DARTS Astro

total 766

No.
target_name
center_ra
center_dec
center_ra_b1950
center_dec_b1950
center_ecliptic_lon
center_ecliptic_lat
center_galactic_lon
center_galactic_lat
roll_angle
observation_start_time_mjd
observation_start_time
observation_end_time_mjd
observation_end_time
observation_id
exposure
proposal_exposure
xis0_exposure
xis1_exposure
xis2_exposure
xis3_exposure
xis0_observation_mode
xis1_observation_mode
xis2_observation_mode
xis3_observation_mode
hxd_observation_mode
hxd_coarse_clock_rate_exposure
hxd_first_clock_rate_exposure
hxd_normal_clock_rate_exposure
hxd_all_clock_rate_exposure
hxd_wam_exposure
hxd_burst_num
processing_status
processing_end_time_mjd
processing_end_time
public_date_mjd
public_date
distribute_start_date_mjd
distribute_start_date
processing_version
processing_quantity
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle_count
observation_type
proposal_title
main_detector
xis_injection_flag
data_access_url
ql_access_url
ql_image_url
1 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