DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 858
No. |
object_name
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center_ra
|
center_dec
|
center_ra_b1950
|
center_dec_b1950
|
center_ecliptic_lon
|
center_ecliptic_lat
|
center_galactic_lon
|
center_galactic_lat
|
roll_angle
|
observation_start_time_mjd
|
observation_start_time
|
observation_end_time_mjd
|
observation_end_time
|
observation_id
|
exposure
|
awarded_exposure
|
xis0_exposure
|
xis1_exposure
|
xis2_exposure
|
xis3_exposure
|
xis0_observation_mode
|
xis1_observation_mode
|
xis2_observation_mode
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xis3_observation_mode
|
hxd_observation_mode
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hxd_coarse_clock_rate_exposure
|
hxd_first_clock_rate_exposure
|
hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
|
hxd_wam_exposure
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
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proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
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1 | ABELL 773 | 139.3092 | 51.8461 | 138.434684 | 52.055757 | 124.471508 | 34.139728 | 165.95348434 | 43.2527698 | 276.9988 | 55684.9096412037 | 2011-05-03 21:49:53 | 55685.7363541667 | 2011-05-04 17:40:21 | 806027040 | 49.8691 | 50 | 49.8805 | 49.8771 | 0 | 49.8691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1285 | 44.1285 | 71.422 | 1 | PROCESSED | 57601.942962963 | 2016-08-01 22:37:52 | 55652 | 2011-04-01 00:00:00 | 55697.3061458333 | 2011-05-16 07:20:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806027040/ | Quick Look | ||
2 | COMA CLUSTER OFFSET | 194.6939 | 27.9466 | 194.090146 | 28.216217 | 181.281218 | 31.269541 | 60.06105128 | 88.1791818 | 318.0815 | 53885.0996412037 | 2006-05-30 02:23:29 | 53886.8384722222 | 2006-05-31 20:07:24 | 801044010 | 79.172 | 80 | 79.172 | 79.172 | 79.172 | 79.172 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.2282 | 75.2282 | 150.2049 | 2 | PROCESSED | 57534.5195949074 | 2016-05-26 12:28:13 | 54394 | 2007-10-21 00:00:00 | 53926.7587384259 | 2006-07-10 18:12:35 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010091 | In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801044010/ | Quick Look | ||
3 | HYDRA A-2 | 139.672 | -11.9467 | 139.069416 | -11.735403 | 146.240414 | -26.215979 | 242.89463155 | 25.29884455 | 94.9986 | 55509.1804861111 | 2010-11-09 04:19:54 | 55510.3008680556 | 2010-11-10 07:13:15 | 805008010 | 41.8231 | 40 | 41.8311 | 41.8231 | 0 | 41.8311 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.5896 | 34.5896 | 96.7898 | 2 | PROCESSED | 57554.050162037 | 2016-06-15 01:12:14 | 55890 | 2011-11-25 00:00:00 | 55524.1344791667 | 2010-11-24 03:13:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050012 | X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 5 | AO5 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805008010/ | Quick Look | ||
4 | COMA SUBHALO2 | 194.5069 | 27.3689 | 193.901795 | 27.638743 | 181.411119 | 30.679028 | 42.63932899 | 88.51577103 | 315.0001 | 56452.5504976852 | 2013-06-09 13:12:43 | 56453.0265046296 | 2013-06-10 00:38:10 | 808020010 | 21.1563 | 20 | 21.1563 | 21.1563 | 0 | 21.1563 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.608 | 17.608 | 41.1199 | 1 | PROCESSED | 57611.5058564815 | 2016-08-11 12:08:26 | 56872 | 2014-08-03 00:00:00 | 56506.7547222222 | 2013-08-02 18:06:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808020010/ | Quick Look | ||
5 | A3376 NORTH | 90.6541 | -39.7108 | 90.244762 | -39.708634 | 91.122885 | -63.149983 | 246.26196714 | -25.85404299 | 80.8001 | 56553.3109143518 | 2013-09-18 07:27:43 | 56554.8453935185 | 2013-09-19 20:17:22 | 808029010 | 57.6912 | 57 | 57.6912 | 57.6992 | 0 | 57.7072 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.8185 | 50.8185 | 132.57 | 0 | PROCESSED | 57612.703275463 | 2016-08-12 16:52:43 | 56956 | 2014-10-26 00:00:00 | 56588.7436689815 | 2013-10-23 17:50:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808029010/ | Quick Look | ||
6 | A1689-OFFSET3 | 197.7048 | -1.4241 | 197.062246 | -1.158416 | 196.866357 | 5.631394 | 312.98436439 | 61.06880263 | 289.9992 | 54672.423599537 | 2008-07-25 10:09:59 | 54673.474525463 | 2008-07-26 11:23:19 | 803026010 | 44.0942 | 40 | 44.0942 | 44.0942 | 0 | 44.0942 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7063 | 37.7063 | 90.7878 | 1 | PROCESSED | 57543.149537037 | 2016-06-04 03:35:20 | 55076 | 2009-09-02 00:00:00 | 54707.1173263889 | 2008-08-29 02:48:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803026010/ | Quick Look | ||
7 | NGC 5044 OFFSET1 | 198.8505 | -16.143 | 198.184446 | -15.87899 | 203.499232 | -7.562902 | 311.28196707 | 46.33985641 | 290.0004 | 53919.3604398148 | 2006-07-03 08:39:02 | 53920.9599305556 | 2006-07-04 23:02:18 | 801047010 | 54.6204 | 60 | 54.6204 | 54.6204 | 54.6204 | 54.6204 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45.8033 | 45.8033 | 138.1899 | 1 | PROCESSED | 57534.8941203704 | 2016-05-26 21:27:32 | 54394 | 2007-10-21 00:00:00 | 53942.4615740741 | 2006-07-26 11:04:40 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801047010/ | Quick Look | ||
8 | ABELL1835 OFFSET2 | 210.2863 | 2.6798 | 209.652404 | 2.920968 | 207.209815 | 14.079845 | 340.21334307 | 60.40388756 | 306.816 | 55384.1224884259 | 2010-07-07 02:56:23 | 55385.4667939815 | 2010-07-08 11:12:11 | 805038010 | 45.6036 | 50 | 45.6036 | 45.6276 | 0 | 45.6116 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2826 | 41.2826 | 116.1298 | 0 | PROCESSED | 57552.5623611111 | 2016-06-13 13:29:48 | 55801 | 2011-08-28 00:00:00 | 55434.3364930556 | 2010-08-26 08:04:33 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NOBUHIRO OKABE | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805038010/ | Quick Look | ||
9 | NGC 253 | 11.9272 | -25.3509 | 11.313264 | -25.623648 | 0.061683 | -27.85028 | 97.52826827 | -88.03578801 | 242.9951 | 56643.3716203704 | 2013-12-17 08:55:08 | 56645.502962963 | 2013-12-19 12:04:16 | 808053010 | 99.6864 | 100 | 99.6864 | 99.6864 | 0 | 99.6864 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.5642 | 98.5642 | 184.1038 | 0 | PROCESSED | 57613.6331481482 | 2016-08-13 15:11:44 | 57031 | 2015-01-09 00:00:00 | 56664.7662962963 | 2014-01-07 18:23:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080070 | We propose the observation of edge-on starburst galaxies NGC253 and NGC 2146 for 150 ks and 100 ks, respectively. One of the mechanisms that promote the chemical evolution of the universe, starburst outflows have been studied from both aspects of multi-wavelength observations and theory so far. Suzaku original attempts focusing on the abundance patterns has given new insights for a starburst-driven outflow scenario. In AO8, we try to extract the abundance pattern from the south region in NGC 253 and the central region in NGC 2146. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOSHIKI SATO | JAP | 8 | AO8 | OBSERVATION OF EDGE-ON STARBURST GALAXIES NGC 253 & NGC 2146 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808053010/ | Quick Look | ||
10 | A2163SE | 244.1024 | -6.3096 | 243.434314 | -6.186546 | 243.31547 | 14.764116 | 6.72311865 | 30.24259241 | 94.6291 | 57074.4179282407 | 2015-02-21 10:01:49 | 57075.8002662037 | 2015-02-22 19:12:23 | 809009010 | 43.2945 | 50 | 43.2945 | 51.0623 | 0 | 51.0943 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6399421296 | 2016-08-17 15:21:31 | 57453 | 2016-03-06 00:00:00 | 57087.4694212963 | 2015-03-06 11:15:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809009010/ | Quick Look | ||
11 | RBS1066 | 181.3063 | 39.3578 | 180.66961 | 39.636099 | 163.015077 | 36.071469 | 158.19944471 | 74.44309108 | 133.5252 | 56973.6795486111 | 2014-11-12 16:18:33 | 56973.8890277778 | 2014-11-12 21:20:12 | 809105010 | 10.2376 | 12 | 10.2376 | 10.5256 | 0 | 10.5256 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7665509259 | 2016-08-16 18:23:50 | 57358 | 2015-12-02 00:00:00 | 56992.4200810185 | 2014-12-01 10:04:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LORENZO LOVISARI | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809105010/ | Quick Look | ||
12 | M82 N2 | 148.2738 | 70.273 | 147.216273 | 70.508377 | 118.122269 | 52.466944 | 140.95732372 | 40.02876632 | 282.8972 | 57162.9827546296 | 2015-05-20 23:35:10 | 57164.434224537 | 2015-05-22 10:25:17 | 810043010 | 59.8084 | 60 | 59.8084 | 61.9021 | 0 | 61.9021 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 34.13 | 0 | PROCESSED | 57618.7218287037 | 2016-08-18 17:19:26 | 57548 | 2016-06-09 00:00:00 | 57177.3762847222 | 2015-06-04 09:01:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101442 | We propose to carry out Suzaku observations of the starburst galaxy M82. We will search for X-ray emission from winds and shock heated clouds out to its possible outer boundary of ~45 kpc. We will also constrain the density and temperature profiles of the gas/wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, shocked clouds in a wind, etc. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 10 | AO10 | SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810043010/ | Quick Look | ||
13 | ZWCL0008.8+5215 WEST | 2.7765 | 52.5416 | 2.120361 | 52.263518 | 29.435357 | 45.775484 | 116.7279282 | -9.84363991 | 63.9984 | 56847.5889351852 | 2014-07-09 14:08:04 | 56849.9925115741 | 2014-07-11 23:49:13 | 809117010 | 102.3736 | 100 | 102.3816 | 102.3736 | 0 | 102.3896 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3796643518 | 2016-08-15 09:06:43 | 56748 | 2014-04-01 00:00:00 | 56861.6478703704 | 2014-07-23 15:32:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROKI AKAMATSU | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809117010/ | Quick Look | ||
14 | A1914_OFFSET4 | 216.4138 | 37.6152 | 215.900162 | 37.839927 | 196.47734 | 48.33006 | 66.75628519 | 67.60183749 | 330.9949 | 55365.2958333333 | 2010-06-18 07:06:00 | 55366.115462963 | 2010-06-19 02:46:16 | 805094010 | 27.2904 | 40 | 27.2904 | 27.3001 | 0 | 27.2944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.4203 | 25.4203 | 70.816 | 0 | PROCESSED | 57552.407037037 | 2016-06-13 09:46:08 | 55769 | 2011-07-27 00:00:00 | 55403.4672106482 | 2010-07-26 11:12:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADOKA KAWAHARADA | ERIC MILLER | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805094010/ | Quick Look | |
15 | A1831 | 209.8007 | 27.9693 | 209.233208 | 28.211522 | 195.74505 | 37.218341 | 40.05378223 | 74.96810077 | 288.1207 | 53937.1181828704 | 2006-07-21 02:50:11 | 53937.5106481482 | 2006-07-21 12:15:20 | 801077010 | 18.0796 | 18 | 18.0796 | 18.0796 | 18.0796 | 18.0796 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.0891 | 17.0891 | 33.8979 | 1 | PROCESSED | 57535.0011805556 | 2016-05-27 00:01:42 | 54401 | 2007-10-28 00:00:00 | 53943.553599537 | 2006-07-27 13:17:11 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801077010/ | Quick Look | ||
16 | A1750S | 202.5548 | -2.1063 | 201.910476 | -1.848597 | 201.643103 | 6.819901 | 322.18359807 | 59.30814244 | 293.521 | 55751.0328009259 | 2011-07-09 00:47:14 | 55753.0002314815 | 2011-07-11 00:00:20 | 806097010 | 80.1668 | 80 | 80.1668 | 80.1668 | 0 | 80.1668 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.0448 | 67.0448 | 169.9618 | 3 | PROCESSED | 57602.5725578704 | 2016-08-02 13:44:29 | 56148 | 2012-08-09 00:00:00 | 55778.4321412037 | 2011-08-05 10:22:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 063019 | We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADOKA KAWAHARADA | SCOTT RANDALL | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806097010/ | Quick Look | |
17 | A1914_OFFSET1 | 216.5507 | 38.0175 | 216.039339 | 38.24183 | 196.32687 | 48.734523 | 67.63121502 | 67.35438204 | 324.9943 | 55362.5248148148 | 2010-06-15 12:35:44 | 55363.4724768518 | 2010-06-16 11:20:22 | 805091010 | 32.2034 | 40 | 32.2034 | 32.2034 | 0 | 32.2034 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.5086 | 27.5086 | 81.876 | 1 | PROCESSED | 57552.3572569445 | 2016-06-13 08:34:27 | 55766 | 2011-07-24 00:00:00 | 55399.2609722222 | 2010-07-22 06:15:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADOKA KAWAHARADA | ERIC MILLER | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805091010/ | Quick Look | |
18 | 1RXJ0603 | 90.7832 | 42.2686 | 89.889602 | 42.270241 | 90.61448 | 18.829705 | 170.16927881 | 9.72454424 | 80.0992 | 56207.7131828704 | 2012-10-07 17:06:59 | 56210.6307986111 | 2012-10-10 15:08:21 | 807001010 | 124.3416 | 120 | 124.3511 | 124.3439 | 0 | 124.3416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 125.1948 | 125.1948 | 252.0559 | 1 | PROCESSED | 57607.7803009259 | 2016-08-07 18:43:38 | 56595 | 2013-10-30 00:00:00 | 56226.6645717593 | 2012-10-26 15:56:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070025 | We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HIROKI AKAMATSU | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807001010/ | Quick Look | ||
19 | A1674 | 195.9676 | 67.5471 | 195.510877 | 67.814977 | 143.551001 | 62.83408 | 121.10331631 | 49.53698634 | 114.9985 | 54085.1434837963 | 2006-12-16 03:26:37 | 54087.0426388889 | 2006-12-18 01:01:24 | 801062010 | 68.4138 | 100 | 68.4218 | 68.4218 | 0 | 68.4138 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109.0131 | 109.0131 | 164.064 | 2 | PROCESSED | 57536.3777546296 | 2016-05-28 09:03:58 | 54750 | 2008-10-11 00:00:00 | 54094.6003935185 | 2006-12-25 14:24:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010156 | A1674 is a nearby (z=0.106) richness class 3 clsuter with Abell galaxy count of 165, while its X-ray luminsity is as low as 6e43erg/s. We have observed this cluster with ASCA and XMM-Newton, and found iregular extended X-ray emission. The X-ray spectrum can be fitted with a thin thermal model of kT ~ 3keV, but the metal abundance is 0.07 with upper limit of 0.2. We assume this cluster may be a cluster under construction. Utilizing the low background level and high sensitivity of Suzaku XIS, we aim to obtain accurate X-ray spectrum of this cluster to constrain the metal abndance of each species. We also examine possible contribution of diffuse non-thermal emission in cluster scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801062010/ | Quick Look | ||
20 | FORNAX A W-LOBE W | 50.2219 | -37.0341 | 49.742698 | -37.213173 | 32.331063 | -52.814253 | 239.92107074 | -57.06786371 | 27.0759 | 54990.6810763889 | 2009-06-08 16:20:45 | 54991.75375 | 2009-06-09 18:05:24 | 804036010 | 60.3625 | 50 | 60.3625 | 60.3625 | 0 | 60.3625 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.3965 | 56.3965 | 92.6519 | 1 | PROCESSED | 57547.532974537 | 2016-06-08 12:47:29 | 55367 | 2010-06-20 00:00:00 | 55001.0562615741 | 2009-06-19 01:21:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MAKOTO TASHIRO | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804036010/ | Quick Look | ||
21 | COMA_45OFF | 194.2558 | 27.5714 | 193.650381 | 27.84154 | 181.073902 | 30.760176 | 52.91406039 | 88.6829823 | 127.9482 | 54436.4228703704 | 2007-12-02 10:08:56 | 54437.2085185185 | 2007-12-03 05:00:16 | 802047010 | 31.6151 | 30 | 31.6151 | 31.6151 | 0 | 31.6151 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.1691 | 26.1691 | 67.824 | 0 | PROCESSED | 57540.7702083333 | 2016-06-01 18:29:06 | 54814 | 2008-12-14 00:00:00 | 54445.1600925926 | 2007-12-11 03:50:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020149 | With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SUSUMU INOUE | JAP | 2 | AO2 | EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802047010/ | Quick Look | ||
22 | VIRGO W12 | 184.4921 | 10.4589 | 183.855234 | 10.736542 | 179.90666 | 11.371427 | 276.03236295 | 71.56080365 | 100 | 56277.5402546296 | 2012-12-16 12:57:58 | 56278.125150463 | 2012-12-17 03:00:13 | 807105010 | 27.0915 | 24 | 27.0995 | 27.0915 | 0 | 27.0995 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.8528 | 26.8528 | 50.488 | 1 | PROCESSED | 57608.2964930556 | 2016-08-08 07:06:57 | 56018 | 2012-04-01 00:00:00 | 56344.6765162037 | 2013-02-21 16:14:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807105010/ | Quick Look | ||
23 | A1800 | 207.3618 | 28.0973 | 206.789109 | 28.345144 | 193.256107 | 36.394356 | 40.59651819 | 77.12066844 | 302.3644 | 53936.635625 | 2006-07-20 15:15:18 | 53937.1140509259 | 2006-07-21 02:44:14 | 801078010 | 20.0437 | 17 | 20.0473 | 20.0553 | 20.0553 | 20.0437 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.0003 | 19.0003 | 41.3319 | 0 | PROCESSED | 57535.0036458333 | 2016-05-27 00:05:15 | 54401 | 2007-10-28 00:00:00 | 53943.5299652778 | 2006-07-27 12:43:09 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801078010/ | Quick Look | ||
24 | AWM7 NW2 | 42.4678 | 42.1132 | 41.659195 | 41.906559 | 53.004907 | 24.584739 | 145.29354682 | -15.55850289 | 257.0018 | 56705.8674421296 | 2014-02-17 20:49:07 | 56706.6667824074 | 2014-02-18 16:00:10 | 808024010 | 35.333 | 35 | 35.341 | 35.333 | 0 | 35.349 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.0596 | 30.0596 | 69.0559 | 0 | PROCESSED | 57613.8687268518 | 2016-08-13 20:50:58 | 57130 | 2015-04-18 00:00:00 | 56764.8062847222 | 2014-04-17 19:21:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808024010/ | Quick Look | ||
25 | URSA MINOR | 227.2517 | 67.2307 | 227.099638 | 67.419875 | 158.023499 | 73.538029 | 104.9865755 | 44.80382561 | 40.7921 | 54195.7731944444 | 2007-04-05 18:33:24 | 54196.7557175926 | 2007-04-06 18:08:14 | 802052010 | 70.8823 | 67 | 70.8903 | 70.8823 | 0 | 70.8903 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.5872 | 59.5872 | 84.876 | 1 | PROCESSED | 57538.0737731482 | 2016-05-30 01:46:14 | 54695 | 2008-08-17 00:00:00 | 54203.3200462963 | 2007-04-13 07:40:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021405 | We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MICHAEL LOEWENSTEIN | USA | 2 | AO2 | SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802052010/ | Quick Look | ||
26 | BOOTES GROUP 1 | 218.7136 | 35.7235 | 218.197903 | 35.941461 | 200.235171 | 47.529275 | 60.71261374 | 66.41229506 | 153.2269 | 54440.1222106482 | 2007-12-06 02:55:59 | 54441.2015972222 | 2007-12-07 04:50:18 | 802054010 | 42.2242 | 38 | 42.2242 | 42.2242 | 0 | 42.2242 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.3023 | 41.3023 | 93.254 | 0 | PROCESSED | 57540.8293518518 | 2016-06-01 19:54:16 | 54815 | 2008-12-15 00:00:00 | 54448.2273842593 | 2007-12-14 05:27:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802054010/ | Quick Look | ||
27 | ABELL2244 | 255.6885 | 34.0502 | 255.230084 | 34.120069 | 248.255538 | 56.413781 | 56.77689495 | 36.30222985 | 232.8204 | 54392.7992013889 | 2007-10-19 19:10:51 | 54394.3959953704 | 2007-10-21 09:30:14 | 802078010 | 71.3811 | 63 | 71.3891 | 71.3971 | 0 | 71.3811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.1077 | 69.1077 | 137.9498 | 3 | PROCESSED | 57540.332337963 | 2016-06-01 07:58:34 | 54771 | 2008-11-01 00:00:00 | 54403.2516666667 | 2007-10-30 06:02:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022036 | In order to use clusters as cosmological probes, accurate mass determinations are needed. The ICM is an ideal candidate since it provides a map of the DM potential. Measuring the gas properties to the virial radius is imperative for determining the proper cluster mass, since a large part of the cluster mass resides beyond 1/2 r_vir. Current discrepancies in outer cluster kT profiles are due to large uncertainties due to the high background in Chandra and XMM-Newton. With its lower background, Suzaku is able to make this measurement. We propose a 50 ks observation of A2244. A2244 is an ideal candidate to make this measurement; at a redshift of z~0.1, the virial radius can be fit inside Suzaku's field of view, moreover A2244 is an unusual example of a relaxed cluster without a cool core. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DANIEL HUDSON | EUR | 2 | AO2 | A2244 - MEASURING CLUSTER GAS TEMPERATURE TO THE VIRIAL RADIUS IN A RELAXED ISOTHERMAL CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802078010/ | Quick Look | ||
28 | A2665 | 357.7161 | 6.1352 | 357.076736 | 5.857083 | 0.350497 | 6.536022 | 96.94047732 | -53.65177278 | 245.9817 | 54078.2252893518 | 2006-12-09 05:24:25 | 54078.562037037 | 2006-12-09 13:29:20 | 801076010 | 13.944 | 15 | 13.944 | 13.944 | 0 | 13.944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.6073 | 11.6073 | 29.0879 | 0 | PROCESSED | 57536.2715393518 | 2016-05-28 06:31:01 | 54695 | 2008-08-17 00:00:00 | 54089.271412037 | 2006-12-20 06:30:50 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801076010/ | Quick Look | ||
29 | FJ1 | 238.114 | 22.5674 | 237.571568 | 22.715547 | 229.271734 | 41.603316 | 36.86878642 | 48.89749971 | 115.0005 | 56698.0557638889 | 2014-02-10 01:20:18 | 56701.0001851852 | 2014-02-13 00:00:16 | 808041010 | 111.8457 | 100 | 111.8537 | 111.8457 | 0 | 111.8537 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8229166667 | 2016-08-13 19:45:00 | 57130 | 2015-04-18 00:00:00 | 56765.6012152778 | 2014-04-18 14:25:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080054 | Filament Junctions are known to be the most active regions in structure formation in the Universe. These regions can be identified using our original method based on galaxy distribution. In AO8, we try to detect (1) a galaxy-scale halo with a radio relic structure often observed after merger and (2) a galaxy-scale halo just before merger at the Filament Junction. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IKUYUKI MITSUISHI | JAP | 8 | AO8 | EXPLORING EVOLUTION OF GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808041010/ | Quick Look | ||
30 | A1689-OFFSET4 | 197.7965 | -1.1735 | 197.154302 | -0.90795 | 196.855647 | 5.897997 | 313.25406527 | 61.301843 | 290 | 54673.475 | 2008-07-26 11:24:00 | 54674.5091898148 | 2008-07-27 12:13:14 | 803027010 | 42.0199 | 40 | 42.0279 | 42.0279 | 0 | 42.0199 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.8505 | 36.8505 | 89.354 | 2 | PROCESSED | 57543.1496527778 | 2016-06-04 03:35:30 | 55076 | 2009-09-02 00:00:00 | 54707.0673032407 | 2008-08-29 01:36:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803027010/ | Quick Look | ||
31 | A3112 | 49.3542 | -44.4494 | 48.920816 | -44.631605 | 25.154749 | -59.092558 | 253.34888003 | -56.10584592 | 209.0003 | 57003.8439467593 | 2014-12-12 20:15:17 | 57006.6182407407 | 2014-12-15 14:50:16 | 809116020 | 97.989 | 200 | 97.989 | 97.989 | 0 | 97.989 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5061458333 | 2016-08-17 12:08:51 | 57387 | 2015-12-31 00:00:00 | 57017.4238425926 | 2014-12-26 10:10:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 094527 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ESRA BULBUL | USJ | 9 | AO9 | A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809116020/ | Quick Look | ||
32 | ABELL2255_RELIC | 258.3088 | 64.2709 | 258.23432 | 64.327456 | 199.782032 | 84.629727 | 94.17355304 | 34.84143708 | 3.193 | 56810.1311458333 | 2014-06-02 03:08:51 | 56812.4147569444 | 2014-06-04 09:57:15 | 809121010 | 100.6045 | 100 | 100.6045 | 100.8125 | 0 | 100.8045 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1987731482 | 2016-08-15 04:46:14 | 56748 | 2014-04-01 00:00:00 | 56867.7458217593 | 2014-07-29 17:53:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROKI AKAMATSU | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809121010/ | Quick Look | ||
33 | FILAMENT OF GALAXIES | 238.2847 | 27.6247 | 237.767937 | 27.772087 | 227.420415 | 46.484967 | 44.49442625 | 49.89393343 | 305.997 | 55408.8620833333 | 2010-07-31 20:41:24 | 55410.6883101852 | 2010-08-02 16:31:10 | 805030010 | 61.7703 | 80 | 61.7703 | 61.7703 | 0 | 61.7703 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.5833 | 55.5833 | 157.7518 | 0 | PROCESSED | 57552.8205671296 | 2016-06-13 19:41:37 | 55793 | 2011-08-20 00:00:00 | 55427.2133449074 | 2010-08-19 05:07:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050032 | Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAJIME KAWAHARA | JAP | 5 | AO5 | SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805030010/ | Quick Look | ||
34 | A2199 OFFSET6 | 247.2752 | 38.7861 | 246.840866 | 38.894582 | 233.723395 | 59.394916 | 61.88224995 | 43.57632899 | 299.9992 | 55792.1844212963 | 2011-08-19 04:25:34 | 55792.9321875 | 2011-08-19 22:22:21 | 806152010 | 29.7851 | 30 | 29.7851 | 29.7851 | 0 | 29.7851 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.2105 | 22.2105 | 64.5979 | 1 | PROCESSED | 57602.8830324074 | 2016-08-02 21:11:34 | 55652 | 2011-04-01 00:00:00 | 55806.2639467593 | 2011-09-02 06:20:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806152010/ | Quick Look | |
35 | CENA LOBE 2 | 201.7888 | -39.7615 | 201.063878 | -39.502282 | 215.867885 | -28.246306 | 310.35736359 | 22.59471631 | 296.9216 | 56141.4611921296 | 2012-08-02 11:04:07 | 56143.2779861111 | 2012-08-04 06:40:18 | 807041030 | 65.8666 | 65 | 65.8746 | 65.8746 | 0 | 65.8666 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.8659 | 57.8659 | 156.9538 | 2 | PROCESSED | 57606.7677893518 | 2016-08-06 18:25:37 | 56018 | 2012-04-01 00:00:00 | 56162.2467013889 | 2012-08-23 05:55:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807041030/ | Quick Look | ||
36 | COMA SUBHALO1 S | 195.2527 | 28.7629 | 194.651674 | 29.031827 | 181.36326 | 32.219878 | 71.19878606 | 87.32773157 | 296.8003 | 56452.0686458333 | 2013-06-09 01:38:51 | 56452.5459490741 | 2013-06-09 13:06:10 | 808019010 | 20.4808 | 20 | 20.4888 | 20.4808 | 0 | 20.4968 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.4968 | 21.4968 | 41.2319 | 0 | PROCESSED | 57611.4938541667 | 2016-08-11 11:51:09 | 56869 | 2014-07-31 00:00:00 | 56503.6109606482 | 2013-07-30 14:39:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808019010/ | Quick Look | ||
37 | A3376 SOUTH | 90.6172 | -40.196 | 90.211877 | -40.194003 | 91.07062 | -63.635447 | 246.775776 | -26.0046965 | 124.8629 | 56580.8395486111 | 2013-10-15 20:08:57 | 56582.2918055556 | 2013-10-17 07:00:12 | 808030010 | 66.5346 | 57 | 66.5347 | 66.5346 | 0 | 66.5346 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 56.9771 | 56.9771 | 125.45 | 1 | PROCESSED | 57613.0188541667 | 2016-08-13 00:27:09 | 57004 | 2014-12-13 00:00:00 | 56637.6639351852 | 2013-12-11 15:56:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808030010/ | Quick Look | ||
38 | ABELL 3571 | 206.8624 | -32.8524 | 206.14186 | -32.603207 | 216.960537 | -20.284209 | 316.31343933 | 28.55973438 | 103.8412 | 56666.0275 | 2014-01-09 00:39:36 | 56666.7772453704 | 2014-01-09 18:39:14 | 808094010 | 38.279 | 60 | 38.279 | 38.279 | 0 | 38.279 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.0047 | 39.0047 | 64.776 | 0 | PROCESSED | 57613.7763425926 | 2016-08-13 18:37:56 | 57096 | 2015-03-15 00:00:00 | 56730.4916435185 | 2014-03-14 11:47:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081531 | Abell 3571 is one of the brightest cluster in the X-ray sky and one of the main clusters in the Shapley supercluster. We have recently found evidence that it may be passing through a violent (~2000 km/s) merger in the line of sight (los). If corroborated it would be the closest template for the systems of this kind allowing us to study and characterize los mergers. We request a short observation of 60 ksec to corroborate the velocity gradients found with Chandra for this cluster, using the improved spectral resolution and gain stability of Suzaku s XISs. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RENATO DUPKE | USA | 8 | AO8 | ABELL 3571. THE CLOSEST LINE OF SIGHT MERGER? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808094010/ | Quick Look | ||
39 | A262 E3 | 29.2513 | 35.7586 | 28.51426 | 35.514871 | 40.102333 | 22.236821 | 137.59731231 | -25.23895106 | 250.0003 | 56701.0116319444 | 2014-02-13 00:16:45 | 56701.8717939815 | 2014-02-13 20:55:23 | 808114010 | 38.5681 | 40 | 38.5761 | 38.5681 | 0 | 38.5761 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8129861111 | 2016-08-13 19:30:42 | 57080 | 2015-02-27 00:00:00 | 56714.7407986111 | 2014-02-26 17:46:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | NORBERT WERNER | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808114010/ | Quick Look | |
40 | A2163BGD1 | 244.2972 | -6.0675 | 243.630135 | -5.945298 | 243.467732 | 15.036983 | 7.08170195 | 30.23063611 | 97.9997 | 57078.1207523148 | 2015-02-25 02:53:53 | 57078.9737384259 | 2015-02-25 23:22:11 | 809010010 | 28.6539 | 30 | 28.6539 | 28.6619 | 0 | 28.6699 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6666782407 | 2016-08-17 16:00:01 | 57454 | 2016-03-07 00:00:00 | 57087.4740393518 | 2015-03-06 11:22:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809010010/ | Quick Look | ||
41 | PKS 2356-61 | 359.7661 | -60.908 | 359.120501 | -61.186478 | 324.284485 | -53.222548 | 314.02525269 | -55.07790138 | 249.6445 | 54075.7140740741 | 2006-12-06 17:08:16 | 54078.21625 | 2006-12-09 05:11:24 | 801016010 | 100.8372 | 100 | 100.8452 | 100.8372 | 0 | 100.8532 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.1255 | 92.1255 | 216.1579 | 3 | PROCESSED | 57536.3143171296 | 2016-05-28 07:32:37 | 54456 | 2007-12-22 00:00:00 | 54088.6546759259 | 2006-12-19 15:42:44 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010059 | We propose a 100 ksec Suzaku observation of the radio galaxy PKS 2356-61. PKS 2356-61 is reported to reside in a group of galaxies, and a sign of a diffuse X-ray emission with a possibly high temperature surrounding PKS 2356-61 was suggested with ASCA. Our objective is the determination of the origin of the diffuse emission to evaluate AGN heating of the intragroup gas by PKS 2356-61. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SOOJING HONG | JAP | 1 | AO1 | HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801016010/ | Quick Look | ||
42 | A3376 WEST RELIC | 90.0363 | -39.9917 | 89.629297 | -39.992531 | 90.071049 | -63.433501 | 246.43145562 | -26.38385089 | 126.3601 | 54034.3950231482 | 2006-10-26 09:28:50 | 54035.9176388889 | 2006-10-27 22:01:24 | 800011020 | 62.2648 | 60 | 62.2648 | 62.2648 | 62.2648 | 62.2648 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55.5629 | 55.5629 | 131.5378 | 2 | PROCESSED | 57535.9705902778 | 2016-05-27 23:17:39 | 54694 | 2008-08-16 00:00:00 | 54090.2671643518 | 2006-12-21 06:24:43 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001039 | We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 0 | SWG | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011020/ | Quick Look | ||
43 | HYDRA A-1 | 139.3695 | -11.9475 | 138.767154 | -11.737163 | 145.930071 | -26.316597 | 242.69436566 | 25.06487811 | 95 | 55508.1097569444 | 2010-11-08 02:38:03 | 55509.1800115741 | 2010-11-09 04:19:13 | 805007010 | 42.5647 | 40 | 42.5727 | 42.5647 | 0 | 42.5727 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.2072 | 35.2072 | 92.4558 | 1 | PROCESSED | 57554.0434143518 | 2016-06-15 01:02:31 | 55890 | 2011-11-25 00:00:00 | 55524.1752430556 | 2010-11-24 04:12:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050012 | X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 5 | AO5 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805007010/ | Quick Look | ||
44 | FILAMENT JUNCTION 3 | 151.4159 | 39.7399 | 150.662748 | 39.98344 | 138.765722 | 26.114357 | 181.90509124 | 53.56333781 | 291.576 | 55672.3023611111 | 2011-04-21 07:15:24 | 55673.6362268518 | 2011-04-22 15:16:10 | 806005010 | 55.0232 | 60 | 55.0232 | 55.0312 | 0 | 55.0392 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.8669 | 49.8669 | 115.2299 | 2 | PROCESSED | 57601.5861921296 | 2016-08-01 14:04:07 | 56061 | 2012-05-14 00:00:00 | 55692.3338425926 | 2011-05-11 08:00:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806005010/ | Quick Look | ||
45 | NGC 2300 GROUP | 112.8158 | 85.6965 | 108.675805 | 85.795148 | 93.626997 | 62.54508 | 127.72434362 | 27.79082708 | 339.9138 | 55235.7626388889 | 2010-02-08 18:18:12 | 55236.5002893518 | 2010-02-09 12:00:25 | 804030010 | 37.0591 | 100 | 37.0591 | 37.0591 | 0 | 37.0591 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.4534 | 34.4534 | 63.7299 | 1 | PROCESSED | 57550.5366666667 | 2016-06-11 12:52:48 | 55619 | 2011-02-27 00:00:00 | 55251.1588310185 | 2010-02-24 03:48:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804030010/ | Quick Look | ||
46 | RCS212414-6325.8 | 321.0509 | -63.4275 | 320.054735 | -63.642547 | 299.532953 | -45.130077 | 330.62476764 | -40.84164156 | 79.2319 | 55691.4113541667 | 2011-05-10 09:52:21 | 55691.979375 | 2011-05-10 23:30:18 | 806082010 | 36.3224 | 35 | 36.3304 | 36.3304 | 0 | 36.3224 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.914 | 26.914 | 49.0679 | 1 | PROCESSED | 57602.0065046296 | 2016-08-02 00:09:22 | 56068 | 2012-05-21 00:00:00 | 55701.1927546296 | 2011-05-20 04:37:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806082010/ | Quick Look | ||
47 | ABELL 1795 Far North | 207.223 | 26.9995 | 206.646903 | 27.247656 | 193.71055 | 35.352954 | 35.63943573 | 77.21561208 | 130.4264 | 53715.3208796296 | 2005-12-11 07:42:04 | 53715.9730092593 | 2005-12-11 23:21:08 | 800012030 | 30.6406 | 30 | 30.6486 | 30.6406 | 30.6639 | 30.6566 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27.8833 | 27.8833 | 56.3379 | 1 | PROCESSED | 57532.4195833333 | 2016-05-24 10:04:12 | 54247 | 2007-05-27 00:00:00 | 54039.1003703704 | 2006-10-31 02:24:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012030/ | Quick Look | ||
48 | A2199 OFFSET7 | 247.8714 | 39.0623 | 247.44001 | 39.168102 | 234.433925 | 59.797533 | 62.28955825 | 43.12499555 | 270.0014 | 55792.9380324074 | 2011-08-19 22:30:46 | 55793.5717708333 | 2011-08-20 13:43:21 | 806153010 | 28.9786 | 30 | 28.9946 | 28.9786 | 0 | 28.9946 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23.6221 | 23.6221 | 54.7439 | 1 | PROCESSED | 57602.8895138889 | 2016-08-02 21:20:54 | 55652 | 2011-04-01 00:00:00 | 55806.2932175926 | 2011-09-02 07:02:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806153010/ | Quick Look | |
49 | A133_S | 15.6819 | -22.1029 | 15.071421 | -22.371383 | 5.125588 | -26.4157 | 150.58121257 | -84.35810156 | 44.9946 | 55355.2966203704 | 2010-06-08 07:07:08 | 55356.727974537 | 2010-06-09 17:28:17 | 805022010 | 51.128 | 50 | 51.128 | 51.128 | 0 | 51.128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8599 | 42.8599 | 123.6558 | 1 | PROCESSED | 57551.9312962963 | 2016-06-12 22:21:04 | 55737 | 2011-06-25 00:00:00 | 55370.2538310185 | 2010-06-23 06:05:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805022010/ | Quick Look | ||
50 | RXCJ1053.7+5453 | 163.1919 | 54.9274 | 162.433556 | 55.193301 | 139.011043 | 43.216014 | 152.52898808 | 54.84022784 | 128.7233 | 56962.235150463 | 2014-11-01 05:38:37 | 56964.4029513889 | 2014-11-03 09:40:15 | 809120010 | 87.0847 | 100 | 87.0847 | 101.5529 | 0 | 101.5529 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7267708333 | 2016-08-16 17:26:33 | 56748 | 2014-04-01 00:00:00 | 57071.4205671296 | 2015-02-18 10:05:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROKI AKAMATSU | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809120010/ | Quick Look | ||
51 | A1914_OFFSET1 | 216.5784 | 38.0421 | 216.067238 | 38.26635 | 196.337734 | 48.766613 | 67.66951456 | 67.3249966 | 134.001 | 55565.4188194445 | 2011-01-04 10:03:06 | 55565.728599537 | 2011-01-04 17:29:11 | 805091020 | 11.393 | 10 | 11.401 | 11.393 | 0 | 11.401 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.3763 | 11.3763 | 25.4979 | 0 | PROCESSED | 57600.5573263889 | 2016-07-31 13:22:33 | 55995 | 2012-03-09 00:00:00 | 55627.1165625 | 2011-03-07 02:47:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADOKA KAWAHARADA | RYO NAGINO | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805091020/ | Quick Look | |
52 | A1914_OFFSET3 | 216.2252 | 37.8719 | 215.712166 | 38.097165 | 196.093912 | 48.482824 | 67.5271644 | 67.6467927 | 330.9949 | 55364.3811805556 | 2010-06-17 09:08:54 | 55365.2953587963 | 2010-06-18 07:05:19 | 805093010 | 28.5066 | 40 | 28.5066 | 28.5066 | 0 | 28.5066 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3813 | 26.3813 | 78.9679 | 1 | PROCESSED | 57552.3531018518 | 2016-06-13 08:28:28 | 55769 | 2011-07-27 00:00:00 | 55400.3084375 | 2010-07-23 07:24:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADOKA KAWAHARADA | ERIC MILLER | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805093010/ | Quick Look | |
53 | A2199 OFFSET11 | 246.6136 | 39.2216 | 246.181473 | 39.33303 | 232.494915 | 59.651332 | 62.4602069 | 44.10568707 | 268 | 55815.9308449074 | 2011-09-11 22:20:25 | 55816.4036342593 | 2011-09-12 09:41:14 | 806157010 | 20.6533 | 20 | 20.6613 | 20.6533 | 0 | 20.6613 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.551 | 20.551 | 40.8439 | 3 | PROCESSED | 57603.1066898148 | 2016-08-03 02:33:38 | 55652 | 2011-04-01 00:00:00 | 55865.9405555556 | 2011-10-31 22:34:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806157010/ | Quick Look | |
54 | NGC 5044 OFFSET2 | 199.1117 | -16.388 | 198.444886 | -16.124395 | 203.827071 | -7.694393 | 311.59229028 | 46.06278821 | 290.7836 | 53920.9609143518 | 2006-07-04 23:03:43 | 53922.7598842593 | 2006-07-06 18:14:14 | 801048010 | 62.451 | 60 | 62.451 | 62.451 | 62.451 | 62.451 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57.1102 | 57.1102 | 155.3149 | 2 | PROCESSED | 57534.8962615741 | 2016-05-26 21:30:37 | 54422 | 2007-11-18 00:00:00 | 54034.2926736111 | 2006-10-26 07:01:27 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801048010/ | Quick Look | ||
55 | A2199 OFFSET2 | 247.0222 | 38.9947 | 246.589024 | 39.104311 | 233.2293 | 59.533721 | 62.15962406 | 43.78139177 | 300.0001 | 55790.2001851852 | 2011-08-17 04:48:16 | 55790.5974884259 | 2011-08-17 14:20:23 | 806148010 | 20.2856 | 20 | 20.2856 | 20.2856 | 0 | 20.2856 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.074 | 15.074 | 34.3199 | 1 | PROCESSED | 57602.8518287037 | 2016-08-02 20:26:38 | 55652 | 2011-04-01 00:00:00 | 55806.1895601852 | 2011-09-02 04:32:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806148010/ | Quick Look | |
56 | FORNAX OFFSET3 | 55.0322 | -35.1579 | 54.552305 | -35.31846 | 39.454432 | -52.642961 | 236.21473388 | -53.30533318 | 63.6008 | 54664.1800810185 | 2008-07-17 04:19:19 | 54665.2009143518 | 2008-07-18 04:49:19 | 803008010 | 41.2795 | 30 | 41.2875 | 41.2795 | 0 | 41.2955 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0699 | 35.0699 | 88.1898 | 0 | PROCESSED | 57543.0818055556 | 2016-06-04 01:57:48 | 55055 | 2009-08-12 00:00:00 | 54689.4341087963 | 2008-08-11 10:25:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803008010/ | Quick Look | ||
57 | PERSEUS OFFSET-F | 49.9431 | 41.79 | 49.113812 | 41.609338 | 58.684902 | 22.607146 | 150.41345254 | -13.03211324 | 269.9991 | 55609.6649305556 | 2011-02-17 15:57:30 | 55610.152974537 | 2011-02-18 03:40:17 | 805046010 | 20.7197 | 25 | 20.7197 | 20.7197 | 0 | 20.7197 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.813 | 18.813 | 42.1599 | 0 | PROCESSED | 57600.9628125 | 2016-07-31 23:06:27 | 55990 | 2012-03-04 00:00:00 | 55621.2476967593 | 2011-03-01 05:56:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805046010/ | Quick Look | ||
58 | A2495 | 342.5777 | 10.9124 | 341.95313 | 10.647232 | 348.269753 | 16.897696 | 81.20126485 | -41.9387619 | 237.1467 | 54061.4694097222 | 2006-11-22 11:15:57 | 54062.0787037037 | 2006-11-23 01:53:20 | 801080010 | 18.0313 | 18 | 18.0313 | 18.3673 | 0 | 18.1193 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.3891 | 16.3891 | 52.6339 | 3 | PROCESSED | 57536.1381365741 | 2016-05-28 03:18:55 | 54695 | 2008-08-17 00:00:00 | 54088.9563194444 | 2006-12-19 22:57:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080010/ | Quick Look | ||
59 | NGC 4382 | 186.3492 | 18.1851 | 185.718232 | 18.461926 | 178.313661 | 19.153245 | 267.72488674 | 79.23166289 | 294.1787 | 54638.1652199074 | 2008-06-21 03:57:55 | 54640.4481944444 | 2008-06-23 10:45:24 | 803005010 | 99.0682 | 90 | 99.0682 | 99.0682 | 0 | 99.0682 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.4447 | 93.4447 | 197.2038 | 3 | PROCESSED | 57542.911412037 | 2016-06-03 21:52:26 | 55020 | 2009-07-08 00:00:00 | 54651.2282291667 | 2008-07-04 05:28:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030033 | We proposeto observe a S0 galaxy, NGC 4382 for 90 ks with Suzaku. The purpose of the observation is to study abundance pattern of O/Ne/Mg/Si/Fe of S0 galaxies and to study history of S0 galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 3 | AO3 | THE ISM ABUNDANCE OF A S0 GALAXY, NGC 4382 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803005010/ | Quick Look | ||
60 | FORNAX A W-LOBE S | 50.3569 | -37.3111 | 49.879649 | -37.489667 | 32.298971 | -53.110795 | 240.40306132 | -56.92864271 | 79.0007 | 55065.4424189815 | 2009-08-22 10:37:05 | 55066.6731365741 | 2009-08-23 16:09:19 | 804038020 | 45.5693 | 42 | 45.5693 | 45.5693 | 0 | 45.5693 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 38.9534 | 38.9534 | 106.2599 | 0 | PROCESSED | 57548.3175347222 | 2016-06-09 07:37:15 | 55444 | 2010-09-05 00:00:00 | 55078.0721064815 | 2009-09-04 01:43:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MAKOTO TASHIRO | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804038020/ | Quick Look | ||
61 | A2199 OFFSET16 | 247.7994 | 39.696 | 247.372677 | 39.802115 | 233.944751 | 60.385033 | 63.15474779 | 43.20527386 | 235.0008 | 55840.9241666667 | 2011-10-06 22:10:48 | 55841.4308217593 | 2011-10-07 10:20:23 | 806162010 | 28.3158 | 30 | 28.3158 | 28.3158 | 0 | 28.3158 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28.6983 | 28.6983 | 43.7679 | 0 | PROCESSED | 57603.3467824074 | 2016-08-03 08:19:22 | 55652 | 2011-04-01 00:00:00 | 55858.377037037 | 2011-10-24 09:02:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806162010/ | Quick Look | |
62 | FG25 | 234.9579 | 30.7058 | 234.452539 | 30.866616 | 221.876556 | 48.458584 | 48.772653 | 53.18955534 | 294.6599 | 56136.7541898148 | 2012-07-28 18:06:02 | 56137.0821875 | 2012-07-29 01:58:21 | 807049010 | 10.6393 | 10 | 10.6393 | 10.6393 | 0 | 10.6393 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.074 | 11.074 | 28.3281 | 0 | PROCESSED | 57606.6807523148 | 2016-08-06 16:20:17 | 56527 | 2013-08-23 00:00:00 | 56161.2376736111 | 2012-08-22 05:42:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ELENA D'ONGHIA | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807049010/ | Quick Look | ||
63 | A 2218 OFFSETB | 249.9091 | 65.2119 | 249.835523 | 65.307656 | 180.044789 | 81.713752 | 96.37864193 | 38.09205953 | 233.3309 | 53670.1916319444 | 2005-10-27 04:35:57 | 53670.4620833333 | 2005-10-27 11:05:24 | 800020010 | 14.9215 | 15 | 14.9375 | 14.9335 | 14.9215 | 14.9415 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14.1931 | 14.1931 | 23.3561 | 0 | PROCESSED | 57527.6596180556 | 2016-05-19 15:49:51 | 54247 | 2007-05-27 00:00:00 | 54036.8343981482 | 2006-10-28 20:01:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001096 | To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | SEARCH FOR OXYGEN LINES FROM WARM IGM | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800020010/ | Quick Look | |||
64 | VIRGO E13 | 191.4157 | 14.448 | 190.788981 | 14.721164 | 184.610172 | 17.765771 | 296.58532586 | 77.24852866 | 284.9997 | 56486.2639351852 | 2013-07-13 06:20:04 | 56486.8515856482 | 2013-07-13 20:26:17 | 808128010 | 20.4817 | 20 | 20.4897 | 20.4817 | 0 | 20.4897 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.787 | 18.787 | 50.7599 | 0 | PROCESSED | 57611.9056134259 | 2016-08-11 21:44:05 | 56383 | 2013-04-01 00:00:00 | 56503.6194444444 | 2013-07-30 14:52:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808128010/ | Quick Look | ||
65 | THE MOON | 131.4647 | 12.9515 | 130.775529 | 13.134573 | 130.365878 | -4.869219 | 213.82172975 | 31.16197152 | 285.4003 | 56783.5475578704 | 2014-05-06 13:08:29 | 56783.6842361111 | 2014-05-06 16:25:18 | 809001010 | 4.6424 | 45 | 4.6464 | 4.6424 | 0 | 4.6504 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.5647 | 4.5647 | 11.806 | 0 | PROCESSED | 57615.0366898148 | 2016-08-15 00:52:50 | 57162 | 2015-05-20 00:00:00 | 56793.5228125 | 2014-05-16 12:32:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001010/ | Quick Look | ||
66 | FORNAX A HOST GALAXY | 50.6684 | -37.2029 | 50.191244 | -37.380302 | 32.749558 | -53.117138 | 240.15407206 | -56.69497357 | 218.3809 | 54091.6179976852 | 2006-12-22 14:49:55 | 54092.8689699074 | 2006-12-23 20:51:19 | 801015010 | 48.7217 | 50 | 48.7217 | 48.7217 | 0 | 48.7217 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.3987 | 48.3987 | 108.0839 | 1 | PROCESSED | 57536.4184837963 | 2016-05-28 10:02:37 | 54735 | 2008-09-26 00:00:00 | 54132.9200347222 | 2007-02-01 22:04:51 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010029 | We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO TASHIRO | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801015010/ | Quick Look | ||
67 | COMA NW5 | 194.3037 | 29.1454 | 193.700799 | 29.41548 | 180.283789 | 32.183117 | 91.00313756 | 87.61452721 | 319.9965 | 55733.4693865741 | 2011-06-21 11:15:55 | 55734.0682407407 | 2011-06-22 01:38:16 | 806042010 | 21.0972 | 20 | 21.1201 | 21.1132 | 0 | 21.0972 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.4401 | 20.4401 | 51.724 | 0 | PROCESSED | 57602.3799537037 | 2016-08-02 09:07:08 | 55652 | 2011-04-01 00:00:00 | 55768.342025463 | 2011-07-26 08:12:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806042010/ | Quick Look | ||
68 | COMA SW5.5 | 193.6448 | 27.0863 | 193.037174 | 27.357142 | 180.762937 | 30.083449 | 29.67661506 | 89.29968791 | 314.5983 | 55735.866400463 | 2011-06-23 20:47:37 | 55736.3037037037 | 2011-06-24 07:17:20 | 806048010 | 15.2345 | 15 | 15.245 | 15.2345 | 0 | 15.2345 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.4375 | 16.4375 | 37.776 | 0 | PROCESSED | 57602.4025347222 | 2016-08-02 09:39:39 | 55652 | 2011-04-01 00:00:00 | 55794.9965625 | 2011-08-21 23:55:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806048010/ | Quick Look | ||
69 | 3C390.3_VICINITY_1 | 276.9861 | 79.7253 | 277.865171 | 79.689308 | 84.608267 | 76.703493 | 111.37115096 | 27.70478895 | 240.0064 | 56607.4234953704 | 2013-11-11 10:09:50 | 56608.4910648148 | 2013-11-12 11:47:08 | 808046010 | 57.71 | 50 | 57.71 | 57.72 | 0 | 57.7141 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.9408 | 52.9408 | 92.2319 | 1 | PROCESSED | 57613.2938425926 | 2016-08-13 07:03:08 | 56991 | 2014-11-30 00:00:00 | 56625.6961458333 | 2013-11-29 16:42:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080060 | We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO SAKAI | JAP | 8 | AO8 | DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808046010/ | Quick Look | ||
70 | BULLET-BKG | 105.498 | -55.9182 | 105.253708 | -55.844379 | 132.076188 | -77.080913 | 266.15428465 | -20.7753384 | 287.5121 | 56422.4617592593 | 2013-05-10 11:04:56 | 56424.0029976852 | 2013-05-12 00:04:19 | 808057010 | 51.0907 | 50 | 51.0987 | 51.0907 | 0 | 51.1067 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6938 | 46.6938 | 133.1496 | 0 | PROCESSED | 57611.3081365741 | 2016-08-11 07:23:43 | 56799 | 2014-05-22 00:00:00 | 56433.6980208333 | 2013-05-21 16:45:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808057010/ | Quick Look | ||
71 | A262 E4 | 29.5568 | 35.6351 | 28.819272 | 35.392091 | 40.300853 | 22.029449 | 137.89892988 | -25.28797491 | 250 | 56701.8723148148 | 2014-02-13 20:56:08 | 56702.5974652778 | 2014-02-14 14:20:21 | 808115010 | 31.9389 | 30 | 31.9469 | 31.9389 | 0 | 31.9549 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8117361111 | 2016-08-13 19:28:54 | 57080 | 2015-02-27 00:00:00 | 56714.739525463 | 2014-02-26 17:44:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | NORBERT WERNER | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808115010/ | Quick Look | |
72 | RXCJ0605 | 91.7111 | -35.2772 | 91.267409 | -35.26998 | 92.696732 | -58.702768 | 241.82465393 | -23.81756849 | 309.9841 | 55323.0313194444 | 2010-05-07 00:45:06 | 55323.8550810185 | 2010-05-07 20:31:19 | 805065030 | 42.4239 | 40 | 42.4319 | 42.4319 | 0 | 42.4239 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.146 | 39.146 | 71.1619 | 0 | PROCESSED | 57551.4298263889 | 2016-06-12 10:18:57 | 55287 | 2010-04-01 00:00:00 | 55341.5040393518 | 2010-05-25 12:05:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805065030/ | Quick Look | ||
73 | ABELL 426 W5.5 | 47.9127 | 41.6204 | 47.090331 | 41.432362 | 57.05648 | 22.874112 | 149.19418163 | -13.99181892 | 94.0012 | 55429.9950115741 | 2010-08-21 23:52:49 | 55430.3626967593 | 2010-08-22 08:42:17 | 805115010 | 9.8216 | 10 | 9.8256 | 9.8356 | 0 | 9.8216 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.999 | 6.999 | 31.768 | 0 | PROCESSED | 57553.1611342593 | 2016-06-14 03:52:02 | 55287 | 2010-04-01 00:00:00 | 55446.1245023148 | 2010-09-07 02:59:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805115010/ | Quick Look | ||
74 | NGC 2300 GROUP | 112.834 | 85.6974 | 108.693645 | 85.79613 | 93.629136 | 62.546385 | 127.72312729 | 27.79205873 | 339.9186 | 55237.1794907407 | 2010-02-10 04:18:28 | 55238.2502777778 | 2010-02-11 06:00:24 | 804030020 | 52.5611 | 100 | 52.5611 | 52.5611 | 0 | 52.5611 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.712 | 47.712 | 92.498 | 0 | PROCESSED | 57550.5807986111 | 2016-06-11 13:56:21 | 55633 | 2011-03-13 00:00:00 | 55266.3365625 | 2010-03-11 08:04:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804030020/ | Quick Look | ||
75 | A3526 | 191.1432 | -39.6142 | 190.459557 | -39.340673 | 207.301582 | -31.717062 | 301.49310157 | 23.23836897 | 110.0059 | 55944.2688078704 | 2012-01-18 06:27:05 | 55944.754375 | 2012-01-18 18:06:18 | 806090010 | 18.3702 | 16 | 18.3782 | 18.3702 | 0 | 18.3857 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.795 | 14.795 | 41.9499 | 2 | PROCESSED | 57604.405775463 | 2016-08-04 09:44:19 | 56352 | 2013-03-01 00:00:00 | 55985.1138310185 | 2012-02-28 02:43:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ANDREW FABIAN | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806090010/ | Quick Look | ||
76 | J2218.8-0258 | 334.694 | -2.9598 | 334.046783 | -3.210826 | 335.453457 | 7.033577 | 59.75779093 | -46.24852305 | 49.9996 | 56072.7972685185 | 2012-05-25 19:08:04 | 56073.7370833333 | 2012-05-26 17:41:24 | 807086010 | 38.3981 | 35 | 38.4061 | 38.3981 | 0 | 38.4061 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.9739 | 36.9739 | 81.1958 | 1 | PROCESSED | 57605.5228703704 | 2016-08-05 12:32:56 | 56500 | 2013-07-27 00:00:00 | 56134.0402199074 | 2012-07-26 00:57:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072018 | We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | E.G. PATRICK BOS | EUR | 7 | AO7 | CLUSTERS AND THE COSMIC WEB | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807086010/ | Quick Look | ||
77 | A 2218 CENTER | 249.0052 | 66.205 | 248.955095 | 66.304813 | 172.75657 | 81.615548 | 97.72589248 | 38.11630228 | 233.3294 | 53669.4904050926 | 2005-10-26 11:46:11 | 53670.1905555556 | 2005-10-27 04:34:24 | 800019010 | 31.9354 | 35 | 31.9434 | 31.9434 | 31.9354 | 31.9434 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.9371 | 28.9371 | 60.4879 | 1 | PROCESSED | 57527.6471990741 | 2016-05-19 15:31:58 | 54247 | 2007-05-27 00:00:00 | 54036.9596990741 | 2006-10-28 23:01:58 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001096 | To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | SEARCH FOR OXYGEN LINES FROM WARM IGM | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800019010/ | Quick Look | |||
78 | ABELL 2259 | 260.1834 | 27.7413 | 259.686949 | 27.789931 | 256.20097 | 50.711544 | 50.50845469 | 31.05916058 | 109.9997 | 57082.4117476852 | 2015-03-01 09:52:55 | 57083.6002199074 | 2015-03-02 14:24:19 | 809081020 | 42.5928 | 42.5 | 42.5928 | 43.0168 | 0 | 43.0568 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.687650463 | 2016-08-17 16:30:13 | 57465 | 2016-03-18 00:00:00 | 57097.407037037 | 2015-03-16 09:46:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809081020/ | Quick Look | ||
79 | SPT-CL J0000-5748 | 0.2511 | -57.8123 | 359.609856 | -58.090789 | 327.861661 | -51.025666 | 315.62746494 | -58.05556131 | 46.7517 | 55694.989849537 | 2011-05-13 23:45:23 | 55696.1169097222 | 2011-05-15 02:48:21 | 806074010 | 50.3986 | 50 | 50.3986 | 50.3986 | 0 | 50.3986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.4563 | 42.4563 | 97.3498 | 0 | PROCESSED | 57602.0636921296 | 2016-08-02 01:31:43 | 56072 | 2012-05-25 00:00:00 | 55705.1979166667 | 2011-05-24 04:45:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806074010/ | Quick Look | ||
80 | Z235 | 10.9622 | 24.4059 | 10.298374 | 24.132304 | 19.875378 | 18.073678 | 120.72614401 | -38.43334342 | 59.0539 | 53944.0060185185 | 2006-07-28 00:08:40 | 53944.6148032407 | 2006-07-28 14:45:19 | 801083010 | 20.0335 | 20 | 20.0415 | 20.0415 | 20.0415 | 20.0335 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19.5263 | 19.5263 | 52.5899 | 1 | PROCESSED | 57535.0666782407 | 2016-05-27 01:36:01 | 54401 | 2007-10-28 00:00:00 | 53955.6800925926 | 2006-08-08 16:19:20 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801083010/ | Quick Look | ||
81 | ABELL 262 CENTER | 28.1922 | 36.1591 | 27.457024 | 35.91293 | 39.406526 | 22.931602 | 136.56609466 | -25.08359968 | 69.9979 | 54329.1761921296 | 2007-08-17 04:13:43 | 54330.0446643518 | 2007-08-18 01:04:19 | 802001010 | 37.1645 | 36 | 37.1645 | 37.1645 | 0 | 37.1645 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.1304 | 34.1304 | 75.0299 | 1 | PROCESSED | 57539.6070949074 | 2016-05-31 14:34:13 | 54730 | 2008-09-21 00:00:00 | 54350.5576851852 | 2007-09-07 13:23:04 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020004 | We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802001010/ | Quick Look | ||
82 | VIRGO W5 | 186.3906 | 11.6158 | 185.756069 | 11.892616 | 181.170087 | 13.184054 | 280.29277845 | 73.33982916 | 99.9992 | 56273.927037037 | 2012-12-12 22:14:56 | 56274.3467476852 | 2012-12-13 08:19:19 | 807098010 | 16.6144 | 15 | 16.6261 | 16.6224 | 0 | 16.6144 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.174 | 18.174 | 36.256 | 0 | PROCESSED | 57608.2663078704 | 2016-08-08 06:23:29 | 56018 | 2012-04-01 00:00:00 | 56303.5207407407 | 2013-01-11 12:29:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807098010/ | Quick Look | ||
83 | VIRGO S5 | 187.6482 | 10.8577 | 187.014441 | 11.133804 | 182.643107 | 12.991025 | 285.16119801 | 73.00623042 | 308.4993 | 56112.5062037037 | 2012-07-04 12:08:56 | 56112.7681828704 | 2012-07-04 18:26:11 | 807119010 | 12.7732 | 10 | 12.7812 | 12.7732 | 0 | 12.7892 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.087 | 12.087 | 22.6239 | 0 | PROCESSED | 57606.5630439815 | 2016-08-06 13:30:47 | 56018 | 2012-04-01 00:00:00 | 56141.1590625 | 2012-08-02 03:49:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807119010/ | Quick Look | ||
84 | VIRGO E6 | 189.4489 | 13.3515 | 188.818836 | 13.626346 | 183.257959 | 15.984737 | 289.22685608 | 75.85896695 | 284.9998 | 56482.9353935185 | 2013-07-09 22:26:58 | 56483.2543171296 | 2013-07-10 06:06:13 | 808121010 | 14.633 | 14 | 14.641 | 14.641 | 0 | 14.633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0441 | 11.0441 | 27.5519 | 0 | PROCESSED | 57611.7799421296 | 2016-08-11 18:43:07 | 56383 | 2013-04-01 00:00:00 | 56496.5976157407 | 2013-07-23 14:20:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808121010/ | Quick Look | ||
85 | VIRGO E10 | 190.6018 | 13.9952 | 189.973652 | 14.269099 | 184.050004 | 17.029845 | 293.36819262 | 76.69896749 | 284.9995 | 56484.6167476852 | 2013-07-11 14:48:07 | 56485.1960416667 | 2013-07-12 04:42:18 | 808125010 | 21.4435 | 20 | 21.4435 | 21.4435 | 0 | 21.4435 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.152 | 19.152 | 50.044 | 1 | PROCESSED | 57611.8325115741 | 2016-08-11 19:58:49 | 56383 | 2013-04-01 00:00:00 | 56498.6333796296 | 2013-07-25 15:12:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808125010/ | Quick Look | ||
86 | A1689-OFFSET2 | 197.956 | -1.5158 | 197.313284 | -1.250483 | 197.134748 | 5.642151 | 313.46570539 | 60.93832198 | 289.9994 | 54671.3493518518 | 2008-07-24 08:23:04 | 54672.423125 | 2008-07-25 10:09:18 | 803025010 | 43.5468 | 40 | 43.5468 | 43.5468 | 0 | 43.5468 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.5486 | 36.5486 | 92.7159 | 2 | PROCESSED | 57543.1297685185 | 2016-06-04 03:06:52 | 55076 | 2009-09-02 00:00:00 | 54707.2585763889 | 2008-08-29 06:12:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NOBUHIRO OKABE | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803025010/ | Quick Look | ||
87 | A2061_1 | 229.9941 | 30.5295 | 229.479101 | 30.70939 | 216.056203 | 46.759039 | 47.89500096 | 57.43543483 | 120.6365 | 56306.3817939815 | 2013-01-14 09:09:47 | 56307.4847800926 | 2013-01-15 11:38:05 | 807029010 | 42.2923 | 40 | 42.3006 | 42.2991 | 0 | 42.2923 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.1838 | 38.1838 | 95.294 | 0 | PROCESSED | 57608.511087963 | 2016-08-08 12:15:58 | 56703 | 2014-02-15 00:00:00 | 56337.5472222222 | 2013-02-14 13:08:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070070 | We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO OKABE | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807029010/ | Quick Look | ||
88 | BULLET-OFFSET1 | 104.8831 | -55.8434 | 104.638861 | -55.772465 | 130.550899 | -77.176368 | 265.96507608 | -21.0808269 | 287.0003 | 56416.3315277778 | 2013-05-04 07:57:24 | 56419.0787037037 | 2013-05-07 01:53:20 | 808055010 | 102.9172 | 100 | 102.9412 | 102.9172 | 0 | 102.9412 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.4395 | 93.4395 | 237.3167 | 4 | PROCESSED | 57611.2833564815 | 2016-08-11 06:48:02 | 56795 | 2014-05-18 00:00:00 | 56429.7533101852 | 2013-05-17 18:04:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808055010/ | Quick Look | ||
89 | A3376 WEST RELIC | 90.0415 | -39.9946 | 89.634521 | -39.995405 | 90.079962 | -63.436398 | 246.43569548 | -26.38071178 | 132.0018 | 53681.5938078704 | 2005-11-07 14:15:05 | 53684.7883912037 | 2005-11-10 18:55:17 | 800011010 | 126.9969 | 150 | 126.9969 | 127.1809 | 127.0769 | 127.0289 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 112.9113 | 112.9113 | 230.9397 | 3 | PROCESSED | 57528.0013541667 | 2016-05-20 00:01:57 | 54247 | 2007-05-27 00:00:00 | 54037.6050231482 | 2006-10-29 14:31:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001039 | We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 0 | SWG | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800011010/ | Quick Look | ||
90 | ABELL 426 W7 | 47.3511 | 41.6379 | 46.530265 | 41.447862 | 56.625896 | 23.013072 | 148.81593544 | -14.19658633 | 93.9992 | 55431.0429398148 | 2010-08-23 01:01:50 | 55431.5078356482 | 2010-08-23 12:11:17 | 805109010 | 15.4161 | 15 | 15.4481 | 15.4321 | 0 | 15.4161 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2824 | 13.2824 | 40.1599 | 0 | PROCESSED | 57553.1742824074 | 2016-06-14 04:10:58 | 55287 | 2010-04-01 00:00:00 | 55449.2612731482 | 2010-09-10 06:16:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805109010/ | Quick Look | ||
91 | A2163NW | 243.7926 | -5.9349 | 243.126237 | -5.810502 | 242.931845 | 15.076918 | 6.85972512 | 30.71314923 | 93.93 | 57075.8011574074 | 2015-02-22 19:13:40 | 57077.0558333333 | 2015-02-24 01:20:24 | 809008010 | 48.0634 | 50 | 48.0634 | 49.7339 | 0 | 49.7194 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6490046296 | 2016-08-17 15:34:34 | 57454 | 2016-03-07 00:00:00 | 57087.4664467593 | 2015-03-06 11:11:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809008010/ | Quick Look | ||
92 | A2199 OFFSET1 | 247.4695 | 38.9998 | 247.037043 | 39.107408 | 233.880438 | 59.644289 | 62.18539249 | 43.43422484 | 299.9971 | 55789.6293171296 | 2011-08-16 15:06:13 | 55790.1995717593 | 2011-08-17 04:47:23 | 806147010 | 20.2965 | 20 | 20.2965 | 20.2965 | 0 | 20.2965 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2982 | 19.2982 | 49.2599 | 0 | PROCESSED | 57602.803287037 | 2016-08-02 19:16:44 | 55652 | 2011-04-01 00:00:00 | 55806.270150463 | 2011-09-02 06:29:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806147010/ | Quick Look | |
93 | A2572B | 349.6066 | 18.7294 | 348.98329 | 18.45586 | 358.210513 | 21.259827 | 94.21850787 | -38.90117923 | 59.1565 | 53922.7742939815 | 2006-07-06 18:34:59 | 53923.3002199074 | 2006-07-07 07:12:19 | 801073010 | 24.0595 | 21 | 24.0755 | 24.0595 | 24.0675 | 24.0755 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21.4951 | 21.4951 | 45.3979 | 1 | PROCESSED | 57534.8583912037 | 2016-05-26 20:36:05 | 54401 | 2007-10-28 00:00:00 | 53930.6043055556 | 2006-07-14 14:30:12 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801073010/ | Quick Look | ||
94 | A2199 OFFSET15 | 246.482 | 39.889 | 246.05467 | 40.001004 | 231.881042 | 60.252338 | 63.3872074 | 44.22195617 | 255.0003 | 55823.9923726852 | 2011-09-19 23:49:01 | 55824.6403935185 | 2011-09-20 15:22:10 | 806161010 | 28.1669 | 30 | 28.1829 | 28.1669 | 0 | 28.1829 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 28.0746 | 28.0746 | 55.9819 | 0 | PROCESSED | 57603.196412037 | 2016-08-03 04:42:50 | 55652 | 2011-04-01 00:00:00 | 55851.4457060185 | 2011-10-17 10:41:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | AURORA SIMIONESCU | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806161010/ | Quick Look | |
95 | 1RXJ0603 OFFSET | 92.2783 | 42.2687 | 91.384795 | 42.277603 | 91.783385 | 18.842189 | 170.6889541 | 10.70559867 | 80.0991 | 56214.8308564815 | 2012-10-14 19:56:26 | 56215.5314236111 | 2012-10-15 12:45:15 | 807002010 | 26.8334 | 30 | 26.8334 | 26.8574 | 0 | 26.8414 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.3531 | 28.3531 | 60.5159 | 1 | PROCESSED | 57607.7719907407 | 2016-08-07 18:31:40 | 56690 | 2014-02-02 00:00:00 | 56323.4936574074 | 2013-01-31 11:50:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070025 | We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HIROKI AKAMATSU | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807002010/ | Quick Look | ||
96 | CENA LOBE BGD1 | 205.3783 | -39.3349 | 204.641576 | -39.082547 | 218.514411 | -26.72025 | 313.38854271 | 22.51794697 | 286.0001 | 56122.4603125 | 2012-07-14 11:02:51 | 56123.1043634259 | 2012-07-15 02:30:17 | 807042010 | 22.2455 | 20 | 22.2455 | 22.2455 | 0 | 22.2455 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8556 | 18.8556 | 55.616 | 1 | PROCESSED | 57606.6151157407 | 2016-08-06 14:45:46 | 56018 | 2012-04-01 00:00:00 | 56142.2381597222 | 2012-08-03 05:42:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LUKASZ STAWARZ | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807042010/ | Quick Look | ||
97 | COMA W SHOCK1 | 194.1832 | 28.2738 | 193.578654 | 28.544023 | 180.637957 | 31.358455 | 77.58391557 | 88.36116739 | 275.406 | 56475.3084143518 | 2013-07-02 07:24:07 | 56475.66125 | 2013-07-02 15:52:12 | 808090010 | 16.692 | 15 | 16.692 | 16.716 | 0 | 16.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.638 | 13.638 | 30.4759 | 1 | PROCESSED | 57611.6582407407 | 2016-08-11 15:47:52 | 56897 | 2014-08-28 00:00:00 | 56524.6518518518 | 2013-08-20 15:38:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081529 | Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AURORA SIMIONESCU | USA | 8 | AO8 | THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808090010/ | Quick Look | ||
98 | A478 OFFSET A | 63.4449 | 10.2053 | 62.759891 | 10.079352 | 63.389046 | -10.816509 | 182.72704568 | -28.38203256 | 259.1008 | 55600.4642361111 | 2011-02-08 11:08:30 | 55601.5488194444 | 2011-02-09 13:10:18 | 805001010 | 44.3964 | 45 | 44.3964 | 44.3964 | 0 | 44.3964 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.2374 | 35.2374 | 93.6998 | 1 | PROCESSED | 57600.8998148148 | 2016-07-31 21:35:44 | 55983 | 2012-02-26 00:00:00 | 55617.4093981482 | 2011-02-25 09:49:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | ANDREW FABIAN | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805001010/ | Quick Look | |
99 | THE MOON | 337.3918 | -5.9294 | 336.739564 | -6.185815 | 336.879419 | 3.286876 | 58.6068568 | -50.1809823 | 252.3009 | 56990.3496643518 | 2014-11-29 08:23:31 | 56990.483587963 | 2014-11-29 11:36:22 | 809001320 | 6.3868 | 45 | 6.3868 | 6.3868 | 0 | 6.3868 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4101851852 | 2016-08-17 09:50:40 | 57415 | 2016-01-28 00:00:00 | 57006.395 | 2014-12-15 09:28:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHIHIRO UEDA | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809001320/ | Quick Look | ||
100 | A133_N | 15.6732 | -21.6726 | 15.062059 | -21.941094 | 5.322246 | -26.023104 | 148.68503798 | -83.97324559 | 44.9987 | 55352.9000347222 | 2010-06-05 21:36:03 | 55354.0974768518 | 2010-06-07 02:20:22 | 805020010 | 50.2334 | 50 | 50.2334 | 50.2334 | 0 | 50.2334 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44.176 | 44.176 | 103.416 | 1 | PROCESSED | 57551.8040740741 | 2016-06-12 19:17:52 | 55765 | 2011-07-23 00:00:00 | 55393.4422916667 | 2010-07-16 10:36:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805020010/ | Quick Look | ||
101 | FJ1145+6430 | 176.4302 | 64.5188 | 175.749504 | 64.796472 | 138.22089 | 54.839324 | 134.11889935 | 51.15827028 | 157.0241 | 56940.8652199074 | 2014-10-10 20:45:55 | 56941.847337963 | 2014-10-11 20:20:10 | 809036010 | 44.5555 | 45 | 44.5555 | 44.9155 | 0 | 44.9235 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6416435185 | 2016-08-16 15:23:58 | 57345 | 2015-11-19 00:00:00 | 56979.4120949074 | 2014-11-18 09:53:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IKUYUKI MITSUISHI | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809036010/ | Quick Look | ||
102 | CIZA J1358.9-4750 | 209.651 | -47.7758 | 208.860998 | -47.532845 | 225.745985 | -33.169178 | 314.45332941 | 13.58776424 | 104.5762 | 56313.755 | 2013-01-21 18:07:12 | 56315.4835648148 | 2013-01-23 11:36:20 | 807037010 | 61.6899 | 60 | 61.7299 | 61.6899 | 0 | 61.731 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.9497 | 58.9497 | 149.3318 | 1 | PROCESSED | 57608.595162037 | 2016-08-08 14:17:02 | 56718 | 2014-03-02 00:00:00 | 56351.6358680556 | 2013-02-28 15:15:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070101 | We propose a Suzaku observation of newly found merging cluster in the Zone of Avoidance, CIZA J1358.9-4750. The cluster has double core, and apparently in an early phase of merging. Targets with this phase is rare. With this observation, we want to obtain the temperature map of the bridge region and identify the existence of heating, to understand the merging phase of this cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TERUKAZU NISHIDA | JAP | 7 | AO7 | OBSERVATION OF THE NEWLY DISCOVERED MERGING CLUSTER NEAR THE GALACTIC DISC; CIZA J1358.9-4750 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807037010/ | Quick Look | ||
103 | CENTAURUS CLUSTER N | 192.2138 | -40.9141 | 191.523743 | -40.64159 | 208.863601 | -32.495572 | 302.40583252 | 21.95501054 | 115.2417 | 55961.0060763889 | 2012-02-04 00:08:45 | 55962.6667939815 | 2012-02-05 16:00:11 | 806011010 | 54.0496 | 50 | 54.0496 | 54.0496 | 0 | 54.0496 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.6109 | 48.6109 | 143.4758 | 2 | PROCESSED | 57604.5565972222 | 2016-08-04 13:21:30 | 56360 | 2013-03-09 00:00:00 | 55992.1577546296 | 2012-03-06 03:47:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060035 | We propose to observe two fields at 0.1-0.2r180 of the Centaurus cluster for total 90 ks exposures with Suzaku. The purpose of the observations is to determine Mg and Fe distributions of the intracluster medium up to 0.2 r180 and to study origin of metals in the intracluster medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 6 | AO6 | MG AND FE ABUNDANCES OF THE ICM IN THE CENTAURUS CLUSTER UP TO 0.2R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806011010/ | Quick Look | ||
104 | ABELL2801 | 9.6433 | -29.1188 | 9.027926 | -29.393572 | 356.054774 | -30.312746 | 357.12193154 | -86.53506096 | 232.0377 | 53701.3547106482 | 2005-11-27 08:30:47 | 53702.1668865741 | 2005-11-28 04:00:19 | 800008010 | 34.89 | 25 | 34.89 | 34.89 | 34.89 | 34.89 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.1636 | 30.1636 | 70.1639 | 1 | PROCESSED | 57528.0891898148 | 2016-05-20 02:08:26 | 54247 | 2007-05-27 00:00:00 | 54038.3717361111 | 2006-10-30 08:55:18 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYUKI TAMURA | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800008010/ | Quick Look | ||
105 | ABELL 1795 Near North | 207.2221 | 26.7993 | 206.645445 | 27.047459 | 193.815884 | 35.172187 | 34.737463 | 77.20142043 | 130.7334 | 53714.7756481482 | 2005-12-10 18:36:56 | 53715.3203587963 | 2005-12-11 07:41:19 | 800012020 | 24.4106 | 25 | 24.4266 | 24.4106 | 24.4426 | 24.4346 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 25.1798 | 25.1798 | 47.0559 | 2 | PROCESSED | 57532.404375 | 2016-05-24 09:42:18 | 54247 | 2007-05-27 00:00:00 | 54038.8804166667 | 2006-10-30 21:07:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012020/ | Quick Look | ||
106 | ABELL 1795 Near South | 207.2228 | 26.4007 | 206.645046 | 26.648859 | 194.026663 | 34.812966 | 32.94964182 | 77.16185549 | 129.833 | 53715.9739467593 | 2005-12-11 23:22:29 | 53716.5355787037 | 2005-12-12 12:51:14 | 800012040 | 26.074 | 25 | 26.098 | 26.0919 | 26.074 | 26.086 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.7986 | 25.7986 | 48.522 | 1 | PROCESSED | 57532.4329282407 | 2016-05-24 10:23:25 | 54247 | 2007-05-27 00:00:00 | 54039.0706018518 | 2006-10-31 01:41:40 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MARK BAUTZ | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800012040/ | Quick Look | ||
107 | NGC4388 | 186.4461 | 12.6674 | 185.812197 | 12.944186 | 180.780806 | 14.166666 | 279.11809751 | 74.34084148 | 119.622 | 53728.3779976852 | 2005-12-24 09:04:19 | 53731.250162037 | 2005-12-27 06:00:14 | 800017010 | 123.6341 | 100 | 123.9249 | 125.8143 | 123.6341 | 124.1523 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111.8209 | 111.8209 | 248.128 | 3 | PROCESSED | 57532.5484143518 | 2016-05-24 13:09:43 | 54247 | 2007-05-27 00:00:00 | 54039.5984375 | 2006-10-31 14:21:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001077 | Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKESHI TSURU | JAP | 0 | SWG | VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800017010/ | Quick Look | ||
108 | A2104W | 234.9146 | -3.2969 | 234.261116 | -3.135581 | 233.381893 | 15.795133 | 2.73337641 | 39.30878407 | 117.9077 | 54121.3401388889 | 2007-01-21 08:09:48 | 54121.8960532407 | 2007-01-21 21:30:19 | 801001010 | 19.9269 | 20 | 19.9269 | 19.9269 | 0 | 19.9269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.2001 | 17.2001 | 48.0079 | 2 | PROCESSED | 57536.8971875 | 2016-05-28 21:31:57 | 54735 | 2008-09-26 00:00:00 | 54137.0936805556 | 2007-02-06 02:14:54 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku |