 351.28666586 | -51.42688059 | 44.0074 | 56035.2081018518 | 2012-04-18 04:59:40 | 56035.6736921296 | 2012-04-18 16:10:07 | 507010010 | 20.3496 | 20 | 20.3576 | 20.3496 | 0 | 20.3648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.278 | 14.278 | 40.2139 | 0 | PROCESSED | 57605.1975231482 | 2016-08-05 04:44:26 | 56420 | 2013-05-08 00:00:00 | 56049.1880555556 | 2012-05-02 04:30:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507010010/ | Quick Look | ![]() |
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604 | VELA JR P31 | 133.8003 | -46.8845 | 133.374404 | -46.692518 | 161.076222 | -59.989175 | 267.03483855 | -1.15221367 | 347.0003 | 54655.085 | 2008-07-08 02:02:24 | 54655.3273032407 | 2008-07-08 07:51:19 | 503043010 | 11.2095 | 10 | 11.2175 | 11.2255 | 0 | 11.2095 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.542 | 11.542 | 20.9279 | 0 | PROCESSED | 57542.9998263889 | 2016-06-03 23:59:45 | 55048 | 2009-08-05 00:00:00 | 54679.372974537 | 2008-08-01 08:57:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503043010/ | Quick Look | ![]() |
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605 | LDN1563 | 75.5223 | 13.867 | 74.815457 | 13.795738 | 75.781245 | -8.862376 | 187.14890409 | -16.70886793 | 81.7388 | 56161.9528356482 | 2012-08-22 22:52:05 | 56164.0488194444 | 2012-08-25 01:10:18 | 507078010 | 78.6693 | 80 | 78.6693 | 78.6693 | 0 | 78.6693 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.6801 | 69.6801 | 181.0619 | 0 | PROCESSED | 57606.963275463 | 2016-08-06 23:07:07 | 56018 | 2012-04-01 00:00:00 | 56212.8492476852 | 2012-10-12 20:22:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507078010/ | Quick Look | ![]() |
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606 | RX J1713.7-3946 NE | 258.6449 | -39.4419 | 257.780148 | -39.385009 | 260.872484 | -16.359233 | 347.70840856 | -0.44579664 | 85.9991 | 56714.667349537 | 2014-02-26 16:00:59 | 56716.5279513889 | 2014-02-28 12:40:15 | 508017010 | 100.6728 | 100 | 100.7048 | 100.6968 | 0 | 100.6728 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 104.394 | 104.394 | 160.7277 | 1 | PROCESSED | 57613.9490162037 | 2016-08-13 22:46:35 | 57093 | 2015-03-12 00:00:00 | 56727.6718865741 | 2014-03-11 16:07:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080029 | We proposed Suzaku observation of a thermal emission line in the young TeV gamma-ray SNR RX J1713.7-3946. Most recently, we found the candidate of thermal emission line toward North-East of the SNR analyzed with Suzaku archive data. The region is present in the vicinity of the small molecular cloud interacts with the SNR shock wave. Main purpose is significant detection of the Si line about 5 sigma. This observation will be observable only with Suzaku and lead to a large step forward on cosmic-ray acceleration and shock-cloud interaction in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | HIDETOSHI SANO | JAP | 8 | AO8 | SUZAKU OBSERVATION OF A THERMAL EMISSION LINE IN THE SNR RX J1713.7-3946 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508017010/ | Quick Look | ![]() |
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607 | JUPITER | 103.9685 | 23.1027 | 103.212311 | 23.168111 | 102.830346 | 0.281775 | 192.5818164 | 11.23089407 | 264.4391 | 56763.3891666667 | 2014-04-16 09:20:24 | 56763.722349537 | 2014-04-16 17:20:11 | 508023050 | 14.3106 | 160 | 14.3106 | 14.3207 | 0 | 14.3207 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9511111111 | 2016-08-14 22:49:36 | 57212 | 2015-07-09 00:00:00 | 56782.4912731482 | 2014-05-05 11:47:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023050/ | Quick Look | ![]() |
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608 | VELA JR WEST2 | 131.7715 | -45.9871 | 131.345884 | -45.80238 | 157.754454 | -59.989666 | 265.452568 | -1.6600557 | 116.213 | 56619.4434490741 | 2013-11-23 10:38:34 | 56620.0800115741 | 2013-11-24 01:55:13 | 508037010 | 29.185 | 30 | 29.193 | 29.201 | 0 | 29.185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0652 | 35.0652 | 54.9859 | 1 | PROCESSED | 57613.3840277778 | 2016-08-13 09:13:00 | 56995 | 2014-12-04 00:00:00 | 56629.6443055556 | 2013-12-03 15:27:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDETOSHI SANO | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508037010/ | Quick Look | ![]() |
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609 | G359.0-0.9 NE | 266.7211 | -30.1578 | 265.918955 | -30.139926 | 267.135952 | -6.749255 | 359.09932581 | -0.86996543 | 100.9984 | 56720.9624537037 | 2014-03-04 23:05:56 | 56722.041875 | 2014-03-06 01:00:18 | 508057010 | 49.8156 | 50 | 49.8156 | 49.8396 | 0 | 49.8236 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 45.0097 | 45.0097 | 93.2479 | 1 | PROCESSED | 57613.9450925926 | 2016-08-13 22:40:56 | 57102 | 2015-03-21 00:00:00 | 56740.6678009259 | 2014-03-24 16:01:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508057010/ | Quick Look | ![]() |
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610 | VELA PWN S1 | 128.1818 | -46.8811 | 127.77491 | -46.709753 | 154.389152 | -62.054406 | 264.65396784 | -4.16648977 | 122.1894 | 56988.5541087963 | 2014-11-27 13:17:55 | 56988.8905324074 | 2014-11-27 21:22:22 | 509017010 | 15.4638 | 15 | 15.4638 | 15.4878 | 0 | 15.7838 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8238194444 | 2016-08-16 19:46:18 | 57368 | 2015-12-12 00:00:00 | 57002.4344328704 | 2014-12-11 10:25:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509017010/ | Quick Look | ![]() |
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611 | G166.0+4.3_NE | 81.7708 | 42.9893 | 80.873891 | 42.947312 | 83.615806 | 19.731256 | 166.12860985 | 4.39756168 | 84.8043 | 56919.0138773148 | 2014-09-19 00:19:59 | 56920.3092824074 | 2014-09-20 07:25:22 | 509022010 | 54.3942 | 60 | 54.3942 | 61.5931 | 0 | 61.5931 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5656134259 | 2016-08-16 13:34:29 | 57296 | 2015-10-01 00:00:00 | 56940.6693981482 | 2014-10-10 16:03:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509022010/ | Quick Look | ![]() |
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612 | OFF-FIELD5 | 318.3256 | -10.4856 | 317.650019 | -10.692475 | 317.524522 | 5.342962 | 39.92155172 | -36.21028826 | 81.4906 | 56787.0661226852 | 2014-05-10 01:35:13 | 56789.4168171296 | 2014-05-12 10:00:13 | 509046010 | 80.908 | 80 | 80.908 | 80.908 | 0 | 80.908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.3404 | 71.3404 | 203.0697 | 2 | PROCESSED | 57615.126724537 | 2016-08-15 03:02:29 | 56748 | 2014-04-01 00:00:00 | 56806.674212963 | 2014-05-29 16:10:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | ANJALI GUPTA | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509046010/ | Quick Look | ![]() |
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613 | 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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614 | 73P/SW3 | 17.8996 | -9.1693 | 17.272719 | -9.434717 | 12.886588 | -15.48163 | 138.7272506 | -71.42013328 | 59.3998 | 53893.8025 | 2006-06-07 19:15:36 | 53893.8689699074 | 2006-06-07 20:51:19 | 500014030 | 3.2361 | 35 | 3.2361 | 3.2361 | 3.2361 | 3.2361 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.4331 | 2.4331 | 5.7359 | 0 | PROCESSED | 57534.5821875 | 2016-05-26 13:58:21 | 54267 | 2007-06-16 00:00:00 | 54052.5088310185 | 2006-11-13 12:12:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014030/ | Quick Look | ![]() |
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615 | 73P/SW3 | 18.2084 | -9.2837 | 17.581929 | -9.54866 | 13.13101 | -15.70655 | 139.744498 | -71.45365551 | 59.3985 | 53894.2087384259 | 2006-06-08 05:00:35 | 53894.2689467593 | 2006-06-08 06:27:17 | 500014090 | 1.5089 | 35 | 1.5089 | 1.5089 | 1.5089 | 1.5089 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1.6552 | 1.6552 | 5.202 | 0 | PROCESSED | 57534.5937037037 | 2016-05-26 14:14:56 | 54267 | 2007-06-16 00:00:00 | 54052.5382986111 | 2006-11-13 12:55:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500014090/ | Quick Look | ![]() |
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616 | CYGNUS LOOP NE1 | 314.1885 | 31.738 | 313.671289 | 31.544868 | 329.414773 | 46.489683 | 75.60815027 | -8.84073861 | 223.0005 | 53697.7354282407 | 2005-11-23 17:39:01 | 53698.2051388889 | 2005-11-24 04:55:24 | 500020010 | 20.3437 | 20 | 20.3517 | 20.3517 | 20.3517 | 20.3437 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17.992 | 17.992 | 40.5759 | 0 | PROCESSED | 57528.0684837963 | 2016-05-20 01:38:37 | 54247 | 2007-05-27 00:00:00 | 54037.9167476852 | 2006-10-29 22:00:07 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500020010/ | Quick Look | ![]() |
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617 | CYGNUS LOOP NE2 | 313.9681 | 31.9542 | 313.452396 | 31.761838 | 329.292075 | 46.763002 | 75.65570239 | -8.55863001 | 223.0005 | 53698.2056134259 | 2005-11-24 04:56:05 | 53698.6766666667 | 2005-11-24 16:14:24 | 500021010 | 21.4135 | 20 | 21.4455 | 21.4375 | 21.4295 | 21.4135 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.6541 | 21.6541 | 40.6939 | 0 | PROCESSED | 57528.0693518518 | 2016-05-20 01:39:52 | 54247 | 2007-05-27 00:00:00 | 54038.4014351852 | 2006-10-30 09:38:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500021010/ | Quick Look | ![]() |
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618 | 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 | ![]() |
619 | HIGH LAT. DIFFUSE B | 38.7468 | -52.2774 | 38.331334 | -52.495237 | 4.39034 | -61.411521 | 272.40280946 | -58.27300774 | 280.6379 | 53783.933900463 | 2006-02-17 22:24:49 | 53786.5211111111 | 2006-02-20 12:30:24 | 500027020 | 103.553 | 100 | 103.553 | 103.561 | 103.561 | 103.561 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68.6094 | 68.6094 | 223.5238 | 3 | PROCESSED | 57533.0790972222 | 2016-05-25 01:53:54 | 54247 | 2007-05-27 00:00:00 | 54041.5670717593 | 2006-11-02 13:36:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000044 | We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500027020/ | Quick Look | ![]() |
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620 | 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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621 | GC14 | 267.1584 | -29.141 | 266.362704 | -29.125263 | 267.496319 | -5.724596 | 0.16624555 | -0.66947426 | 260.5381 | 54382.6950694444 | 2007-10-09 16:40:54 | 54383.1530555556 | 2007-10-10 03:40:24 | 502002010 | 23.1903 | 20 | 23.2063 | 23.1903 | 0 | 23.2063 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.9329 | 20.9329 | 39.5599 | 0 | PROCESSED | 57540.2209490741 | 2016-06-01 05:18:10 | 54771 | 2008-11-01 00:00:00 | 54402.7240740741 | 2007-10-29 17:22:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502002010/ | Quick Look | ![]() |
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622 | COMET_8P_TUTTLE-P2_18 | 40.6547 | -37.9803 | 40.155519 | -38.192358 | 20.729743 | -50.258243 | 244.9394556 | -64.31314542 | 254.1595 | 54492.2963773148 | 2008-01-27 07:06:47 | 54492.4293287037 | 2008-01-27 10:18:14 | 502063180 | 6.1505 | 6 | 6.1505 | 6.1505 | 0 | 6.1505 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.6133 | 6.6133 | 11.4799 | 0 | PROCESSED | 57541.4227083333 | 2016-06-02 10:08:42 | 54912 | 2009-03-22 00:00:00 | 54546.2369675926 | 2008-03-21 05:41:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502063180/ | Quick Look | ![]() |
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623 | ARC2 | 39.9365 | -39.101 | 39.440937 | -39.3153 | 19.107499 | -50.973986 | 247.81076012 | -64.49485898 | 35.5401 | 54256.3120486111 | 2007-06-05 07:29:21 | 54258.149525463 | 2007-06-07 03:35:19 | 502071010 | 105.7271 | 100 | 105.7351 | 105.7351 | 0 | 105.7271 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.9236 | 82.9236 | 158.7418 | 1 | PROCESSED | 57538.8944097222 | 2016-05-30 21:27:57 | 54702 | 2008-08-24 00:00:00 | 54264.533275463 | 2007-06-13 12:47:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | B | ROBIN SHELTON | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502071010/ | Quick Look | ![]() |
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624 | GC_LARGEPROJECT8 | 265.1842 | -30.7499 | 264.378561 | -30.724571 | 265.818402 | -7.37856 | 357.90048261 | -0.05223369 | 268.8911 | 54727.1991782407 | 2008-09-18 04:46:49 | 54728.3141203704 | 2008-09-19 07:32:20 | 503014010 | 55.3651 | 50 | 55.3651 | 55.3891 | 0 | 55.3651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.2069 | 51.2069 | 96.3118 | 1 | PROCESSED | 57543.8756481482 | 2016-06-04 21:00:56 | 54557 | 2008-04-01 00:00:00 | 54783.7018055556 | 2008-11-13 16:50:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503014010/ | Quick Look | ![]() |
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625 | CYGNUS LOOP (P22) | 312.8353 | 32.4047 | 312.324184 | 32.216345 | 328.267069 | 47.560901 | 75.39493092 | -7.53123997 | 61.4354 | 54620.2981134259 | 2008-06-03 07:09:17 | 54620.7522453704 | 2008-06-03 18:03:14 | 503058010 | 19.2873 | 15 | 19.2873 | 19.2873 | 0 | 19.2873 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.2203 | 17.2203 | 39.212 | 0 | PROCESSED | 57542.7062037037 | 2016-06-03 16:56:56 | 55003 | 2009-06-21 00:00:00 | 54636.2807638889 | 2008-06-19 06:44:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503058010/ | Quick Look | ![]() |
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626 | VELA FRAGMENT E | 119.9016 | -44.3755 | 119.497107 | -44.237549 | 140.837519 | -62.635644 | 259.34445053 | -7.61175769 | 281.1138 | 54582.309224537 | 2008-04-26 07:25:17 | 54583.7849421296 | 2008-04-27 18:50:19 | 503096010 | 79.2004 | 70 | 79.2189 | 79.2004 | 0 | 79.2324 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.2529 | 84.2529 | 127.4899 | 1 | PROCESSED | 57542.4144212963 | 2016-06-03 09:56:46 | 54960 | 2009-05-09 00:00:00 | 54594.2098842593 | 2008-05-08 05:02:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | TERRANCE GAETZ | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503096010/ | Quick Look | ![]() |
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627 | BLOWOUT5 | 312.2204 | 31.3402 | 311.705242 | 31.154062 | 326.94204 | 46.789679 | 74.2273165 | -7.78955911 | 225.5762 | 55176.0660532407 | 2009-12-11 01:35:07 | 55176.7307175926 | 2009-12-11 17:32:14 | 504015010 | 30.4064 | 25 | 30.4064 | 30.4064 | 0 | 30.4064 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.6921 | 28.6921 | 57.4239 | 0 | PROCESSED | 57549.7666898148 | 2016-06-10 18:24:02 | 55555 | 2010-12-25 00:00:00 | 55189.2693981482 | 2009-12-24 06:27:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504015010/ | Quick Look | ![]() |
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628 | NGC 6888 | 303.111 | 38.3992 | 302.65502 | 38.248061 | 320.307714 | 56.205556 | 75.54872423 | 2.39562358 | 36.3096 | 54999.0718981482 | 2009-06-17 01:43:32 | 55001.1793287037 | 2009-06-19 04:18:14 | 504084010 | 88.8468 | 75 | 88.8548 | 88.8468 | 0 | 88.8548 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.4052 | 82.4052 | 182.0679 | 2 | PROCESSED | 57547.6754976852 | 2016-06-08 16:12:43 | 55378 | 2010-07-01 00:00:00 | 55012.4221180556 | 2009-06-30 10:07:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041321 | Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. | GALACTIC DIFFUSE EMISSION | 5 | A | SVETOZAR ZHEKOV | USA | 4 | AO4 | X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504084010/ | Quick Look | ![]() |
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629 | CYGNUS LOOP 9 | 312.876 | 30.2229 | 312.354142 | 30.034417 | 327.064975 | 45.541284 | 73.70000859 | -8.9268412 | 80.5836 | 55307.2796064815 | 2010-04-21 06:42:38 | 55308.0106597222 | 2010-04-22 00:15:21 | 505017010 | 29.9968 | 29 | 29.9968 | 29.9968 | 0 | 29.9968 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.6281 | 27.6281 | 63.1499 | 1 | PROCESSED | 57551.2933217593 | 2016-06-12 07:02:23 | 55287 | 2010-04-01 00:00:00 | 55364.2675347222 | 2010-06-17 06:25:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505017010/ | Quick Look | ![]() |
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630 | SNR G304.6+0.1 | 196.4463 | -62.6951 | 195.657347 | -62.427468 | 227.041423 | -49.777353 | 304.57643925 | 0.13082789 | 321.0575 | 55442.9126736111 | 2010-09-03 21:54:15 | 55445.5356828704 | 2010-09-06 12:51:23 | 505074010 | 99.5817 | 100 | 99.6217 | 99.5817 | 0 | 99.6297 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.5653 | 90.5653 | 226.5319 | 1 | PROCESSED | 57553.3505555556 | 2016-06-14 08:24:48 | 55827 | 2011-09-23 00:00:00 | 55461.4231712963 | 2010-09-22 10:09:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051306 | Galactic supernova remnants are believed to be the primary source of cosmic rays below 10^15.5 eV even though the exact acceleration mechanism remains unknown. This uncertainty results from the lack of remnants with synchrotron X-ray and GeV emission, needed to distinguish accelerated electrons from protons using broadband spectral modeling. An analysis of recent XMM and Fermi data suggests SNR G304.6+0.1 is just the third remnant with both, but the observed hard X-ray excess is also consistent with bremsstrahlung emission. We request a deep Suzaku observation of this source to determine the nature of its hard X-ray emission - critical for identifying the underlying acceleration mechanism. | GALACTIC DIFFUSE EMISSION | 5 | B | JOSEPH GELFAND | USA | 5 | AO5 | THE ORIGIN OF THE HARD X-RAY AND GEV GAMMA-RAY EMISSION OF SNR G304.6+0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505074010/ | Quick Look | ![]() |
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631 | GALACTIC_BULGE6 | 271.3758 | -31.4828 | 270.564538 | -31.487512 | 271.175264 | -8.047458 | 359.95693453 | -4.99276165 | 88.0304 | 55639.361087963 | 2011-03-19 08:39:58 | 55640.3565162037 | 2011-03-20 08:33:23 | 505081010 | 50.1669 | 50 | 50.1714 | 50.1669 | 0 | 50.1795 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43.6357 | 43.6357 | 85.9898 | 0 | PROCESSED | 57601.2415277778 | 2016-08-01 05:47:48 | 55287 | 2010-04-01 00:00:00 | 55649.2186574074 | 2011-03-29 05:14:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505081010/ | Quick Look | ![]() |
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632 | GALACTIC_BULGE14 | 264.9946 | -32.433 | 264.177795 | -32.406725 | 265.713815 | -9.066176 | 356.38820164 | -0.80858885 | 270.5244 | 55479.5865509259 | 2010-10-10 14:04:38 | 55480.8980671296 | 2010-10-11 21:33:13 | 505083010 | 52.9383 | 50 | 52.9383 | 52.9383 | 0 | 52.9383 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.4073 | 42.4073 | 113.3039 | 1 | PROCESSED | 57553.7064236111 | 2016-06-14 16:57:15 | 55287 | 2010-04-01 00:00:00 | 55491.0402893518 | 2010-10-22 00:58:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505083010/ | Quick Look | ![]() |
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633 | THE KEPLER SNR | 262.6745 | -21.5044 | 261.925136 | -21.467093 | 263.174286 | 1.76325 | 4.50818409 | 6.8092486 | 272.4561 | 55469.9826736111 | 2010-09-30 23:35:03 | 55470.368287037 | 2010-10-01 08:50:20 | 505092010 | 17.7141 | 620 | 17.7221 | 17.7301 | 0 | 17.7141 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.8694 | 17.8694 | 33.3079 | 0 | PROCESSED | 57553.595 | 2016-06-14 14:16:48 | 55287 | 2010-04-01 00:00:00 | 55482.4747453704 | 2010-10-13 11:23:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092010/ | Quick Look | ![]() |
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634 | 3C 59 VICINITY 1 | 32.0992 | 30.0806 | 31.374147 | 29.84386 | 40.280714 | 16.078754 | 142.1363254 | -29.90513458 | 254.1341 | 55940.8410763889 | 2012-01-14 20:11:09 | 55942.215474537 | 2012-01-16 05:10:17 | 506024010 | 55.8581 | 50 | 55.8581 | 55.8581 | 0 | 55.8581 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.0404 | 46.0404 | 118.7379 | 1 | PROCESSED | 57604.3853356482 | 2016-08-04 09:14:53 | 56331 | 2013-02-08 00:00:00 | 55960.1998032407 | 2012-02-03 04:47:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060067 | We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed. | GALACTIC DIFFUSE EMISSION | 5 | C | KAZUHIRO SAKAI | JAP | 6 | AO6 | STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506024010/ | Quick Look | ![]() |
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635 | G18.8+0.3 | 275.9435 | -12.3781 | 275.241856 | -12.405238 | 275.902948 | 10.940788 | 18.78460262 | 0.39706413 | 83.4994 | 55994.9180324074 | 2012-03-08 22:01:58 | 55996.1598958333 | 2012-03-10 03:50:15 | 506051010 | 52.0205 | 50 | 52.0205 | 52.0285 | 0 | 52.0365 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.882 | 44.882 | 107.2639 | 1 | PROCESSED | 57604.8541435185 | 2016-08-04 20:29:58 | 56382 | 2013-03-31 00:00:00 | 56016.6717708333 | 2012-03-30 16:07:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061311 | We propose a 50 ks exploratory observation of an interesting first-quadrant supernova remnant, G18.8+0.3, for which radio-continuum and CO data indicate interaction with a molecular cloud. Prior X-ray studies are limited to a 14 ks ROSAT PSPC observation producing about 500 counts. We expect about 12,000 counts with Suzaku, which should permit basic characterization of the spectrum and morphology of X-rays: shell-type, mixed-morphology (central thermal emission) or even composite (central PWN). Spectral analysis will allow us to determine or estimate shock speed, age, ambient density, and swept-up mass. As more middle-aged remnants are found to have unusual properties such as GeV-TeV emission, the study of objects like G18.8+0.3 assumes greater importance. | GALACTIC DIFFUSE EMISSION | 5 | C | STEPHEN REYNOLDS | USA | 6 | AO6 | G18.8+0.3: A SUPERNOVA REMNANT WITH STRONG MOLECULAR INTERACTION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506051010/ | Quick Look | ![]() |
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636 | G272.2-3.2 | 136.7114 | -52.1231 | 136.316281 | -51.921066 | 170.818449 | -63.077248 | 272.22308022 | -3.18374401 | 297.1287 | 55709.5476041667 | 2011-05-28 13:08:33 | 55711.9009490741 | 2011-05-30 21:37:22 | 506060010 | 130.0782 | 150 | 130.0862 | 130.0942 | 0 | 130.0782 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 121.8303 | 121.8303 | 203.3058 | 3 | PROCESSED | 57602.216087963 | 2016-08-02 05:11:10 | 55652 | 2011-04-01 00:00:00 | 55735.3493171296 | 2011-06-23 08:23:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060010/ | Quick Look | ![]() |
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637 | HESSJ1507-622_CENTER | 226.7316 | -62.3464 | 225.708755 | -62.153708 | 244.337801 | -42.703137 | 317.95199358 | -3.49348671 | 301.8082 | 56181.4881712963 | 2012-09-11 11:42:58 | 56183.9549189815 | 2012-09-13 22:55:05 | 507025010 | 79.8869 | 80 | 79.8949 | 79.9029 | 0 | 79.8869 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.1958 | 74.1958 | 213.1037 | 1 | PROCESSED | 57607.0557986111 | 2016-08-07 01:20:21 | 56582 | 2013-10-17 00:00:00 | 56212.7347337963 | 2012-10-12 17:38:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070033 | HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator. | GALACTIC DIFFUSE EMISSION | 5 | B | YUKIKATSU TERADA | HIRONORI MATSUMOTO | JAP | 7 | AO7 | SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507025010/ | Quick Look | ![]() |
638 | CAS A | 350.8607 | 58.8031 | 350.294827 | 58.528522 | 27.373119 | 54.842451 | 111.73599633 | -2.14263527 | 251.3043 | 56281.1375115741 | 2012-12-20 03:18:01 | 56283.3466666667 | 2012-12-22 08:19:12 | 507038010 | 102.411 | 100 | 102.419 | 102.411 | 0 | 102.426 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 126.7103 | 126.7103 | 190.8458 | 0 | PROCESSED | 57608.4566435185 | 2016-08-08 10:57:34 | 56683 | 2014-01-26 00:00:00 | 56316.9831365741 | 2013-01-24 23:35:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070050 | We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | C | YOSHITOMO MAEDA | JAP | 7 | AO7 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507038010/ | Quick Look | ![]() |
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639 | GRXE_E_5 | 268.0495 | -26.6011 | 267.269457 | -26.589728 | 268.243808 | -3.171982 | 2.75089625 | -0.04390767 | 105.4995 | 56373.3059722222 | 2013-03-22 07:20:36 | 56375.3646990741 | 2013-03-24 08:45:10 | 507072010 | 101.2435 | 100 | 101.2435 | 101.2435 | 0 | 101.2435 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.6676 | 102.6676 | 177.8658 | 1 | PROCESSED | 57610.9241087963 | 2016-08-10 22:10:43 | 56018 | 2012-04-01 00:00:00 | 56384.595787037 | 2013-04-02 14:17:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507072010/ | Quick Look | ![]() |
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640 | W28_SOUTH | 270.2522 | -23.558 | 269.490042 | -23.557374 | 270.221597 | -0.117322 | 6.38418356 | -0.23955939 | 89.9033 | 56738.9940393518 | 2014-03-22 23:51:25 | 56740.1793518518 | 2014-03-24 04:18:16 | 508006010 | 40.8518 | 100 | 40.8838 | 40.8518 | 0 | 40.8942 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 35.4568 | 35.4568 | 102.4078 | 1 | PROCESSED | 57614.1110648148 | 2016-08-14 02:39:56 | 57359 | 2015-12-03 00:00:00 | 56754.6877083333 | 2014-04-07 16:30:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080017 | A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP. | GALACTIC DIFFUSE EMISSION | 5 | A | MAKOTO SAWADA | JAP | 8 | AO8 | INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508006010/ | Quick Look | ![]() |
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641 | CYG_COCOON2 | 306.1992 | 40.9463 | 305.753337 | 40.782769 | 326.198572 | 57.540222 | 78.99355785 | 1.86268914 | 253.1744 | 56603.8842939815 | 2013-11-07 21:13:23 | 56605.000162037 | 2013-11-09 00:00:14 | 508020010 | 46.4489 | 50 | 46.4489 | 46.4489 | 0 | 46.4489 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.6569 | 44.6569 | 96.3739 | 3 | PROCESSED | 57613.2763194444 | 2016-08-13 06:37:54 | 57018 | 2014-12-27 00:00:00 | 56652.6462152778 | 2013-12-26 15:30:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080048 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density and spatial distribution in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | TSUNEFUMI MIZUNO | JAP | 8 | AO8 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508020010/ | Quick Look | ![]() |
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642 | VELA PWN W4 | 126.476 | -45.2086 | 126.060911 | -45.04388 | 150.453491 | -61.215385 | 262.5995548 | -4.15230559 | 95.0003 | 56591.4348726852 | 2013-10-26 10:26:13 | 56591.8813888889 | 2013-10-26 21:09:12 | 508045010 | 16.8588 | 15 | 16.8843 | 16.8588 | 0 | 16.8748 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.0055 | 16.0055 | 38.578 | 0 | PROCESSED | 57613.1152893518 | 2016-08-13 02:46:01 | 57009 | 2014-12-18 00:00:00 | 56643.6542708333 | 2013-12-17 15:42:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | KOJI MORI | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508045010/ | Quick Look | ![]() |
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643 | VELA PWN GEV6 | 128.0698 | -45.8067 | 127.654656 | -45.635799 | 153.081718 | -61.174639 | 263.73946045 | -3.59392918 | 121.6832 | 56987.9020717593 | 2014-11-26 21:38:59 | 56988.5530324074 | 2014-11-27 13:16:22 | 509016010 | 18.0926 | 15 | 18.1086 | 18.0926 | 0 | 18.1086 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8287037037 | 2016-08-16 19:53:20 | 57450 | 2016-03-03 00:00:00 | 57083.4111574074 | 2015-03-02 09:52:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509016010/ | Quick Look | ![]() |
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644 | L106_B3 | 337.3111 | 61.2453 | 336.866796 | 60.988922 | 21.907924 | 61.425064 | 106.66847152 | 2.94694679 | 86.3781 | 55332.0617013889 | 2010-05-16 01:28:51 | 55333.5078587963 | 2010-05-17 12:11:19 | 505054010 | 59.3804 | 60 | 59.3804 | 59.3804 | 0 | 59.3804 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 54.0551 | 54.0551 | 124.908 | 3 | PROCESSED | 57551.5609259259 | 2016-06-12 13:27:44 | 55765 | 2011-07-23 00:00:00 | 55393.2646759259 | 2010-07-16 06:21:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050086 | We propose observarions of two fields on and near midplane (b = 0 and 3 deg.) in order to study bump-like emission peaked at 0.9 keV observed in midplane. The two fields proposed for observations has been observed by Chandra. By comparing the spectra taken by Suzaku and Chandra, we will determine the contribution of point sources (stars), and investigate posisble contribution of diffuse thermal plasma. | GALACTIC DIFFUSE EMISSION | 5 | B | YOH TAKEI | JAP | 5 | AO5 | ORIGIN OF SOFT X-RAY EMISSION IN THE MILKY-WAY DISK | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505054010/ | Quick Look | ![]() |
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645 | VICINITY_4U1957+11 | 300.5977 | 12.1307 | 300.008296 | 11.990222 | 305.849194 | 31.842544 | 52.0534723 | -9.74567764 | 252.1551 | 55499.6275578704 | 2010-10-30 15:03:41 | 55501.8265625 | 2010-11-01 19:50:15 | 505057010 | 80.5839 | 80 | 80.5839 | 80.5839 | 0 | 80.5839 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.2042 | 59.2042 | 189.9759 | 2 | PROCESSED | 57553.9949305556 | 2016-06-14 23:52:42 | 55882 | 2011-11-17 00:00:00 | 55515.3752083333 | 2010-11-15 09:00:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050090 | We propose for an observation of the vicinity of 4U 1957+11, in order to study the Galactic low-latitude hot gas. Recently, detection of OVII and NeIX aborption lines was reported in the spectrum of 4U 1957+11 (Yao et al. 2008). By combining a Suzaku observation of diffuse hot plasma around the object with the reported absorption line equivalnet widths, we will constrain the temperature, line-of-sight length, density of the hot plasma of the direction. Not only to understand the Galactic gas, but also to understand feedback mechanism from a galaxy to the intergalactic space will our study play an important role. | GALACTIC DIFFUSE EMISSION | 5 | B | YOH TAKEI | JAP | 5 | AO5 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC LOW-LATITUDE HOT GAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505057010/ | Quick Look | ![]() |
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646 | RCW86 SW | 220.2761 | -62.6782 | 219.292066 | -62.464185 | 240.754321 | -44.190898 | 315.14426109 | -2.43598628 | 109.6929 | 53778.0961689815 | 2006-02-12 02:18:29 | 53780.2814699074 | 2006-02-14 06:45:19 | 500004010 | 100.7659 | 100 | 100.7819 | 100.7659 | 100.7819 | 100.7819 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90.6819 | 90.6819 | 188.7918 | 2 | PROCESSED | 57533.035787037 | 2016-05-25 00:51:32 | 54247 | 2007-05-27 00:00:00 | 54041.2835648148 | 2006-11-02 06:48:20 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001019 | The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 0 | SWG | THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500004010/ | Quick Look | ![]() |
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647 | 73P/SW3 | 279.2884 | 33.5067 | 278.829487 | 33.462856 | 284.096243 | 56.493773 | 62.26395264 | 17.33399104 | 47.3721 | 53862.3946875 | 2006-05-07 09:28:21 | 53862.4794444444 | 2006-05-07 11:30:24 | 500012010 | 3.25 | 5 | 3.25 | 3.25 | 3.25 | 3.25 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.3139 | 2.3139 | 7.304 | 0 | PROCESSED | 57533.6418402778 | 2016-05-25 15:24:15 | 54256 | 2007-06-05 00:00:00 | 54042.1755671296 | 2006-11-03 04:12:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500012010/ | Quick Look | ![]() |
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648 | JUPITER | 29.0829 | 10.6504 | 28.417372 | 10.406323 | 30.788902 | -1.172897 | 147.71201597 | -49.07381266 | 249.1851 | 55939.2483912037 | 2012-01-13 05:57:41 | 55939.8634722222 | 2012-01-13 20:43:24 | 506006050 | 23.2827 | 160 | 23.2907 | 23.2827 | 0 | 23.2954 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2679 | 19.2679 | 53.136 | 0 | PROCESSED | 57604.3330902778 | 2016-08-04 07:59:39 | 56331 | 2013-02-08 00:00:00 | 55960.1390740741 | 2012-02-03 03:20:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006050/ | Quick Look | ![]() |
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649 | WESTERLUND1_2 | 252.808 | -46.1402 | 251.891543 | -46.055758 | 257.089266 | -23.465452 | 339.79276992 | -1.14410237 | 285.6981 | 55451.2033912037 | 2010-09-12 04:52:53 | 55452.6077777778 | 2010-09-13 14:35:12 | 505050010 | 52.6541 | 50 | 52.6541 | 52.6541 | 0 | 52.6541 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7536 | 42.7536 | 121.3099 | 0 | PROCESSED | 57553.3934375 | 2016-06-14 09:26:33 | 55829 | 2011-09-25 00:00:00 | 55463.2091435185 | 2010-09-24 05:01:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505050010/ | Quick Look | ![]() |
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650 | SNR G106.3+2.7 P2 | 336.9121 | 60.9439 | 336.468568 | 60.688281 | 21.166616 | 61.378787 | 106.34649405 | 2.79001657 | 12.2687 | 55423.4230787037 | 2010-08-15 10:09:14 | 55424.0209837963 | 2010-08-16 00:30:13 | 505072010 | 24.5562 | 50 | 24.5722 | 24.5562 | 0 | 24.5722 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.6147 | 26.6147 | 51.6559 | 1 | PROCESSED | 57553.084212963 | 2016-06-14 02:01:16 | 55807 | 2011-09-03 00:00:00 | 55441.2685069444 | 2010-09-02 06:26:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051305 | After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. | GALACTIC DIFFUSE EMISSION | 5 | C | ESTER ALIU | USA | 5 | AO5 | ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505072010/ | Quick Look | ![]() |
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651 | CARINA SW | 160.2531 | -60.104 | 159.777159 | -59.842292 | 202.080754 | -59.579426 | 287.34811018 | -1.23919183 | 109.6766 | 55542.7308333333 | 2010-12-12 17:32:24 | 55543.4438888889 | 2010-12-13 10:39:12 | 505075010 | 47.0039 | 45 | 47.0039 | 47.0119 | 0 | 47.0119 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.4341 | 42.4341 | 61.5999 | 0 | PROCESSED | 57554.3916435185 | 2016-06-15 09:23:58 | 55960 | 2012-02-03 00:00:00 | 55592.9230324074 | 2011-01-31 22:09:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051312 | X-ray nebulae with kT =0.1-0.8 keV, log Lx up to 35 ergs/s, and size of 1-1000 pc accompany a number of giant HII region. The Carinae Nebula is the best region to study their origin with 10-100 times more luminous soft X-rays than any other giant HII regions in our Galaxy. X-ray observations especially with Suzaku revealed that a part, or all, of the diffuse plasma would heat up by earlier supernova explosions, but it is unknown when these explosions occurred and how they made the current X-ray nebula. The Chandra Carina Complex Project displayed that the southern part of the nebula emits strong hydrogen-like oxygen line. We will measure helium-like oxygen line with Suzaku to measure its plasma temperature and abundance to help understand relation with plasma in the nebula center. | GALACTIC DIFFUSE EMISSION | 5 | C | KENJI HAMAGUCHI | USA | 5 | AO5 | SOUTHERN PART OF DIFFUSE PLASMA IN THE CARINA NEBULA - RICH IN OXYGEN? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505075010/ | Quick Look | ![]() |
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652 | CYGNUS LOOP BLOWOUT5 | 312.5999 | 28.7931 | 312.071808 | 28.605616 | 325.981178 | 44.311018 | 72.41540255 | -9.63024021 | 60.972 | 55708.6627546296 | 2011-05-27 15:54:22 | 55709.5335185185 | 2011-05-28 12:48:16 | 506015010 | 36.7552 | 35 | 36.7632 | 36.7552 | 0 | 36.7695 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 31.6317 | 31.6317 | 75.216 | 1 | PROCESSED | 57602.1728935185 | 2016-08-02 04:08:58 | 56093 | 2012-06-15 00:00:00 | 55725.2447569444 | 2011-06-13 05:52:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506015010/ | Quick Look | ![]() |
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653 | THE KEPLER SNR | 262.6706 | -21.4823 | 261.92136 | -21.444974 | 263.169538 | 1.785137 | 4.52493262 | 6.82424916 | 102.5027 | 55615.8474421296 | 2011-02-23 20:20:19 | 55616.8174768518 | 2011-02-24 19:37:10 | 505092030 | 34.2015 | 150 | 34.2095 | 34.2015 | 0 | 34.2095 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.1199 | 29.1199 | 83.7958 | 0 | PROCESSED | 57601.0436342593 | 2016-08-01 01:02:50 | 55287 | 2010-04-01 00:00:00 | 55628.1747569444 | 2011-03-08 04:11:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092030/ | Quick Look | ![]() |
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654 | VELA JR SE2 | 133.8563 | -47.0644 | 133.431556 | -46.872219 | 161.338969 | -60.118086 | 267.19687484 | -1.23927515 | 109.9991 | 56620.734375 | 2013-11-24 17:37:30 | 56621.062650463 | 2013-11-25 01:30:13 | 508061010 | 14.4492 | 15 | 14.4492 | 14.4711 | 0 | 14.4572 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.7997 | 18.7997 | 28.3599 | 0 | PROCESSED | 57613.398912037 | 2016-08-13 09:34:26 | 56998 | 2014-12-07 00:00:00 | 56632.5722685185 | 2013-12-06 13:44:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | TARO FUKUYAMA | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508061010/ | Quick Look | ![]() |
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655 | VELA PWN E4 | 130.4202 | -45.4045 | 129.99462 | -45.224746 | 155.536956 | -59.986634 | 264.40968594 | -2.03918199 | 304.5026 | 55712.4105902778 | 2011-05-31 09:51:15 | 55712.7362268518 | 2011-05-31 17:40:10 | 506047010 | 17.0314 | 15 | 17.0354 | 17.0549 | 0 | 17.0314 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.1078 | 15.1078 | 28.128 | 0 | PROCESSED | 57602.173900463 | 2016-08-02 04:10:25 | 56093 | 2012-06-15 00:00:00 | 55726.0290046296 | 2011-06-14 00:41:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506047010/ | Quick Look | ![]() |
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656 | VELAFRAGG TAIL | 125.0448 | -47.7009 | 124.65466 | -47.541789 | 151.337516 | -63.864294 | 264.09848727 | -6.37839252 | 263.1844 | 55658.0366898148 | 2011-04-07 00:52:50 | 55658.8565162037 | 2011-04-07 20:33:23 | 506057010 | 49.3543 | 50 | 49.3703 | 49.3543 | 0 | 49.3703 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9581 | 43.9581 | 70.8259 | 1 | PROCESSED | 57601.4287268518 | 2016-08-01 10:17:22 | 56043 | 2012-04-26 00:00:00 | 55673.1976736111 | 2011-04-22 04:44:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062021 | The Vela supernova remnant (SNR) displays remarkable features which appear to be ejecta ``shrapnel'' visible beyond the main shell. One of these shrapnel (A) is distinct from the others in that its X-ray spectrum exhibits a high Si abundance, while the other shrapnel exhibit enhanced O, Ne, and Mg abundances. One unexplored ejecta shrapnel (G) is located on the opposite side of the remnant from shrapnel A, suggesting that the SN explosion may have resulted in a jet-counterjet Si-rich structure, reminiscent of Cas A. We propose to observe this shrapnel for the first time to determine if it is also Si-rich like shrapnel A. If this is the case, the Vela SNR may be the first direct evidence of a jet-induced SN explosion. | GALACTIC DIFFUSE EMISSION | 5 | A | FABRIZIO BOCCHINO | EUR | 6 | AO6 | ASYMMETRIC SN EXPLOSION IN VELA SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506057010/ | Quick Look | ![]() |
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657 | CAS A | 350.8704 | 58.8069 | 350.304462 | 58.532314 | 27.384002 | 54.841803 | 111.74200441 | -2.14072863 | 228.5251 | 56672.9492708333 | 2014-01-15 22:46:57 | 56673.8064699074 | 2014-01-16 19:21:19 | 508011010 | 0 | 120 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.771412037 | 2016-08-13 18:30:50 | 56717 | 2014-03-01 00:00:00 | 56712.601400463 | 2014-02-24 14:26:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080021 | We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHITOMO MAEDA | JAP | 8 | AO8 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508011010/ | Quick Look | ![]() |
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658 | W44_SOUTH | 284.0546 | 1.2208 | 283.419443 | 1.15468 | 285.391807 | 23.913502 | 34.56340933 | -0.50670684 | 73.0006 | 56756.507025463 | 2014-04-09 12:10:07 | 56757.3474074074 | 2014-04-10 08:20:16 | 508003020 | 32.3696 | 33 | 32.3776 | 32.3776 | 0 | 32.3696 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5034 | 29.5034 | 72.5959 | 1 | PROCESSED | 57614.2259837963 | 2016-08-14 05:25:25 | 57193 | 2015-06-20 00:00:00 | 56825.6834027778 | 2014-06-17 16:24:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508003020/ | Quick Look | ![]() |
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659 | N63A | 83.9019 | -66.0368 | 83.884731 | -66.066447 | 9.218584 | -87.500527 | 275.90835505 | -32.28360929 | 166.1398 | 56628.8025347222 | 2013-12-02 19:15:39 | 56629.9556828704 | 2013-12-03 22:56:11 | 508071010 | 82.0387 | 80 | 82.0467 | 82.0387 | 0 | 82.0467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.8129 | 70.8129 | 99.6119 | 3 | PROCESSED | 57613.5008680556 | 2016-08-13 12:01:15 | 56383 | 2013-04-01 00:00:00 | 56639.6281365741 | 2013-12-13 15:04:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508071010/ | Quick Look | ![]() |
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660 | MBM16 | 49.7645 | 11.5821 | 49.080902 | 11.401011 | 50.440387 | -6.505796 | 170.59989958 | -37.2737153 | 77.5997 | 56511.9409027778 | 2013-08-07 22:34:54 | 56513.916875 | 2013-08-09 22:00:18 | 508078010 | 82.3246 | 80 | 82.3246 | 82.3246 | 0 | 82.3246 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.0718 | 79.0718 | 170.6898 | 2 | PROCESSED | 57612.2763541667 | 2016-08-12 06:37:57 | 56383 | 2013-04-01 00:00:00 | 56587.6759490741 | 2013-10-22 16:13:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508078010/ | Quick Look | ![]() |
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661 | MBM36 | 238.3853 | -4.8926 | 237.724645 | -4.745297 | 237.254427 | 15.02643 | 3.92555744 | 35.61619893 | 279.5456 | 56531.6987268518 | 2013-08-27 16:46:10 | 56533.8883333333 | 2013-08-29 21:19:12 | 508079020 | 79.6067 | 80 | 79.6067 | 79.6067 | 0 | 79.6067 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.717 | 67.717 | 189.166 | 2 | PROCESSED | 57612.4621064815 | 2016-08-12 11:05:26 | 56383 | 2013-04-01 00:00:00 | 56603.7246875 | 2013-11-07 17:23:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079020/ | Quick Look | ![]() |
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662 | G93.3+6.9 SOUTH | 313.0658 | 55.1877 | 312.717301 | 54.998248 | 351.809721 | 66.81178 | 93.13746865 | 6.81993623 | 52.2984 | 56817.2417708333 | 2014-06-09 05:48:09 | 56819.1057638889 | 2014-06-11 02:32:18 | 509041010 | 85.4695 | 80 | 85.7132 | 85.4695 | 0 | 85.7131 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2181712963 | 2016-08-15 05:14:10 | 57201 | 2015-06-28 00:00:00 | 56835.7539236111 | 2014-06-27 18:05:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | MICHAEL STAGE | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509041010/ | Quick Look | ![]() |
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663 | FERMI_JET_COCOON_1 | 324.2719 | -34.1434 | 323.519422 | -34.36838 | 315.213492 | -18.826861 | 11.0027102 | -48.00136957 | 252.0162 | 56980.9718402778 | 2014-11-19 23:19:27 | 56981.4029166667 | 2014-11-20 09:40:12 | 509047010 | 23.1647 | 20 | 23.1647 | 23.1887 | 0 | 23.1727 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.793125 | 2016-08-16 19:02:06 | 57444 | 2016-02-26 00:00:00 | 57076.4062037037 | 2015-02-23 09:44:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MATTHEW MILLER | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509047010/ | Quick Look | ![]() |
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664 | DIFFUSE1CENTER | 201.5497 | 7.7363 | 200.922947 | 7.99578 | 196.916148 | 15.561038 | 327.54309857 | 68.93048937 | 123.2999 | 57014.2523842593 | 2014-12-23 06:03:26 | 57014.7820949074 | 2014-12-23 18:46:13 | 509058010 | 20.5308 | 20 | 20.5308 | 20.5308 | 0 | 20.5308 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5530555556 | 2016-08-17 13:16:24 | 57475 | 2016-03-28 00:00:00 | 57107.4252546296 | 2015-03-26 10:12:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509058010/ | Quick Look | ![]() |
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665 | 3C400.2 NW | 294.5044 | 17.3912 | 293.942879 | 17.276968 | 300.273195 | 38.29194 | 53.66788209 | -2.01364052 | 81.5888 | 56770.4644907407 | 2014-04-23 11:08:52 | 56770.9410763889 | 2014-04-23 22:35:09 | 509068010 | 21.47 | 20 | 21.4853 | 21.486 | 0 | 21.47 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.9678 | 20.9678 | 41.1719 | 0 | PROCESSED | 57614.9785416667 | 2016-08-14 23:29:06 | 57152 | 2015-05-10 00:00:00 | 56789.6036805556 | 2014-05-12 14:29:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | JACCO VINK | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509068010/ | Quick Look | ![]() |
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666 | G306.3-0.9 | 200.4753 | -63.5602 | 199.643661 | -63.298602 | 230.10249 | -49.420915 | 306.31531317 | -0.88874973 | 306.5675 | 56889.7845833333 | 2014-08-20 18:49:48 | 56894.0099768518 | 2014-08-25 00:14:22 | 509072010 | 190.0114 | 200 | 190.0181 | 190.0114 | 0 | 190.0114 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.4515 | 14.4515 | 20.22 | 0 | PROCESSED | 57616.5396759259 | 2016-08-16 12:57:08 | 57305 | 2015-10-10 00:00:00 | 56938.2302777778 | 2014-10-08 05:31:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 093109 | The origin of the distorted, inhomogeneous structure of mixed-morphology SNRs (MM SNRs) is a mystery. Recently we have discovered recombining plasma from MM SNRs. The existence of recombining plasma implies rapid cooling process in past. Recombining plasma, together with the peculiar morphologies, would indicate a new SNR evolution scenario. Our systematic analysis of recombining SNRs shows that the recombination ages are almost the same, although their dynamical ages range over an order of magnitude. Such a trend can be explained by past rapid rarefaction. This hypothesis can be tested by measuring a recombination age of a dynamically young recombining SNR. We thus propose a 100-ks Suzaku observation of G306.3-0.9, a candidate of the youngest recombining SNR ever. | GALACTIC DIFFUSE EMISSION | 5 | A | MAKOTO SAWADA | Reynolds,Matsumura | JUS | 9 | AO9 | THE DYNAMICS OF MIXED-MORPHOLOGY SNRS PROBED BY THE YOUNGEST RECOMBINING PLASMA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509072010/ | Quick Look | ![]() |
667 | SN1006_BGD3 | 226.4731 | -42.5186 | 225.649158 | -42.32537 | 236.222692 | -24.044133 | 327.77356316 | 13.77561257 | 286.5156 | 56888.6466550926 | 2014-08-19 15:31:11 | 56889.2084606482 | 2014-08-20 05:00:11 | 509085010 | 31.65 | 30 | 31.65 | 31.65 | 0 | 31.65 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5050115741 | 2016-08-16 12:07:13 | 56748 | 2014-04-01 00:00:00 | 56910.6423611111 | 2014-09-10 15:25:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYA YAMAGUCHI | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509085010/ | Quick Look | ![]() |
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668 | 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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669 | SN 1987A | 83.8361 | -69.2786 | 83.928024 | -69.308301 | 307.518784 | -86.433209 | 279.71542477 | -31.94667609 | 132.5904 | 53677.835775463 | 2005-11-03 20:03:31 | 53678.3475 | 2005-11-04 08:20:24 | 500006010 | 36.7863 | 40 | 36.7863 | 36.7863 | 36.7863 | 36.7863 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.9198 | 32.9198 | 44.1661 | 1 | PROCESSED | 57527.9193518518 | 2016-05-19 22:03:52 | 54247 | 2007-05-27 00:00:00 | 54037.1281481482 | 2006-10-29 03:04:32 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001028 | SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies. | GALACTIC DIFFUSE EMISSION | 5 | A | GUENTHER HASINGER | JAP | 0 | SWG | SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500006010/ | Quick Look | ![]() |
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670 | GALACTIC RIDGE | 281.0049 | -4.0776 | 280.344509 | -4.129178 | 281.602156 | 18.920781 | 28.45801897 | -0.21166151 | 265.5297 | 53671.1112037037 | 2005-10-28 02:40:08 | 53673.8960069445 | 2005-10-30 21:30:15 | 500009010 | 93.3276 | 100 | 93.3436 | 93.3596 | 93.3436 | 93.3276 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 77.5364 | 77.5364 | 240.5759 | 0 | PROCESSED | 57527.7330439815 | 2016-05-19 17:35:35 | 54247 | 2007-05-27 00:00:00 | 54037.6929513889 | 2006-10-29 16:37:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | KEN EBISAWA | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009010/ | Quick Look | ![]() |
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671 | 73P/SW3 | 318.3252 | 23.9905 | 317.766876 | 23.78347 | 329.890581 | 37.931404 | 71.97868305 | -16.64134569 | 72.7093 | 53868.4091666667 | 2006-05-13 09:49:12 | 53868.4752199074 | 2006-05-13 11:24:19 | 500013050 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.584 | 2.584 | 5.7039 | 0 | PROCESSED | 57534.2992476852 | 2016-05-26 07:10:55 | 54256 | 2007-06-05 00:00:00 | 54089.4348611111 | 2006-12-20 10:26:12 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013050/ | Quick Look | ![]() |
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672 | 73P/SW3 | 318.7382 | 23.8104 | 318.178519 | 23.602036 | 330.247137 | 37.622205 | 72.09504522 | -17.04458663 | 72.7096 | 53868.4758333333 | 2006-05-13 11:25:12 | 53868.5418865741 | 2006-05-13 13:00:19 | 500013060 | 3.218 | 20 | 3.218 | 3.218 | 3.218 | 3.218 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.539 | 2.539 | 5.6959 | 0 | PROCESSED | 57534.3046759259 | 2016-05-26 07:18:44 | 54256 | 2007-06-05 00:00:00 | 54042.3000462963 | 2006-11-03 07:12:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013060/ | Quick Look | ![]() |
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673 | 73P/SW3 | 319.575 | 23.4516 | 319.012619 | 23.240566 | 330.968775 | 37.00001 | 72.3420597 | -17.8575616 | 72.7092 | 53868.609212963 | 2006-05-13 14:37:16 | 53868.6738310185 | 2006-05-13 16:10:19 | 500013080 | 3.1644 | 20 | 3.1644 | 3.1644 | 3.1644 | 3.1644 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.986 | 2.986 | 5.5519 | 0 | PROCESSED | 57534.3120601852 | 2016-05-26 07:29:22 | 54256 | 2007-06-05 00:00:00 | 54042.3213657407 | 2006-11-03 07:42:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013080/ | Quick Look | ![]() |
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674 | 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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675 | 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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676 | 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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677 | 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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678 | COMET_8P_TUTTLE-P1-2 | 27.9946 | 7.7582 | 27.33663 | 7.511628 | 28.768937 | -3.5069 | 147.87340904 | -52.1573456 | 248.4994 | 54470.5826041667 | 2008-01-05 13:58:57 | 54470.6488310185 | 2008-01-05 15:34:19 | 502062020 | 2.2193 | 2 | 2.2193 | 2.2193 | 0 | 2.2193 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2.164 | 2.164 | 5.718 | 0 | PROCESSED | 57540.985162037 | 2016-06-01 23:38:38 | 54908 | 2009-03-18 00:00:00 | 54542.2129166667 | 2008-03-17 05:06:36 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062020/ | Quick Look | ![]() |
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679 | COMET_8P_TUTTLE-P1-4 | 28.0997 | 7.2516 | 27.442835 | 7.005266 | 28.688048 | -4.017818 | 148.34803657 | -52.5857522 | 248.4989 | 54470.7159143518 | 2008-01-05 17:10:55 | 54470.7821527778 | 2008-01-05 18:46:18 | 502062040 | 1.7233 | 2 | 1.7233 | 1.7233 | 0 | 1.7233 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1.4567 | 1.4567 | 5.722 | 0 | PROCESSED | 57540.9953125 | 2016-06-01 23:53:15 | 54908 | 2009-03-18 00:00:00 | 54542.2187847222 | 2008-03-17 05:15:03 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062040/ | Quick Look | ![]() |
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680 | GC_LARGEPROJECT13 | 264.4001 | -31.8052 | 263.587715 | -31.776061 | 265.18111 | -8.457548 | 356.65040302 | -0.04773216 | 95.4712 | 54881.6929282407 | 2009-02-19 16:37:49 | 54883.0522453704 | 2009-02-21 01:15:14 | 503019010 | 52.7764 | 50 | 52.7764 | 52.7972 | 0 | 52.7844 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4395 | 42.4395 | 117.4338 | 0 | PROCESSED | 57545.6322106482 | 2016-06-06 15:10:23 | 54557 | 2008-04-01 00:00:00 | 54902.1118171296 | 2009-03-12 02:41:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503019010/ | Quick Look | ![]() |
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681 | HESS J1800-240B | 270.1124 | -24.0578 | 269.347343 | -24.056487 | 270.09306 | -0.616951 | 5.8867537 | -0.376417 | 87.1402 | 54562.3157523148 | 2008-04-06 07:34:41 | 54563.0141666667 | 2008-04-07 00:20:24 | 503026010 | 31.6728 | 30 | 31.6728 | 31.6728 | 0 | 31.6728 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.7698 | 26.7698 | 60.32 | 1 | PROCESSED | 57542.2491319444 | 2016-06-03 05:58:45 | 54953 | 2009-05-02 00:00:00 | 54580.1793402778 | 2008-04-24 04:18:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAAKI TANAKA | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503026010/ | Quick Look | ![]() |
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682 | VELA JR P25 | 132.5224 | -46.8921 | 132.101077 | -46.704657 | 159.613489 | -60.474295 | 266.48184745 | -1.82836861 | 347.0024 | 54653.1675462963 | 2008-07-06 04:01:16 | 54653.4335532407 | 2008-07-06 10:24:19 | 503037010 | 13.16 | 10 | 13.16 | 13.16 | 0 | 13.16 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.4325 | 12.4325 | 22.9759 | 0 | PROCESSED | 57542.9817476852 | 2016-06-03 23:33:43 | 55048 | 2009-08-05 00:00:00 | 54679.3166203704 | 2008-08-01 07:35:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503037010/ | Quick Look | ![]() |
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683 | CYGNUS LOOP (P27) | 313.8328 | 30.0104 | 313.308096 | 29.818528 | 328.031945 | 45.024246 | 74.06049539 | -9.7037521 | 49.6211 | 54599.5480092593 | 2008-05-13 13:09:08 | 54600.0494675926 | 2008-05-14 01:11:14 | 503063010 | 22.7843 | 20 | 22.7923 | 22.7843 | 0 | 22.8003 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.0688 | 20.0688 | 43.3239 | 0 | PROCESSED | 57542.5253587963 | 2016-06-03 12:36:31 | 54975 | 2009-05-24 00:00:00 | 54609.1396990741 | 2008-05-23 03:21:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503063010/ | Quick Look | ![]() |
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684 | VICINITY_OF_PKS_2155-2 | 330.1861 | -29.9649 | 329.464287 | -30.205624 | 321.680429 | -16.673826 | 18.22929909 | -52.62033555 | 55.8323 | 54588.3553356482 | 2008-05-02 08:31:41 | 54590.7293865741 | 2008-05-04 17:30:19 | 503083010 | 87.3274 | 80 | 87.3274 | 87.3274 | 0 | 87.3274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.8451 | 75.8451 | 205.1059 | 3 | PROCESSED | 57542.4726736111 | 2016-06-03 11:20:39 | 54975 | 2009-05-24 00:00:00 | 54608.2608912037 | 2008-05-22 06:15:41 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030135 | The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | A | TOSHISHIGE HAGIHARA | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503083010/ | Quick Look | ![]() |
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685 | RIM2 | 311.426 | 31.5946 | 310.913676 | 31.411344 | 326.171395 | 47.287726 | 74.00572356 | -7.09996284 | 246.8661 | 55153.9497337963 | 2009-11-18 22:47:37 | 55154.4843055556 | 2009-11-19 11:37:24 | 504006010 | 26.3059 | 24 | 26.3059 | 26.3059 | 0 | 26.3059 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.237 | 22.237 | 46.1839 | 0 | PROCESSED | 57549.4609490741 | 2016-06-10 11:03:46 | 55534 | 2010-12-04 00:00:00 | 55166.4447916667 | 2009-12-01 10:40:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504006010/ | Quick Look | ![]() |
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686 | RIM3 | 311.3232 | 31.2993 | 310.809596 | 31.116423 | 325.884456 | 47.049295 | 73.71675058 | -7.21258663 | 246.4181 | 55154.4849189815 | 2009-11-19 11:38:17 | 55155.1204166667 | 2009-11-20 02:53:24 | 504007010 | 21.5566 | 19 | 21.5566 | 21.5566 | 0 | 21.5566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.481 | 17.481 | 54.9039 | 0 | PROCESSED | 57549.4865277778 | 2016-06-10 11:40:36 | 55534 | 2010-12-04 00:00:00 | 55166.4304166667 | 2009-12-01 10:19:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504007010/ | Quick Look | ![]() |
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687 | RIM6 | 314.3771 | 31.4503 | 313.858117 | 31.256512 | 329.460239 | 46.161653 | 75.4881661 | -9.14820234 | 247.047 | 55155.7987615741 | 2009-11-20 19:10:13 | 55156.1745833333 | 2009-11-21 04:11:24 | 504010010 | 14.3275 | 11 | 14.3475 | 14.3435 | 0 | 14.3275 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7152 | 10.7152 | 32.468 | 0 | PROCESSED | 57549.4929513889 | 2016-06-10 11:49:51 | 55534 | 2010-12-04 00:00:00 | 55166.4272916667 | 2009-12-01 10:15:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504010010/ | Quick Look | ![]() |
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688 | NEP #1 | 270.0492 | 66.5597 | 270.050416 | 66.559437 | 358.096328 | 89.986108 | 96.38280784 | 29.79186901 | 217.1802 | 55150.229212963 | 2009-11-15 05:30:04 | 55151.1953587963 | 2009-11-16 04:41:19 | 504070010 | 56.3367 | 50 | 56.3367 | 56.3447 | 0 | 56.3447 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41.4345 | 41.4345 | 83.4719 | 2 | PROCESSED | 57549.3863657407 | 2016-06-10 09:16:22 | 54922 | 2009-04-01 00:00:00 | 55162.2062268518 | 2009-11-27 04:56:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504070010/ | Quick Look | ![]() |
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689 | SEP #2 | 89.966 | -66.5714 | 89.96805 | -66.571581 | 300.397678 | -89.984546 | 276.39630454 | -29.82495373 | 163.7813 | 55170.9454166667 | 2009-12-05 22:41:24 | 55172.4863194444 | 2009-12-07 11:40:18 | 504071010 | 57.9991 | 50 | 58.0071 | 57.9991 | 0 | 58.0071 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.4152 | 35.4152 | 133.112 | 1 | PROCESSED | 57549.7252546296 | 2016-06-10 17:24:22 | 54922 | 2009-04-01 00:00:00 | 55187.4854398148 | 2009-12-22 11:39:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504071010/ | Quick Look | ![]() |
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690 | SEP #4 | 89.9798 | -66.5683 | 89.981754 | -66.568414 | 282.855223 | -89.989511 | 276.39272547 | -29.81946932 | 185.1981 | 55192.0059490741 | 2009-12-27 00:08:34 | 55193.3995833333 | 2009-12-28 09:35:24 | 504075010 | 49.9566 | 50 | 49.9566 | 49.9566 | 0 | 49.9566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.143 | 45.143 | 120.3939 | 1 | PROCESSED | 57549.980474537 | 2016-06-10 23:31:53 | 54922 | 2009-04-01 00:00:00 | 55225.3094907407 | 2010-01-29 07:25:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504075010/ | Quick Look | ![]() |
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691 | W28_EASTSHELL | 270.3727 | -23.2858 | 269.612111 | -23.285763 | 270.332756 | 0.154633 | 6.67541903 | -0.20080463 | 88.0003 | 55617.4542939815 | 2011-02-25 10:54:11 | 55620.1723032407 | 2011-02-28 04:08:07 | 505006010 | 99.9816 | 100 | 99.9816 | 99.9816 | 0 | 99.9816 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.6772 | 83.6772 | 234.8157 | 3 | PROCESSED | 57601.1152430556 | 2016-08-01 02:45:57 | 55287 | 2010-04-01 00:00:00 | 55642.1946643518 | 2011-03-22 04:40:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505006010/ | Quick Look | ![]() |
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692 | CYGNUS LOOP 4 | 312.482 | 31.9468 | 311.969326 | 31.759715 | 327.592245 | 47.259949 | 74.84594636 | -7.58533627 | 81.0154 | 55301.6216087963 | 2010-04-15 14:55:07 | 55301.8912037037 | 2010-04-15 21:23:20 | 505012010 | 12.4535 | 12 | 12.4535 | 12.4535 | 0 | 12.4535 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.182 | 12.182 | 23.2801 | 1 | PROCESSED | 57551.2226736111 | 2016-06-12 05:20:39 | 55287 | 2010-04-01 00:00:00 | 55362.3160763889 | 2010-06-15 07:35:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505012010/ | Quick Look | ![]() |
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693 | JUPITER | 104.585 | 23.053 | 103.829387 | 23.12132 | 103.399653 | 0.287954 | 192.87049462 | 11.72496816 | 267.157 | 56768.1148958333 | 2014-04-21 02:45:27 | 56768.2245138889 | 2014-04-21 05:23:18 | 508023140 | 5.2482 | 160 | 5.2642 | 5.2482 | 0 | 5.2708 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9659259259 | 2016-08-14 23:10:56 | 57212 | 2015-07-09 00:00:00 | 56846.5934143518 | 2014-07-08 14:14:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | YUICHIRO EZOE | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508023140/ | Quick Look | ![]() |
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694 | CYGNUS LOOP 13 | 313.3172 | 30.1574 | 312.794183 | 29.967347 | 327.529928 | 45.333203 | 73.89066537 | -9.26489611 | 82.0018 | 55329.8397337963 | 2010-05-13 20:09:13 | 55330.4925694444 | 2010-05-14 11:49:18 | 505021010 | 21.565 | 21 | 21.565 | 21.597 | 0 | 21.565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.12 | 18.12 | 56.3999 | 1 | PROCESSED | 57551.5081597222 | 2016-06-12 12:11:45 | 55287 | 2010-04-01 00:00:00 | 55393.3656712963 | 2010-07-16 08:46:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505021010/ | Quick Look | ![]() |
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695 | CYGNUS LOOP 15 | 313.2124 | 29.6854 | 312.687356 | 29.495723 | 327.15263 | 44.932937 | 73.46064198 | -9.49078141 | 50.2914 | 55343.3019791667 | 2010-05-27 07:14:51 | 55343.6994675926 | 2010-05-27 16:47:14 | 505023010 | 19.2953 | 19 | 19.2953 | 19.2953 | 0 | 19.2953 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.514 | 16.514 | 34.32 | 1 | PROCESSED | 57551.5915972222 | 2016-06-12 14:11:54 | 55287 | 2010-04-01 00:00:00 | 55355.1545833333 | 2010-06-08 03:42:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505023010/ | Quick Look | ![]() |
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696 | WESTERLUND1_1 | 251.8398 | -46.6023 | 250.920426 | -46.513379 | 256.432477 | -24.011612 | 339.00946678 | -0.92860911 | 283.3468 | 55449.7733217593 | 2010-09-10 18:33:35 | 55451.2015740741 | 2010-09-12 04:50:16 | 505049010 | 51.932 | 50 | 51.932 | 51.932 | 0 | 51.932 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.8437 | 44.8437 | 123.3861 | 1 | PROCESSED | 57553.3910532407 | 2016-06-14 09:23:07 | 55829 | 2011-09-25 00:00:00 | 55461.3235069444 | 2010-09-22 07:45:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | HIRONORI MATSUMOTO | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505049010/ | Quick Look | ![]() |
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697 | THE KEPLER SNR | 262.6712 | -21.4826 | 261.921958 | -21.445277 | 263.170111 | 1.784866 | 4.52498243 | 6.82361728 | 97.9009 | 55634.5331712963 | 2011-03-14 12:47:46 | 55635.5759606482 | 2011-03-15 13:49:23 | 505092060 | 46.4961 | 100 | 46.6401 | 46.4961 | 0 | 46.6401 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.6118 | 38.6118 | 90.05 | 1 | PROCESSED | 57601.1934143518 | 2016-08-01 04:38:31 | 55287 | 2010-04-01 00:00:00 | 55648.2987731482 | 2011-03-28 07:10:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092060/ | Quick Look | ![]() |
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698 | CYGNUS LOOP W-B-N | 311.1498 | 30.6623 | 310.633359 | 30.480063 | 325.327706 | 46.517719 | 73.11766027 | -7.48614398 | 71.1125 | 55692.7736574074 | 2011-05-11 18:34:04 | 55693.7709606482 | 2011-05-12 18:30:11 | 506007010 | 45.9006 | 44 | 45.9006 | 45.9006 | 0 | 45.9006 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8337 | 40.8337 | 86.1339 | 0 | PROCESSED | 57602.0331597222 | 2016-08-02 00:47:45 | 56072 | 2012-05-25 00:00:00 | 55705.1432523148 | 2011-05-24 03:26:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060042 | The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 6 | AO6 | HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506007010/ | Quick Look | ![]() |
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699 | CYGNUS LOOP BLOWOUT4 | 312.6611 | 29.185 | 312.13473 | 28.997294 | 326.258052 | 44.653722 | 72.76042835 | -9.42856877 | 61.4261 | 55707.9937268518 | 2011-05-26 23:50:58 | 55708.6620486111 | 2011-05-27 15:53:21 | 506014010 | 26.0551 | 25 | 26.0551 | 26.0631 | 0 | 26.0711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2713 | 20.2713 | 57.7379 | 0 | PROCESSED | 57602.1387037037 | 2016-08-02 03:19:44 | 56092 | 2012-06-14 00:00:00 | 55725.2494097222 | 2011-06-13 05:59:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506014010/ | Quick Look | ![]() |
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700 | S147_NE | 85.8826 | 28.3008 | 85.092656 | 28.278902 | 86.363834 | 4.912026 | 180.30181638 | -0.72311498 | 273.9004 | 55996.1741666667 | 2012-03-10 04:10:48 | 55997.2919097222 | 2012-03-11 07:00:21 | 506030010 | 48.0142 | 45 | 48.0302 | 48.0142 | 0 | 48.0382 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.608 | 42.608 | 96.5559 | 0 | PROCESSED | 57604.8622685185 | 2016-08-04 20:41:40 | 56385 | 2013-04-03 00:00:00 | 56016.6658912037 | 2012-03-30 15:58:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060080 | We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it. | GALACTIC DIFFUSE EMISSION | 5 | C | YOSHITAKA HANABATA | JAP | 6 | AO6 | STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506030010/ | Quick Look | ![]() |
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701 | VELA PWN NE1 | 129.3684 | -44.9817 | 128.942936 | -44.80588 | 153.830902 | -60.001311 | 263.62243766 | -2.36980886 | 142.6395 | 55916.6230439815 | 2011-12-21 14:57:11 | 55917.0070601852 | 2011-12-22 00:10:10 | 506041010 | 15.408 | 15 | 15.424 | 15.408 | 0 | 15.424 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.5681 | 11.5681 | 33.1759 | 1 | PROCESSED | 57604.1925347222 | 2016-08-04 04:37:15 | 56305 | 2013-01-13 00:00:00 | 55937.7788310185 | 2012-01-11 18:41:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506041010/ | Quick Look | ![]() |
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702 | VELA PWN E2 | 129.5733 | -45.3227 | 129.149771 | -45.146105 | 154.428094 | -60.221749 | 263.98172095 | -2.46094632 | 304.5019 | 55711.9038773148 | 2011-05-30 21:41:35 | 55712.1328935185 | 2011-05-31 03:11:22 | 506045010 | 13.904 | 15 | 13.92 | 13.904 | 0 | 13.92 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.404 | 8.404 | 19.7759 | 0 | PROCESSED | 57602.1624074074 | 2016-08-02 03:53:52 | 56092 | 2012-06-14 00:00:00 | 55725.2563888889 | 2011-06-13 06:09:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | SATORU KATSUDA | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506045010/ | Quick Look | ![]() |
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703 | FERMI_BUBBLE_N1 | 234.2494 | 5.0833 | 233.629011 | 5.247167 | 230.509588 | 23.755664 | 11.24626366 | 44.86747445 | 287.5001 | 56144.9615277778 | 2012-08-05 23:04:36 | 56145.3981365741 | 2012-08-06 09:33:19 | 507001010 | 21.0485 | 20 | 21.0485 | 21.0485 | 0 | 21.0485 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.5275 | 17.5275 | 37.7199 | 1 | PROCESSED | 57606.7753703704 | 2016-08-06 18:36:32 | 56533 | 2013-08-29 00:00:00 | 56167.2004166667 | 2012-08-28 04:48:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507001010/ | Quick Look | ![]() |
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704 | FERMI_BUBBLE_N8 | 234.713 | 2.1937 | 234.081258 | 2.355767 | 231.775859 | 21.073749 | 8.32709248 | 42.83416107 | 287.4999 | 56148.4316782407 | 2012-08-09 10:21:37 | 56148.9953240741 | 2012-08-09 23:53:16 | 507008010 | 22.115 | 20 | 22.119 | 22.115 | 0 | 22.123 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22.3246 | 22.3246 | 48.694 | 0 | PROCESSED | 57606.8152546296 | 2016-08-06 19:33:58 | 56536 | 2013-09-01 00:00:00 | 56169.1379976852 | 2012-08-30 03:18:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507008010/ | Quick Look | ![]() |
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705 | FERMI_BUBBLE_S5 | 332.6607 | -46.1905 | 331.884331 | -46.436996 | 316.726495 | -32.387556 | 351.01438321 | -53.09632639 | 44.0062 | 56036.5915625 | 2012-04-19 14:11:51 | 56037.1140972222 | 2012-04-20 02:44:18 | 507013010 | 21.0044 | 20 | 21.0124 | 21.0204 | 0 | 21.0044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.8854 | 20.8854 | 45.1099 | 0 | PROCESSED | 57605.2184259259 | 2016-08-05 05:14:32 | 56420 | 2013-05-08 00:00:00 | 56049.260787037 | 2012-05-02 06:15:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507013010/ | Quick Look | ![]() |
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706 | MBM16 | 49.7705 | 11.5801 | 49.086905 | 11.399033 | 50.445581 | -6.509248 | 170.60706006 | -37.27124926 | 254.3335 | 56691.5957175926 | 2014-02-03 14:17:50 | 56693.5209953704 | 2014-02-05 12:30:14 | 508078020 | 87.8509 | 80 | 87.8509 | 87.8589 | 0 | 87.8589 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7866782407 | 2016-08-13 18:52:49 | 56383 | 2013-04-01 00:00:00 | 56706.5234375 | 2014-02-18 12:33:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | MASSIMILIANO GALEAZZI | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508078020/ | Quick Look | ![]() |
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707 | GC_SOUTH_4 | 268.4148 | -29.4524 | 267.616941 | -29.442757 | 268.602472 | -6.019039 | 0.45858363 | -1.77042753 | 273.9837 | 56206.6347106482 | 2012-10-06 15:13:59 | 56207.6987731482 | 2012-10-07 16:46:14 | 507031010 | 52.8743 | 50 | 52.8903 | 52.8903 | 0 | 52.8743 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 54.1402 | 54.1402 | 91.9199 | 0 | PROCESSED | 57607.3059837963 | 2016-08-07 07:20:37 | 56595 | 2013-10-30 00:00:00 | 56226.5383449074 | 2012-10-26 12:55:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | SHINYA NAKASHIMA | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507031010/ | Quick Look | ![]() |
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708 | G32.8-0.1 NORTH | 282.8355 | -0.0511 | 282.194351 | -0.111437 | 283.93132 | 22.770824 | 32.87550481 | -0.00195799 | 74.4992 | 56037.6100347222 | 2012-04-20 14:38:27 | 56038.7897685185 | 2012-04-21 18:57:16 | 507035010 | 55.1475 | 50 | 55.1475 | 55.1475 | 0 | 55.1475 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 53.4834 | 53.4834 | 101.9259 | 0 | PROCESSED | 57605.250162037 | 2016-08-05 06:00:14 | 56421 | 2013-05-09 00:00:00 | 56054.2396990741 | 2012-05-07 05:45:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | AYA BAMBA | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507035010/ | Quick Look | ![]() |
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709 | W44_SOUTH | 284.0612 | 1.21 | 283.425992 | 1.143849 | 285.397736 | 23.902065 | 34.55680978 | -0.51750637 | 254.9998 | 56587.9436921296 | 2013-10-22 22:38:55 | 56589.5105671296 | 2013-10-24 12:15:13 | 508003010 | 66.7193 | 100 | 66.7333 | 66.7284 | 0 | 66.7193 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 59.54 | 59.54 | 135.3439 | 0 | PROCESSED | 57613.1119675926 | 2016-08-13 02:41:14 | 57193 | 2015-06-20 00:00:00 | 56603.6796180556 | 2013-11-07 16:18:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508003010/ | Quick Look | ![]() |
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710 | W28_SOUTH | 270.2594 | -23.5602 | 269.497229 | -23.559609 | 270.228192 | -0.119534 | 6.38554367 | -0.24638203 | 269.9307 | 56938.465162037 | 2014-10-08 11:09:50 | 56939.7308101852 | 2014-10-09 17:32:22 | 508006020 | 61.7346 | 60 | 61.7346 | 61.7385 | 0 | 61.7465 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6318402778 | 2016-08-16 15:09:51 | 57359 | 2015-12-03 00:00:00 | 56993.4258333333 | 2014-12-02 10:13:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080017 | A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP. | GALACTIC DIFFUSE EMISSION | 5 | A | MAKOTO SAWADA | JAP | 8 | AO8 | INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508006020/ | Quick Look | ![]() |
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711 | NW_BGD | 233.685 | -9.8963 | 233.005634 | -9.73009 | 233.775325 | 9.095249 | 355.50550051 | 35.80785483 | 289.7923 | 56499.8451041667 | 2013-07-26 20:16:57 | 56500.4266319445 | 2013-07-27 10:14:21 | 508008010 | 24.1275 | 20 | 24.1275 | 24.1275 | 0 | 24.1275 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.0402 | 22.0402 | 50.216 | 1 | PROCESSED | 57612.0809953704 | 2016-08-12 01:56:38 | 56955 | 2014-10-25 00:00:00 | 56587.4600578704 | 2013-10-22 11:02:29 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | MASAYA TAHARA | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508008010/ | Quick Look | ![]() |
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712 | CAS A | 350.8384 | 58.8278 | 350.272774 | 58.553239 | 27.387727 | 54.868389 | 111.73335389 | -2.11549771 | 73.3126 | 56828.040162037 | 2014-06-20 00:57:50 | 56828.7711111111 | 2014-06-20 18:30:24 | 508011020 | 28.0732 | 30 | 28.0812 | 28.0732 | 0 | 29.7402 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 30.9971 | 30.9971 | 63.1439 | 2 | PROCESSED | 57615.2981712963 | 2016-08-15 07:09:22 | 57206 | 2015-07-03 00:00:00 | 56839.7807986111 | 2014-07-01 18:44:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080021 | We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHITOMO MAEDA | JAP | 8 | AO8 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508011020/ | Quick Look | ![]() |
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713 | HESS J1641-463 | 250.6069 | -46.2544 | 249.692976 | -46.159834 | 255.458921 | -23.78613 | 338.71856162 | -0.05766971 | 282.1914 | 56898.1501736111 | 2014-08-29 03:36:15 | 56898.2719907407 | 2014-08-29 06:31:40 | 509010010 | 0 | 40 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5288773148 | 2016-08-16 12:41:35 | 56748 | 2014-04-01 00:00:00 | 56979.4106944445 | 2014-11-18 09:51:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090045 | The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 9 | AO9 | IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509010010/ | Quick Look | ![]() |
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714 | G166.0+4.3_SE | 81.6669 | 42.6537 | 80.773056 | 42.61122 | 83.513405 | 19.400906 | 166.36639381 | 4.14814693 | 85.0186 | 56921.2402777778 | 2014-09-21 05:46:00 | 56922.0209606482 | 2014-09-22 00:30:11 | 509024010 | 31.2731 | 60 | 31.2731 | 34.2171 | 0 | 34.2731 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5684722222 | 2016-08-16 13:38:36 | 57626 | 2016-08-26 00:00:00 | 56945.4935532407 | 2014-10-15 11:50:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | AKIHIRO TAKATA | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509024010/ | Quick Look | ![]() |
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715 | 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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716 | RCW86_NORTH | 220.4956 | -62.2074 | 219.51679 | -61.994077 | 240.607034 | -43.72111 | 315.43082177 | -2.04872285 | 96.1584 | 54860.901099537 | 2009-01-29 21:37:35 | 54862.1175231482 | 2009-01-31 02:49:14 | 503002010 | 55.376 | 50 | 55.384 | 55.384 | 0 | 55.376 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.2731 | 50.2731 | 105.0818 | 2 | PROCESSED | 57545.4267939815 | 2016-06-06 10:14:35 | 55329 | 2010-05-13 00:00:00 | 54880.5551041667 | 2009-02-18 13:19:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROYA YAMAGUCHI | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503002010/ | Quick Look | ![]() |
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717 | KES 79 | 283.1953 | 0.6959 | 282.557686 | 0.633849 | 284.399792 | 23.479242 | 33.70438491 | 0.01846016 | 73.5801 | 55674.9437152778 | 2011-04-23 22:38:57 | 55676.4716782407 | 2011-04-25 11:19:13 | 506059010 | 50.897 | 50 | 50.897 | 50.897 | 0 | 50.897 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8978 | 40.8978 | 131.96 | 2 | PROCESSED | 57601.597025463 | 2016-08-01 14:19:43 | 55652 | 2011-04-01 00:00:00 | 55697.1427083333 | 2011-05-16 03:25:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506059010/ | Quick Look | ![]() |
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718 | 3C400.2 NE | 294.7841 | 17.3445 | 294.222174 | 17.229031 | 300.592872 | 38.189932 | 53.75798011 | -2.26924911 | 81.5891 | 56770.0289351852 | 2014-04-23 00:41:40 | 56770.4640162037 | 2014-04-23 11:08:11 | 509071010 | 20.231 | 20 | 20.239 | 20.239 | 0 | 20.231 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.505 | 18.505 | 37.5838 | 0 | PROCESSED | 57614.9798148148 | 2016-08-14 23:30:56 | 57152 | 2015-05-10 00:00:00 | 56789.6056712963 | 2014-05-12 14:32:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | JACCO VINK | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509071010/ | Quick Look | ![]() |
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719 | W63 | 304.8117 | 45.7821 | 304.405742 | 45.623994 | 328.881818 | 62.294552 | 82.4091518 | 5.43831098 | 57.9996 | 57171.5134837963 | 2015-05-29 12:19:25 | 57172.616712963 | 2015-05-30 14:48:04 | 510025010 | 42.7003 | 150 | 44.302 | 44.606 | 0 | 42.7003 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.7747 | 13.7747 | 92.7739 | 0 | PROCESSED | 57618.8028703704 | 2016-08-18 19:16:08 | 57636 | 2016-09-05 00:00:00 | 57260.7216898148 | 2015-08-26 17:19:14 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101315 | We propose to conduct a deep Suzaku observation of the X-ray bright central portion of the Galactic supernova remnant (SNR) W63 (G82.2+5.3). This SNR belongs to a class of objects known as mixed-morphology SNRs (MMSNRs) that feature a shell-like radio morphology with a center-filled thermal X-ray morphology: the origin of these contrasting morphologies for these SNRs remains unknown. Our proposed Suzaku observation of this SNR will investigate the putative overabundances of such elements as magnesium, silicon and sulfur (as reported in a previous analysis of an ASCA observation of W63) as well as search for evidence of over-ionization conditions in the X-ray emitting plasma, as has been reported for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | C | THOMAS PANNUTI | USA | 10 | AO10 | A SUZAKU OBSERVATION OF THE GALACTIC SUPERNOVA REMNANT W63 (G82.2+5.3) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/510025010/ | Quick Look | ![]() |
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720 | 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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721 | GC19 | 265.8593 | -28.4466 | 265.068242 | -28.424576 | 266.336192 | -5.058113 | 0.1669402 | 0.66404713 | 262.6738 | 54384.9647569444 | 2007-10-11 23:09:15 | 54385.4112731482 | 2007-10-12 09:52:14 | 502007010 | 22.0174 | 20 | 22.0174 | 22.0414 | 0 | 22.0254 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.5248 | 19.5248 | 38.572 | 0 | PROCESSED | 57540.2498842593 | 2016-06-01 05:59:50 | 54771 | 2008-11-01 00:00:00 | 54402.4381365741 | 2007-10-29 10:30:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | MOTOHIDE KOKUBUN | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502007010/ | Quick Look | ![]() |
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722 | VELA JR P16 | 132.6844 | -46.1051 | 132.256587 | -45.917087 | 158.947915 | -59.751955 | 265.94403391 | -1.24290223 | 347.0001 | 54291.4605671296 | 2007-07-10 11:03:13 | 54291.7363773148 | 2007-07-10 17:40:23 | 502038010 | 16.442 | 10 | 16.45 | 16.45 | 0 | 16.442 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.277 | 16.277 | 23.8239 | 1 | PROCESSED | 57539.143900463 | 2016-05-31 03:27:13 | 54696 | 2008-08-18 00:00:00 | 54328.4979398148 | 2007-08-16 11:57:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502038010/ | Quick Look | ![]() |
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723 | COMET_8P_TUTTLE-P1-7 | 28.2572 | 6.4878 | 27.602012 | 6.241824 | 28.565429 | -4.78789 | 149.08057764 | -53.2281425 | 248.4991 | 54470.9158333333 | 2008-01-05 21:58:48 | 54470.9820717593 | 2008-01-05 23:34:11 | 502062070 | 3.219 | 2 | 3.219 | 3.219 | 0 | 3.219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3.459 | 3.459 | 5.664 | 0 | PROCESSED | 57541.0036805556 | 2016-06-02 00:05:18 | 54908 | 2009-03-18 00:00:00 | 54542.2385532407 | 2008-03-17 05:43:31 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062070/ | Quick Look | ![]() |
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724 | GC_LARGEPROJECT12 | 264.5561 | -31.5945 | 263.745071 | -31.566119 | 265.306919 | -8.241878 | 356.89942182 | -0.04701536 | 96.416 | 54881.313900463 | 2009-02-19 07:32:01 | 54881.6919444445 | 2009-02-19 16:36:24 | 503018030 | 11.914 | 10 | 11.922 | 11.922 | 0 | 11.914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.0909 | 10.0909 | 32.6579 | 1 | PROCESSED | 57545.5776041667 | 2016-06-06 13:51:45 | 54557 | 2008-04-01 00:00:00 | 54895.5872106482 | 2009-03-05 14:05:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503018030/ | Quick Look | ![]() |
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725 | HESSJ1614-B | 243.5783 | -51.8962 | 242.621623 | -51.770198 | 251.47747 | -30.138638 | 331.46625372 | -0.63583262 | 283.7142 | 54730.5632291667 | 2008-09-21 13:31:03 | 54731.2779166667 | 2008-09-22 06:40:12 | 503074010 | 52.6342 | 50 | 52.6422 | 52.6342 | 0 | 52.6342 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.953 | 42.953 | 61.7359 | 0 | PROCESSED | 57543.9760763889 | 2016-06-04 23:25:33 | 55148 | 2009-11-13 00:00:00 | 54780.4609490741 | 2008-11-10 11:03:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030088 | The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | HIRONORI MATSUMOTO | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503074010/ | Quick Look | ![]() |
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726 | VELA JR P19 | 133.9797 | -46.1476 | 133.547729 | -45.954999 | 160.484775 | -59.304415 | 266.55257885 | -0.58147519 | 346.9993 | 54650.629849537 | 2008-07-03 15:06:59 | 54651.2362731482 | 2008-07-04 05:40:14 | 503031010 | 19.8174 | 10 | 19.8174 | 19.8174 | 0 | 19.8174 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.1564 | 17.1564 | 52.3839 | 1 | PROCESSED | 57542.9517824074 | 2016-06-03 22:50:34 | 55036 | 2009-07-24 00:00:00 | 54665.3240393518 | 2008-07-18 07:46:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | YASUNOBU UCHIYAMA | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503031010/ | Quick Look | ![]() |
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727 | KEPLER_BG_GN | 261.9141 | -20.2308 | 261.17196 | -20.189852 | 262.396131 | 2.997058 | 5.199252 | 8.09662946 | 270.3619 | 55105.4689699074 | 2009-10-01 11:15:19 | 55107.4279976852 | 2009-10-03 10:16:19 | 504103010 | 68.6043 | 60 | 68.6043 | 68.6043 | 0 | 68.6123 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.8014 | 55.8014 | 169.2279 | 1 | PROCESSED | 57548.7547800926 | 2016-06-09 18:06:53 | 54922 | 2009-04-01 00:00:00 | 55125.6331828704 | 2009-10-21 15:11:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | SANGWOOK PARK | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504103010/ | Quick Look | ![]() |
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728 | G276.2-7.7 | 135.4479 | -58.0976 | 135.120843 | -57.899721 | 179.6274 | -67.871169 | 276.2324482 | -7.68832918 | 319.4197 | 56102.2534722222 | 2012-06-24 06:05:00 | 56102.610625 | 2012-06-24 14:39:18 | 507066010 | 10.2994 | 10 | 10.2994 | 10.2994 | 0 | 10.2994 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.6275 | 11.6275 | 30.8559 | 0 | PROCESSED | 57605.7340972222 | 2016-08-05 17:37:06 | 56582 | 2013-10-17 00:00:00 | 56219.6536458333 | 2012-10-19 15:41:15 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | TOBIAS PRINZ | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507066010/ | Quick Look | ![]() |
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729 | VELA PWN S2 | 128.0787 | -47.1859 | 127.674645 | -47.014943 | 154.605433 | -62.350481 | 264.85904608 | -4.40317226 | 122.1879 | 56989.4162847222 | 2014-11-28 09:59:27 | 56989.8404976852 | 2014-11-28 20:10:19 | 509018010 | 17.4774 | 15 | 17.4774 | 17.4774 | 0 | 17.4774 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4063773148 | 2016-08-17 09:45:11 | 57368 | 2015-12-12 00:00:00 | 57002.436087963 | 2014-12-11 10:27:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | KOJI MORI | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509018010/ | Quick Look | ![]() |
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730 | G189 NORTH | 94.8937 | 22.8595 | 94.136063 | 22.881413 | 94.510579 | -0.50482 | 189.05453502 | 3.64004382 | 92.0693 | 56941.8561458333 | 2014-10-11 20:32:51 | 56944.6669328704 | 2014-10-14 16:00:23 | 509035010 | 100.65 | 100 | 100.65 | 102.898 | 0 | 102.922 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.652337963 | 2016-08-16 15:39:22 | 57362 | 2015-12-06 00:00:00 | 56996.4204282407 | 2014-12-05 10:05:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091314 | We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars. | GALACTIC DIFFUSE EMISSION | 5 | B | BRIAN WILLIAMS | USA | 9 | AO9 | OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509035010/ | Quick Look | ![]() |
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731 | 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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732 | HESS J1745-303 2 | 266.4705 | -30.0867 | 265.668866 | -30.067612 | 266.916061 | -6.683329 | 359.0474588 | -0.64781783 | 70.5003 | 54531.5601388889 | 2008-03-06 13:26:36 | 54533.6669444444 | 2008-03-08 16:00:24 | 502017010 | 72.5443 | 67 | 72.5523 | 72.5523 | 0 | 72.5443 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.9723 | 63.9723 | 182.0149 | 2 | PROCESSED | 57541.8457291667 | 2016-06-02 20:17:51 | 54919 | 2009-03-29 00:00:00 | 54550.4057986111 | 2008-03-25 09:44:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | RYO YAMAZAKI | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502017010/ | Quick Look | ![]() |
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733 | ARC_BACKGROUND | 39.2055 | -35.7283 | 38.691278 | -35.944876 | 20.761341 | -47.725244 | 240.48717091 | -66.02341726 | 233.8071 | 54830.2554861111 | 2008-12-30 06:07:54 | 54835.3468055556 | 2009-01-04 08:19:24 | 503104010 | 201.8775 | 140 | 201.9575 | 201.8775 | 0 | 201.9815 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5.5028 | 5.5028 | 14.506 | 0 | PROCESSED | 57545.0672685185 | 2016-06-06 01:36:52 | 55328 | 2010-05-12 00:00:00 | 54851.4354166667 | 2009-01-20 10:27:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031235 | Aside from the lengthy bright arcs in the northern sky, few X-ray bright, high latitude regions are understood. Yet, studying this gas is important for understanding the Galactic halo. Here, we propose to study a medium-sized (~7 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make Suzaku observations of the arc and nearby background. With them and an existing Suzaku observation, we will be able to determine the thermal properties of the arc plasma and if the arc is the bright limb of a hot bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | ROBIN SHELTON | USA | 3 | AO3 | A CLOSER LOOT AT HOT HALO GAS: A SUZAKU STUDY OF AN X-RAY BRIGHT ARC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503104010/ | Quick Look | ![]() |
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734 | ASO0382 | 265.491 | -20.8915 | 264.744419 | -20.867803 | 265.774532 | 2.483348 | 6.43327069 | 4.9108593 | 101.5727 | 55276.7369328704 | 2010-03-21 17:41:11 | 55277.3869675926 | 2010-03-22 09:17:14 | 504040010 | 21.2223 | 20 | 21.2223 | 21.2223 | 0 | 21.2223 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3.974 | 3.974 | 56.1089 | 2 | PROCESSED | 57550.9335069444 | 2016-06-11 22:24:15 | 55665 | 2011-04-14 00:00:00 | 55299.411875 | 2010-04-13 09:53:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUYUKI KAWAI | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504040010/ | Quick Look | ![]() |
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735 | 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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736 | COMET_8P_TUTTLE-P1_BGD-2 | 28.5654 | 5.0072 | 27.913501 | 4.76193 | 28.330895 | -6.281929 | 150.57128999 | -54.45813442 | 248.5002 | 54471.5006018518 | 2008-01-06 12:00:52 | 54471.6876273148 | 2008-01-06 16:30:11 | 502061020 | 5.6821 | 4 | 5.6901 | 5.6821 | 0 | 5.6967 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.598 | 5.598 | 16.1519 | 0 | PROCESSED | 57541.2728819444 | 2016-06-02 06:32:57 | 54908 | 2009-03-18 00:00:00 | 54542.2619097222 | 2008-03-17 06:17:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502061020/ | Quick Look | ![]() |
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737 | COMET_8P_TUTTLE-P1_BGD-1 | 28.5142 | 5.254 | 27.861749 | 5.008612 | 28.370132 | -6.032929 | 150.31676982 | -54.25438929 | 248.4996 | 54471.3338888889 | 2008-01-06 08:00:48 | 54471.5001273148 | 2008-01-06 12:00:11 | 502061010 | 8.39 | 6 | 8.39 | 8.39 | 0 | 8.39 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.4419 | 7.4419 | 14.3439 | 0 | PROCESSED | 57541.2728935185 | 2016-06-02 06:32:58 | 54908 | 2009-03-18 00:00:00 | 54542.2616319444 | 2008-03-17 06:16:45 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502061010/ | Quick Look | ![]() |
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738 | COMET_8P_TUTTLE-P1-13 | 28.5683 | 5.0085 | 27.916397 | 4.763237 | 28.334076 | -6.281727 | 150.57488577 | -54.45575395 | 248.5007 | 54471.3158333333 | 2008-01-06 07:34:48 | 54471.3334606482 | 2008-01-06 08:00:11 | 502062130 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1.5039 | 0 | PROCESSED | 57541.2672337963 | 2016-06-02 06:24:49 | 54910 | 2009-03-20 00:00:00 | 54544.4202893518 | 2008-03-19 10:05:13 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062130/ | Quick Look | ![]() |
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739 | G296.1-0.5S | 177.6962 | -62.7172 | 177.080034 | -62.439005 | 216.307928 | -55.355417 | 296.04515802 | -0.65925146 | 111.5869 | 54482.7727662037 | 2008-01-17 18:32:47 | 54484.6668402778 | 2008-01-19 16:00:15 | 502069010 | 69.213 | 67 | 69.213 | 69.213 | 0 | 69.213 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.0096 | 61.0096 | 163.6237 | 2 | PROCESSED | 57541.3665740741 | 2016-06-02 08:47:52 | 54929 | 2009-04-08 00:00:00 | 54563.4417824074 | 2008-04-07 10:36:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | C | KAZIMIERZ BORKOWSKI | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502069010/ | Quick Look | ![]() |
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740 | EXTENDED CHIMNEY | 265.9856 | -29.2095 | 265.189699 | -29.188076 | 266.46906 | -5.817544 | 359.57541621 | 0.16970004 | 69.9995 | 54896.1105555556 | 2009-03-06 02:39:12 | 54899.1218171296 | 2009-03-09 02:55:25 | 503072010 | 140.5733 | 133 | 140.5733 | 140.5733 | 0 | 140.5733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135.4784 | 135.4784 | 260.128 | 1 | PROCESSED | 57545.7802546296 | 2016-06-06 18:43:34 | 55330 | 2010-05-14 00:00:00 | 54916.5067361111 | 2009-03-26 12:09:42 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030086 | We have discovered a chimney structure in the Sgr C region with Suzaku. The Suzaku spectrum of the chimney shows typical parameters of a super nova remnant. However, the chimney has a linear shape, which is inconsistent with a SNR. Thus, we are considering that the chimney is a blowout from super bubble in the Sgr C region. Another possible scenario is that the chimney would be a part of a shell structure formed by explosions (starburst activities, Sgr A*, magnetic reconnection) in the region of Sgr A and Sgr C. Thus, in this proposal, we would like to investigate the structure extending from the chimney. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKESHI TSURU | JAP | 3 | AO3 | THE CHIMNEY OF SGR C : A PART OF A SUPER BUBBLE = A SUPER SHELL ? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503072010/ | Quick Look | ![]() |
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741 | G12.8-0.0 | 273.3975 | -17.831 | 272.667266 | -17.845732 | 273.239831 | 5.571499 | 12.81826803 | -0.01988984 | 90.5577 | 54894.8233680556 | 2009-03-04 19:45:39 | 54896.1050810185 | 2009-03-06 02:31:19 | 503087010 | 56.2026 | 50 | 56.2026 | 56.2026 | 0 | 56.2059 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.5312 | 51.5312 | 110.7278 | 1 | PROCESSED | 57545.7287962963 | 2016-06-06 17:29:28 | 55329 | 2010-05-13 00:00:00 | 54908.5701388889 | 2009-03-18 13:41:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | JOSEPH GELFAND | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/503087010/ | Quick Look | ![]() |
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742 | BLOWOUT4 | 312.7282 | 31.6832 | 312.213719 | 31.495234 | 327.721378 | 46.935084 | 74.77065214 | -7.91349372 | 242.7253 | 55160.4733564815 | 2009-11-25 11:21:38 | 55161.0044444445 | 2009-11-26 00:06:24 | 504014010 | 17.7696 | 15 | 17.8257 | 17.7696 | 0 | 17.8256 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14.2657 | 14.2657 | 45.876 | 0 | PROCESSED | 57549.5615509259 | 2016-06-10 13:28:38 | 55545 | 2010-12-15 00:00:00 | 55176.2692939815 | 2009-12-11 06:27:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504014010/ | Quick Look | ![]() |
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743 | GALACTICDISC3-2 | 16.1096 | 72.7817 | 15.228315 | 72.513728 | 58.016186 | 57.534015 | 123.90816526 | 9.93459858 | 241.5401 | 55216.0250115741 | 2010-01-20 00:36:01 | 55217.5772685185 | 2010-01-21 13:51:16 | 504039010 | 73.5282 | 70 | 73.5282 | 73.5282 | 0 | 73.5282 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.648 | 54.648 | 134.1058 | 1 | PROCESSED | 57550.3049884259 | 2016-06-11 07:19:11 | 55602 | 2011-02-10 00:00:00 | 55236.1178240741 | 2010-02-09 02:49:40 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040097 | To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | C | SHUNSUKE KIMURA | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504039010/ | Quick Look | ![]() |
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744 | G348.5+0.1 | 258.6301 | -38.5295 | 257.772536 | -38.472556 | 260.783274 | -15.450832 | 348.44223752 | 0.09652262 | 91.401 | 55247.6321180556 | 2010-02-20 15:10:15 | 55248.7592476852 | 2010-02-21 18:13:19 | 504097010 | 53.8106 | 50 | 53.8106 | 53.8106 | 0 | 53.8106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3929 | 46.3929 | 97.3598 | 1 | PROCESSED | 57550.6723842593 | 2016-06-11 16:08:14 | 54922 | 2009-04-01 00:00:00 | 55257.0343287037 | 2010-03-02 00:49:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504097010/ | Quick Look | ![]() |
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745 | CYGNUS LOOP 16 | 312.8966 | 29.5255 | 312.371396 | 29.336949 | 326.707962 | 44.890523 | 73.15999246 | -9.37678246 | 49.3574 | 55343.7003125 | 2010-05-27 16:48:27 | 55344.4932407407 | 2010-05-28 11:50:16 | 505024010 | 34.8338 | 34 | 34.8338 | 34.8338 | 0 | 34.8338 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.4182 | 32.4182 | 68.5079 | 1 | PROCESSED | 57551.6200231482 | 2016-06-12 14:52:50 | 55287 | 2010-04-01 00:00:00 | 55355.2000115741 | 2010-06-08 04:48:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI TSUNEMI | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505024010/ | Quick Look | ![]() |
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746 | 0534-69.9 | 83.5094 | -69.9134 | 83.62618 | -69.94462 | 302.596953 | -85.878508 | 280.47493809 | -31.97334872 | 273.4822 | 55286.3873726852 | 2010-03-31 09:17:49 | 55289.2981597222 | 2010-04-03 07:09:21 | 505064010 | 109.2367 | 100 | 109.2687 | 109.2367 | 0 | 109.2767 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79.8262 | 79.8262 | 251.4437 | 2 | PROCESSED | 57551.1453819445 | 2016-06-12 03:29:21 | 55287 | 2010-04-01 00:00:00 | 55302.4291898148 | 2010-04-16 10:18:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | KAZIMIERZ BORKOWSKI | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505064010/ | Quick Look | ![]() |
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747 | GALACTIC_BULGE18 | 269.3126 | -34.5716 | 268.480017 | -34.566233 | 269.41346 | -11.131891 | 356.40349802 | -4.99577293 | 70.9023 | 55633.4308101852 | 2011-03-13 10:20:22 | 55634.5273263889 | 2011-03-14 12:39:21 | 505087010 | 51.4284 | 50 | 51.4684 | 51.4284 | 0 | 51.4755 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44.2072 | 44.2072 | 94.7279 | 1 | PROCESSED | 57601.1565046296 | 2016-08-01 03:45:22 | 55287 | 2010-04-01 00:00:00 | 55649.0417824074 | 2011-03-29 01:00:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505087010/ | Quick Look | ![]() |
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748 | HB21 SOUTH | 311.2245 | 50.5821 | 310.838387 | 50.399364 | 342.625257 | 64.000491 | 88.82715261 | 4.80607932 | 6.557 | 55767.8922337963 | 2011-07-25 21:24:49 | 55768.4953819444 | 2011-07-26 11:53:21 | 506005020 | 23.4607 | 20 | 23.4687 | 23.4767 | 0 | 23.4607 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.2649 | 26.2649 | 52.1039 | 1 | PROCESSED | 57602.6622685185 | 2016-08-02 15:53:40 | 56159 | 2012-08-20 00:00:00 | 55792.1611458333 | 2011-08-19 03:52:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060011 | Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | AYA BAMBA | JAP | 6 | AO6 | ORIGIN OF OVER-IONIZATION OF SNR PLASMAS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506005020/ | Quick Look | ![]() |
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749 | JUPITER | 28.6779 | 10.4549 | 28.01316 | 10.209883 | 30.347447 | -1.217435 | 147.25964186 | -49.40473582 | 249.1856 | 55929.8714467593 | 2012-01-03 20:54:53 | 55930.8243865741 | 2012-01-04 19:47:07 | 506006010 | 33.5331 | 160 | 33.5331 | 33.5331 | 0 | 33.5331 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.1369 | 32.1369 | 82.3239 | 1 | PROCESSED | 57604.310625 | 2016-08-04 07:27:18 | 56316 | 2013-01-24 00:00:00 | 55946.1978472222 | 2012-01-20 04:44:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | KUMI ISHIKAWA | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506006010/ | Quick Look | ![]() |
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750 | G352.7-0.1 | 261.9227 | -35.1119 | 261.088463 | -35.070764 | 263.245639 | -11.859611 | 352.75195989 | -0.12120729 | 94.0335 | 55988.8605671296 | 2012-03-02 20:39:13 | 55993.5536111111 | 2012-03-07 13:17:12 | 506052010 | 201.5474 | 200 | 201.5474 | 201.5474 | 0 | 201.5474 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 171.544 | 171.544 | 405.4396 | 4 | PROCESSED | 57604.9422569445 | 2016-08-04 22:36:51 | 56375 | 2013-03-24 00:00:00 | 56008.397337963 | 2012-03-22 09:32:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061315 | Supernova remnants showing strong Fe K emission are relatively rare, and primarily of Type Ia. We propose a long observation of one of the least well-studied Fe-rich Galactic SNRs, G352.7-0.1, with the goal of characterizing the Fe emission, confirming its likely identification as the remnant of a Type Ia supernova, and constraining the properties of ejected material and the dynamics of the explosion. Its thermal X-ray spectrum is strikingly similar to Tycho's SNR, but unexpectedly X-rays are uniformly distributed throughout the remnant. Our proposed observation will produce high-quality spectra, adequate for detailed studies with some spatial information, that will greatly aid in understanding of this very interesting young remnant. | GALACTIC DIFFUSE EMISSION | 5 | C | KAZIMIERZ BORKOWSKI | USA | 6 | AO6 | STRONG IRON EMISSION IN THE SUPERNOVA REMNANT G352.7-0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506052010/ | Quick Look | ![]() |
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751 | VELA JR WEST1 | 131.7706 | -46.5645 | 131.349361 | -46.379775 | 158.374389 | -60.478179 | 265.90247722 | -2.02224689 | 126.9994 | 56630.5848611111 | 2013-12-04 14:02:12 | 56631.1640162037 | 2013-12-05 03:56:11 | 508036010 | 28.5509 | 30 | 28.5589 | 28.5589 | 0 | 28.5509 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.35 | 27.35 | 50.0179 | 0 | PROCESSED | 57613.5034375 | 2016-08-13 12:04:57 | 57061 | 2015-02-08 00:00:00 | 56695.6005092593 | 2014-02-07 14:24:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | HIDETOSHI SANO | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508036010/ | Quick Look | ![]() |
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752 | 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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753 | GALACTIC RIDGE | 281.0036 | -4.078 | 280.343207 | -4.129572 | 281.600756 | 18.920487 | 28.45707071 | -0.21069081 | 265.5303 | 54023.0938888889 | 2006-10-15 02:15:12 | 54025.8141087963 | 2006-10-17 19:32:19 | 500009020 | 98.8583 | 100 | 98.8743 | 98.8663 | 98.8583 | 98.8743 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81.9519 | 81.9519 | 235.0139 | 1 | PROCESSED | 57535.9070023148 | 2016-05-27 21:46:05 | 54697 | 2008-08-19 00:00:00 | 54055.6082407407 | 2006-11-16 14:35:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | KEN EBISAWA | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500009020/ | Quick Look | ![]() |
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754 | MBM12 | 43.9954 | 19.5008 | 43.287121 | 19.299344 | 47.246432 | 2.625648 | 159.17119109 | -34.46234987 | 73.4994 | 55776.7501388889 | 2011-08-03 18:00:12 | 55780.4398263889 | 2011-08-07 10:33:21 | 506026010 | 150.3202 | 150 | 150.3202 | 150.3202 | 0 | 150.3202 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 143.5349 | 143.5349 | 280.7618 | 5 | PROCESSED | 57602.8321180556 | 2016-08-02 19:58:15 | 56169 | 2012-08-30 00:00:00 | 55802.465625 | 2011-08-29 11:10:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060068 | We propose an observation toward dense molecular cloud region MBM12 that is in front of the Local Hot Bubble. Solar wind charge exchange induced emission, reacted with neutrals in the heliosphere (H-SWCX), is considered to have significant influence to the soft diffuse X-ray background under 1 keV. However, there is no significant evidence of the H-SWCX. From this observation, we try to reveal the existence of H-SWCX induced emission by comparing the OVII line emission (0.57 keV) with Suzaku archive data. We also aim to constrain the time variability of H-SWCX emission, depending on the 12 year solar activity. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROSHI YOSHITAKE | JAP | 6 | AO6 | OBSERVATION TOWARD MOLECULAR CLOUD MBM12 : VERIFYING SOLAR WIND CHARGE EXCHANGE EMISSION IN THE HELIOSPHERE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506026010/ | Quick Look | ![]() |
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755 | GRXE_E_9 | 268.0849 | -26.1545 | 267.307554 | -26.143306 | 268.269555 | -2.725006 | 3.15134991 | 0.15632851 | 103.0998 | 56385.8984490741 | 2013-04-03 21:33:46 | 56388.2085648148 | 2013-04-06 05:00:20 | 507074010 | 98.6516 | 100 | 98.6596 | 98.6596 | 0 | 98.6516 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83.0269 | 83.0269 | 199.5757 | 2 | PROCESSED | 57611.012650463 | 2016-08-11 00:18:13 | 56018 | 2012-04-01 00:00:00 | 56401.6405092593 | 2013-04-19 15:22:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507074010/ | Quick Look | ![]() |
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756 | W44_WEST | 283.939 | 1.3216 | 283.304324 | 1.256024 | 285.27764 | 24.025907 | 34.60037354 | -0.35787423 | 254.9999 | 56589.5109953704 | 2013-10-24 12:15:50 | 56590.9655324074 | 2013-10-25 23:10:22 | 508002010 | 61.1078 | 60 | 61.1398 | 61.1078 | 0 | 61.1398 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.4458 | 58.4458 | 125.6678 | 1 | PROCESSED | 57613.10125 | 2016-08-13 02:25:48 | 56970 | 2014-11-09 00:00:00 | 56603.7391087963 | 2013-11-07 17:44:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | HIROYUKI UCHIDA | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508002010/ | Quick Look | ![]() |
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757 | GRXE_E_7 | 268.3325 | -26.1696 | 267.555037 | -26.159608 | 268.492207 | -2.737339 | 3.2513581 | -0.04270444 | 86.7249 | 56716.5321296296 | 2014-02-28 12:46:16 | 56718.7084953704 | 2014-03-02 17:00:14 | 508076010 | 102.6848 | 100 | 102.6978 | 102.6868 | 0 | 102.6848 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.4539 | 96.4539 | 188.0198 | 3 | PROCESSED | 57613.9520486111 | 2016-08-13 22:50:57 | 56383 | 2013-04-01 00:00:00 | 56727.7217013889 | 2014-03-11 17:19:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086001 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKESHI TSURU | JAP | 8 | AO8 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508076010/ | Quick Look | ![]() |
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758 | DIFFUSE1C | 201.9274 | 6.8104 | 201.299196 | 7.069212 | 197.642152 | 14.849246 | 327.54723828 | 67.93166205 | 123.897 | 57015.2219560185 | 2014-12-24 05:19:37 | 57015.3450115741 | 2014-12-24 08:16:49 | 509060010 | 5.5117 | 20 | 5.5277 | 5.5197 | 0 | 5.5117 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5590393518 | 2016-08-17 13:25:01 | 57417 | 2016-01-30 00:00:00 | 57049.4528587963 | 2015-01-27 10:52:07 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | JOEL BREGMAN | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509060010/ | Quick Look | ![]() |
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759 | 73P/SW3 | 317.5094 | 24.3437 | 316.953773 | 24.139336 | 329.181406 | 38.538464 | 71.75290875 | -15.84652301 | 72.7094 | 53868.2758333333 | 2006-05-13 06:37:12 | 53868.3418865741 | 2006-05-13 08:12:19 | 500013030 | 3.225 | 20 | 3.225 | 3.225 | 3.225 | 3.225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2.915 | 2.915 | 5.7039 | 0 | PROCESSED | 57534.2995023148 | 2016-05-26 07:11:17 | 54256 | 2007-06-05 00:00:00 | 54042.2712731482 | 2006-11-03 06:30:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | FREDERICK PORTER | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/500013030/ | Quick Look | ![]() |
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760 | COMET_8P_TUTTLE-P1-1 | 27.7163 | 7.989 | 27.057965 | 7.741803 | 28.591929 | -3.193745 | 147.31647839 | -52.04673223 | 248.4436 | 54470.5233333333 | 2008-01-05 12:33:36 | 54470.5821759259 | 2008-01-05 13:58:20 | 502062010 | 0.6803 | 2 | 0.6803 | 0.6803 | 0 | 0.6803 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 0.632 | 0.632 | 5.08 | 0 | PROCESSED | 57540.9802199074 | 2016-06-01 23:31:31 | 54908 | 2009-03-18 00:00:00 | 54542.4502083333 | 2008-03-17 10:48:18 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | GREGORY BROWN | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/502062010/ | Quick Look | ![]() |
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761 | RIM1 | 311.6421 | 31.883 | 311.130799 | 31.698954 | 326.587321 | 47.481782 | 74.34868893 | -7.06658523 | 247.7276 | 55152.9451273148 | 2009-11-17 22:40:59 | 55153.9488888889 | 2009-11-18 22:46:24 | 504005010 | 40.7473 | 38 | 40.7473 | 40.7473 | 0 | 40.7473 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.5112 | 34.5112 | 86.7159 | 0 | PROCESSED | 57549.4623726852 | 2016-06-10 11:05:49 | 55534 | 2010-12-04 00:00:00 | 55166.4923148148 | 2009-12-01 11:48:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | HIROSHI TSUNEMI | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504005010/ | Quick Look | ![]() |
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762 | SEP #1 | 89.966 | -66.5774 | 89.968235 | -66.57758 | 292.016086 | -89.97915 | 276.40322057 | -29.82494721 | 141.7136 | 55149.1175925926 | 2009-11-14 02:49:20 | 55150.2141087963 | 2009-11-15 05:08:19 | 504069010 | 51.8621 | 50 | 51.8701 | 51.8621 | 0 | 51.8701 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3534 | 48.3534 | 94.7259 | 2 | PROCESSED | 57549.3577546296 | 2016-06-10 08:35:10 | 54922 | 2009-04-01 00:00:00 | 55160.1496296296 | 2009-11-25 03:35:28 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | STEVEN SNOWDEN | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504069010/ | Quick Look | ![]() |
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763 | W28_CENTER | 270.074 | -23.3664 | 269.312952 | -23.364911 | 270.05835 | 0.07446 | 6.46943001 | -0.00256773 | 84.9544 | 55289.3078935185 | 2010-04-03 07:23:22 | 55290.9918287037 | 2010-04-04 23:48:14 | 505005010 | 73.0036 | 70 | 73.0437 | 73.0036 | 0 | 73.0436 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 57.2981 | 57.2981 | 145.4519 | 2 | PROCESSED | 57551.1131944444 | 2016-06-12 02:43:00 | 55287 | 2010-04-01 00:00:00 | 55322.3694675926 | 2010-05-06 08:52:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KATSUJI KOYAMA | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505005010/ | Quick Look | ![]() |
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764 | FERMI_BUBBLE_N7 | 234.5505 | 3.1681 | 233.922592 | 3.3308 | 231.347519 | 21.977572 | 9.28415113 | 43.5333275 | 287.4999 | 56147.9630787037 | 2012-08-08 23:06:50 | 56148.4306944444 | 2012-08-09 10:20:12 | 507007010 | 22.7991 | 20 | 22.8071 | 22.7991 | 0 | 22.8151 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0084 | 21.0084 | 40.3999 | 0 | PROCESSED | 57606.8138541667 | 2016-08-06 19:31:57 | 56536 | 2013-09-01 00:00:00 | 56169.1051388889 | 2012-08-30 02:31:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | JUN KATAOKA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507007010/ | Quick Look | ![]() |
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765 | W49B | 287.7842 | 9.1154 | 287.185843 | 9.031744 | 290.654437 | 31.289753 | 43.28107632 | -0.18330097 | 82.0063 | 57125.7127893518 | 2015-04-13 17:06:25 | 57128.6891087963 | 2015-04-16 16:32:19 | 509001020 | 103.0426 | 400 | 103.0426 | 113.1875 | 0 | 113.1795 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0199537037 | 2016-08-18 00:28:44 | 56748 | 2014-04-01 00:00:00 | 57142.3645138889 | 2015-04-30 08:44:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUJI KOYAMA | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509001020/ | Quick Look | ![]() |
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766 | HOT BLOB 3 | 127.507 | 51.0389 | 126.590865 | 51.206602 | 116.529664 | 30.99487 | 167.88407696 | 36.01101877 | 263.6154 | 57139.1338657407 | 2015-04-27 03:12:46 | 57140.9141319444 | 2015-04-28 21:56:21 | 509009010 | 81.1183 | 80 | 81.1183 | 81.5423 | 0 | 81.5503 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57644.5780902778 | 2016-09-13 13:52:27 | 57591 | 2016-07-22 00:00:00 | 57224.4589351852 | 2015-07-21 11:00:52 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090044 | Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size. | GALACTIC DIFFUSE EMISSION | 5 | C | NORIO SEKIYA | JAP | 9 | AO9 | ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509009010/ | Quick Look | ![]() |
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