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
|
center_ra_b1950
|
center_dec_b1950
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center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
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exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
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xis3_exposure
|
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
|
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
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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 | ||
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/ |