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
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xis2_observation_mode
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xis3_observation_mode
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hxd_observation_mode
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hxd_coarse_clock_rate_exposure
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hxd_first_clock_rate_exposure
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hxd_normal_clock_rate_exposure
|
hxd_all_clock_rate_exposure
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hxd_wam_exposure
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quantity_of_hxd_burst
|
processing_status
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processing_date_mjd
|
processing_date
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public_date_mjd
|
public_date
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distribution_date_mjd
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distribution_date
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processing_version
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processing_count
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processing_software
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proposal_id
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proposal_abstract
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proposal_category
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proposal_category_code
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proposal_priority
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pi_name
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co_pi_name
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proposal_affiliated_country
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proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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 | ![]() |
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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/ver3.0/801001010/ | Quick Look | ![]() |
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109 | RX J1347.5-1145 | 206.8558 | -11.8095 | 206.189394 | -11.560383 | 209.147012 | -0.679812 | 323.97878779 | 48.76095676 | 291.7151 | 53931.2858333333 | 2006-07-15 06:51:36 | 53933.2551388889 | 2006-07-17 06:07:24 | 801013020 | 79.1105 | 75 | 79.1265 | 79.1105 | 79.1265 | 79.1345 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 69.567 | 69.567 | 170.1098 | 2 | PROCESSED | 57534.9865393518 | 2016-05-26 23:40:37 | 54394 | 2007-10-21 00:00:00 | 53942.463587963 | 2006-07-26 11:07:34 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010014 | We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013020/ | Quick Look | ![]() |
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110 | OPHIUCHUS CLUSTER 0 | 258.0174 | -23.3865 | 257.259196 | -23.326891 | 259.005066 | -0.401441 | 0.50702706 | 9.33401192 | 88.8366 | 54183.0313078704 | 2007-03-24 00:45:05 | 54183.5648726852 | 2007-03-24 13:33:25 | 801021010 | 16.6411 | 15 | 16.6411 | 16.6411 | 0 | 16.6411 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.5209 | 13.5209 | 46.0959 | 0 | PROCESSED | 57537.9746643518 | 2016-05-29 23:23:31 | 54736 | 2008-09-27 00:00:00 | 54209.5175462963 | 2007-04-19 12:25:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801021010/ | Quick Look | ![]() |
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111 | OPHIUCHUS CLUSTER 8 | 258.0175 | -23.6665 | 257.257716 | -23.606887 | 259.028283 | -0.680466 | 0.2749393 | 9.17298979 | 88.8988 | 54182.4897337963 | 2007-03-23 11:45:13 | 54183.0308333333 | 2007-03-24 00:44:24 | 801029010 | 23.7389 | 15 | 23.7469 | 23.7389 | 0 | 23.7469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.678 | 21.678 | 46.746 | 0 | PROCESSED | 57537.9753240741 | 2016-05-29 23:24:28 | 54736 | 2008-09-27 00:00:00 | 54209.5725231482 | 2007-04-19 13:44:26 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801029010/ | Quick Look | ![]() |
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112 | M87 50' SE | 188.2678 | 11.8367 | 187.635305 | 12.112401 | 182.806232 | 14.132107 | 286.30035277 | 74.11241529 | 119.899 | 54071.127650463 | 2006-12-02 03:03:49 | 54072.312037037 | 2006-12-03 07:29:20 | 801039010 | 53.6374 | 50 | 53.6374 | 53.6581 | 0 | 53.6454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.1394 | 46.1394 | 102.309 | 1 | PROCESSED | 57536.2354861111 | 2016-05-28 05:39:06 | 54735 | 2008-09-26 00:00:00 | 54088.5776736111 | 2006-12-19 13:51:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010084 | The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIRONORI MATSUMOTO | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801039010/ | Quick Look | ![]() |
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113 | PERSEUS CL OFFSET | 49.2788 | 41.3719 | 48.454118 | 41.188803 | 58.04223 | 22.344257 | 150.2212005 | -13.65398882 | 65.9966 | 53980.7676273148 | 2006-09-02 18:25:23 | 53981.4543287037 | 2006-09-03 10:54:14 | 801049020 | 32.4646 | 30 | 32.4806 | 32.4646 | 32.4966 | 32.4886 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 28.2912 | 28.2912 | 59.3199 | 1 | PROCESSED | 57535.422025463 | 2016-05-27 10:07:43 | 54526 | 2008-03-01 00:00:00 | 54021.2712731482 | 2006-10-13 06:30:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049020/ | Quick Look | ![]() |
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114 | ABELL 2199 OFFSET 4 | 247.0296 | 39.3161 | 246.598828 | 39.425672 | 233.044127 | 59.841273 | 62.60481799 | 43.78660639 | 250.4756 | 54012.6800462963 | 2006-10-04 16:19:16 | 54013.3044444444 | 2006-10-05 07:18:24 | 801060010 | 24.4546 | 25 | 24.4706 | 24.4626 | 24.4546 | 24.4775 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.811 | 25.811 | 53.9399 | 0 | PROCESSED | 57535.7612615741 | 2016-05-27 18:16:13 | 54735 | 2008-09-26 00:00:00 | 54024.6738888889 | 2006-10-16 16:10:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801060010/ | Quick Look | ![]() |
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115 | Z8276 | 266.0474 | 32.9693 | 265.586798 | 32.989586 | 263.998981 | 56.326696 | 57.88393681 | 27.65216461 | 308.1365 | 53961.1406134259 | 2006-08-14 03:22:29 | 53961.4723958333 | 2006-08-14 11:20:15 | 801079010 | 14.9374 | 14 | 14.9374 | 14.9374 | 14.9374 | 14.9374 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15.462 | 15.462 | 28.658 | 0 | PROCESSED | 57535.267962963 | 2016-05-27 06:25:52 | 54391 | 2007-10-18 00:00:00 | 54018.6023842593 | 2006-10-10 14:27:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801079010/ | Quick Look | ![]() |
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116 | A3667_CENTER | 303.141 | -56.7974 | 302.14092 | -56.947599 | 291.656641 | -35.82366 | 340.90266514 | -33.39955413 | 74.263 | 53861.7363078704 | 2006-05-06 17:40:17 | 53862.3843055556 | 2006-05-07 09:13:24 | 801096010 | 20.8805 | 20 | 20.8885 | 20.8885 | 20.8965 | 20.8805 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.425 | 8.425 | 55.9439 | 1 | PROCESSED | 57533.6497337963 | 2016-05-25 15:35:37 | 54394 | 2007-10-21 00:00:00 | 53913.7840509259 | 2006-06-27 18:49:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801096010/ | Quick Look | ![]() |
117 | CEN45 | 192.5119 | -41.3865 | 191.819775 | -41.11429 | 209.359018 | -32.811033 | 302.65166747 | 21.4844922 | 104.7288 | 54458.1467939815 | 2007-12-24 03:31:23 | 54459.2294444444 | 2007-12-25 05:30:24 | 802008010 | 58.2226 | 53 | 58.2226 | 58.2365 | 0 | 58.2306 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.5171 | 64.5171 | 93.5218 | 2 | PROCESSED | 57540.9525810185 | 2016-06-01 22:51:43 | 54854 | 2009-01-23 00:00:00 | 54486.1941087963 | 2008-01-21 04:39:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020011 | We propose to obtain high-quality X-ray spectra of the subcluster region in the Centaurus cluster, Cen45, aiming at the first reliable detection of a supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that Cen45 is indeed in the process of merging and has a high velocity relative to the main cluster. Utilizing the high-sensitivity Suzaku/XIS spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be accurately measured from the Doppler shift of iron-K lines. With our proposed 40ks observation, we can put a strong constraint on the gas motion in the subcluster region. This will also have great impacts on our understanding of dynamical state of clusters and their evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 2 | AO2 | MEASURING GAS MOTIONS OF THE INFALLING SUBCLUSTER CEN45 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802008010/ | Quick Look | ![]() |
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118 | A963N | 154.2645 | 39.1732 | 153.523641 | 39.42315 | 141.268932 | 26.461753 | 182.34163859 | 55.82043448 | 108.9136 | 54428.4751041667 | 2007-11-24 11:24:09 | 54429.0522453704 | 2007-11-25 01:15:14 | 802010010 | 29.1318 | 25 | 29.1318 | 29.1413 | 0 | 29.1358 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.8843 | 27.8843 | 49.8381 | 0 | PROCESSED | 57540.5914351852 | 2016-06-01 14:11:40 | 54804 | 2008-12-04 00:00:00 | 54434.2199305556 | 2007-11-30 05:16:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020018 | 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 10% precision in a few arcmin scale, which has not been done before to any cluster. 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 | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802010010/ | Quick Look | ![]() |
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119 | FORNAX_GALACTIC_1 | 48.2958 | -37.68 | 47.815673 | -37.866142 | 29.586545 | -52.740717 | 241.51144521 | -58.49700193 | 45.4419 | 54279.8103240741 | 2007-06-28 19:26:52 | 54280.3335532407 | 2007-06-29 08:00:19 | 802037010 | 20.4175 | 20 | 20.4175 | 20.4175 | 0 | 20.4175 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.1912 | 16.1912 | 45.184 | 0 | PROCESSED | 57539.0539814815 | 2016-05-31 01:17:44 | 54695 | 2008-08-17 00:00:00 | 54322.4346064815 | 2007-08-10 10:25:50 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802037010/ | Quick Look | ![]() |
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120 | OPHIUCHUS CLUSTER | 258.1093 | -23.379 | 257.351096 | -23.319827 | 259.088514 | -0.387026 | 0.56233145 | 9.26925896 | 277.7852 | 54367.8835069444 | 2007-09-24 21:12:15 | 54370.5939351852 | 2007-09-27 14:15:16 | 802046010 | 100.525 | 100 | 100.525 | 100.525 | 0 | 100.525 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.9495 | 82.9495 | 234.1619 | 3 | PROCESSED | 57540.1576041667 | 2016-06-01 03:46:57 | 54770 | 2008-10-31 00:00:00 | 54402.5613194444 | 2007-10-29 13:28:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020143 | The verification of the resonance scattering effect to resonance lines in an intracluster medium (ICM) is a big problem that has been carried over from ASCA. Though two interpretations for abnormality of intensity ratio of Fe-Kalpha/Fe Kbeta line, "resonance scattering effect" and "Ni overabundance", have been proposed, a determinate result has not been obtained. Both interpretations give a very big impact to the understanding of chemical evolution of ICM that has been obtained so far. To solve the problem, we propose the measurement of Ni and Fe lines with high precision for Ophiuchus cluster which is bright and hot enough for measuring the K lines. Moreover, this cluster is suggested the existence of non-thermal radiation from observations with Beppo-SAX, INTEGRAL, Swift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AKIHIRO FURUZAWA | JAP | 2 | AO2 | APPROCHING RESONANCE SCATTERING/NI-OVERABUNDANCE PROBLEM IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802046010/ | Quick Look | ![]() |
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121 | COMA_60OFF | 194.0251 | 27.4252 | 193.418894 | 27.695609 | 180.937501 | 30.537759 | 49.19228369 | 88.92228234 | 126.7582 | 54438.1998726852 | 2007-12-04 04:47:49 | 54439.1946990741 | 2007-12-05 04:40:22 | 802048010 | 36.6669 | 30 | 36.6669 | 36.6669 | 0 | 36.6669 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.6962 | 31.6962 | 85.9219 | 1 | PROCESSED | 57540.8231365741 | 2016-06-01 19:45:19 | 54814 | 2008-12-14 00:00:00 | 54445.3011689815 | 2007-12-11 07:13:41 | 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/ver3.0/802048010/ | Quick Look | ![]() |
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122 | BOOTES GROUP 26 | 219.0541 | 33.7727 | 218.530502 | 33.989642 | 201.885156 | 45.915481 | 55.78379271 | 66.53529007 | 323.2958 | 54265.160787037 | 2007-06-14 03:51:32 | 54266.3092476852 | 2007-06-15 07:25:19 | 802055010 | 43.6657 | 38 | 43.6737 | 43.6817 | 0 | 43.6657 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.8727 | 38.8727 | 99.2108 | 0 | PROCESSED | 57538.9553703704 | 2016-05-30 22:55:44 | 54695 | 2008-08-17 00:00:00 | 54271.4809837963 | 2007-06-20 11:32:37 | 3.0.22.43 | 3 | 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 | B | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802055010/ | Quick Look | ![]() |
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123 | PKS 0745-191 | 116.8852 | -19.2901 | 116.331446 | -19.165404 | 123.663194 | -39.639458 | 236.4397894 | 3.03527791 | 293.9994 | 54231.0124884259 | 2007-05-11 00:17:59 | 54231.8216898148 | 2007-05-11 19:43:14 | 802062010 | 32.0065 | 30 | 32.0065 | 32.0305 | 0 | 32.0145 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.7016 | 27.7016 | 69.9099 | 0 | PROCESSED | 57538.6154976852 | 2016-05-30 14:46:19 | 54695 | 2008-08-17 00:00:00 | 54238.8868518518 | 2007-05-18 21:17:04 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062010/ | Quick Look | ![]() |
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124 | FILAMENT JUNCTION 1 | 204.175 | 43.8307 | 203.643106 | 44.085146 | 179.610846 | 48.837733 | 97.2080472 | 70.96687365 | 328.3601 | 55706.688900463 | 2011-05-25 16:32:01 | 55707.984224537 | 2011-05-26 23:37:17 | 806003010 | 52.5091 | 60 | 52.5091 | 52.5171 | 0 | 52.5171 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.1339 | 50.1339 | 111.8899 | 0 | PROCESSED | 57602.1515509259 | 2016-08-02 03:38:14 | 56093 | 2012-06-15 00:00:00 | 55725.311412037 | 2011-06-13 07:28:26 | 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/ver3.0/806003010/ | Quick Look | ![]() |
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125 | PKS 0745-191 | 117.1155 | -19.3739 | 116.561976 | -19.248204 | 123.963107 | -39.669924 | 236.62179243 | 3.1809503 | 294.0002 | 54233.2263773148 | 2007-05-13 05:25:59 | 54234.0369675926 | 2007-05-14 00:53:14 | 802062040 | 32.9092 | 30 | 32.9092 | 32.9092 | 0 | 32.9092 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31.0085 | 31.0085 | 69.9999 | 0 | PROCESSED | 57538.6488541667 | 2016-05-30 15:34:21 | 54695 | 2008-08-17 00:00:00 | 54245.5354861111 | 2007-05-25 12:51:06 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062040/ | Quick Look | ![]() |
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126 | ABELL 262 OFFSET1 | 28.5344 | 36.2686 | 27.797773 | 36.023209 | 39.729024 | 22.927942 | 136.82832457 | -24.90547123 | 69.9996 | 54318.8941898148 | 2007-08-06 21:27:38 | 54320.0772337963 | 2007-08-08 01:51:13 | 802079010 | 54.5894 | 48 | 54.5974 | 54.5894 | 0 | 54.6029 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.9123 | 50.9123 | 102.2038 | 1 | PROCESSED | 57539.4485416667 | 2016-05-31 10:45:54 | 54730 | 2008-09-21 00:00:00 | 54347.4244791667 | 2007-09-04 10:11:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023004 | 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 | Fabio Gastaldello | JUS | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802079010/ | Quick Look | ![]() |
127 | IKT25 | 16.5704 | -72.153 | 16.175469 | -72.420209 | 314.528049 | -65.245772 | 301.32642461 | -44.92895011 | 33.6181 | 54601.2130208333 | 2008-05-15 05:06:45 | 54603.3675810185 | 2008-05-17 08:49:19 | 803002010 | 107.3223 | 100 | 107.3303 | 107.3303 | 0 | 107.3223 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124.1064 | 124.1064 | 186.1339 | 1 | PROCESSED | 57542.58375 | 2016-06-03 14:00:36 | 54981 | 2009-05-30 00:00:00 | 54613.1905439815 | 2008-05-27 04:34:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030016 | In order for the white dwarf, the progenitor of SN Ia, to increase its mass to the Chandrasekhar limit, stellar wind driven by Fe contained in the accreting matter needs to be strong enough. For this reason, SN Ia is difficult to take place in the galaxy with low metallicity. We propose the observation on IKT 25, a type Ia SNR candidate in SMC, in order to decide its origin. Since the Fe abundance of SMC (0.2 solar) is lower than that of any other galaxys where SN Ia (or its remnant) had already been discovered, this observation will give the strongest restriction to the theory of the white dwarf evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYA YAMAGUCHI | JAP | 3 | AO3 | IKT25: TYPE IA SNR CANDIDATE IN SMALL MAGELLANIC CLOUD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803002010/ | Quick Look | ![]() |
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128 | ZWCL_0823_FILAMENT-1 | 126.4596 | 4.2515 | 125.801978 | 4.415646 | 127.752151 | -14.538767 | 220.17063425 | 22.90045491 | 284.0603 | 54603.3781944444 | 2008-05-17 09:04:36 | 54604.4551388889 | 2008-05-18 10:55:24 | 803009010 | 41.3573 | 40 | 41.3573 | 41.3619 | 0 | 41.3619 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.9369 | 35.9369 | 93.0059 | 1 | PROCESSED | 57542.5603472222 | 2016-06-03 13:26:54 | 54979 | 2009-05-28 00:00:00 | 54613.0757060185 | 2008-05-27 01:49:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030039 | We propose Suzaku X-ray follow-up observations of dark matter (DM) halo "sub-clumps" detected by the Subaru weak-lens survey. The sub-clumps we are interested in are the smaller DM halo associated with large scale structures. According to the CDM hierarchical structure formation scenario, they are the elemental component of the universe. Since the barion component associated to the clumps are supposed to be very faint, the X-ray follow-up requires the highest sensitivity for diffuse sources, i.e. the Suzaku XIS detectors. Our aim is to detect barion signals and reveal the history/nature of these sub-clumps. A total of four pointing, two aiming at A222/223 filament and another two at ZwCl0823--A664 filament are proposed. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO NAKAZAWA | JAP | 3 | AO3 | SUZAKU X-RAY FOLLOW-UP OF DARK MATTER SUB-CLUMPS DETECTED WITH SUBARU WEAK-LENS SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803009010/ | Quick Look | ![]() |
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129 | NGC1961BACKGROUND | 85.5048 | 67.8763 | 84.182746 | 67.851301 | 87.633372 | 44.47331 | 145.2497599 | 18.81010884 | 72.0206 | 54748.602962963 | 2008-10-09 14:28:16 | 54749.1197222222 | 2008-10-10 02:52:24 | 803041010 | 24.1435 | 20 | 24.1435 | 24.1435 | 0 | 24.1435 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.099 | 20.099 | 44.6399 | 1 | PROCESSED | 57544.0915393518 | 2016-06-05 02:11:49 | 55148 | 2009-11-13 00:00:00 | 54780.6911342593 | 2008-11-10 16:35:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031401 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio. The Milky Way is missing at least 70% of its baryons while lower mass galaxies retain less than 10% of their baryons. Theory suggests that these baryons were expelled by intense galactic winds during the primary star formation period. These galactic winds carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding the very massive spiral galaxy, NGC 1961, which has 10 times the stellar content of M31 and with v_rot = 450 km/sec. If successful, we will detect a significant fraction of the 5E11 Msun of its missing baryons. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 3 | AO3 | THE BARYONS CONTENT OF THE MOST MASSIVE SPIRAL GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803041010/ | Quick Look | ![]() |
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130 | ABELL S753 RELIC | 211.0241 | -34.0331 | 210.287956 | -33.79356 | 220.862622 | -20.093047 | 319.70505054 | 26.46102153 | 102.5257 | 54838.0480555556 | 2009-01-07 01:09:12 | 54841.6668287037 | 2009-01-10 16:00:14 | 803053010 | 137.5275 | 120 | 137.5355 | 137.5275 | 0 | 137.5355 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 99.5992 | 99.5992 | 312.6056 | 3 | PROCESSED | 57545.2410069444 | 2016-06-06 05:47:03 | 55328 | 2010-05-12 00:00:00 | 54851.4730787037 | 2009-01-20 11:21:14 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031432 | The cluster radio relic PKS B1400-33 in the poor cluster Abell S753 will be observed with the HXD/PIN to detect and characterize the nonthermal Inverse Compton emission. This is one of the brightest cluster radio relics known. Remarkably, it is associated with a relatively poor, cool cluster. Although it has many properties similar to other cluster radio relics, it is possible that it is an old radio lobe, displaced by motions or buoyancy. The HXD/PIN data will be a strong test of merger shock acceleration processes. The XIS observations will constrain the low energy nonthermal spectrum and determine the thermal gas properties near the relic, and allow a merger shock to be detected. The long exposure with the XIS will also provide accurate abundances for the gas in this cool cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CRAIG SARAZIN | USA | 3 | AO3 | PKS B1400-33 AND ABELL S753: A VERY BRIGHT RADIO RELIC IN A POOR CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803053010/ | Quick Look | ![]() |
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131 | A3112 | 49.4785 | -44.2477 | 49.044044 | -44.429449 | 25.501128 | -58.962889 | 252.95565297 | -56.08416767 | 11.0983 | 54609.240162037 | 2008-05-23 05:45:50 | 54611.0557638889 | 2008-05-25 01:20:18 | 803054010 | 67.4982 | 60 | 67.4982 | 67.4982 | 0 | 67.4982 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.0658 | 59.0658 | 156.8578 | 0 | PROCESSED | 57542.6456365741 | 2016-06-03 15:29:43 | 54988 | 2009-06-06 00:00:00 | 54620.3684490741 | 2008-06-03 08:50:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031434 | We propose to perform spatially resolved spectroscopy on the X-ray bright relaxed galaxy cluster Abell 3112, in order to characterize its soft/hard X-ray excess component. Abell 3112 is one of two clusters with very strong soft excess emission (the other being Abell S1101, observed in AO1). The indications provided by this observation will be crucial in order to assess, beyond doubt, the reality of the soft excess emission, previously observed by all soft X-ray missions since EUVE. The proposed observation will constrain the nature of the excess emitter, and address outstanding questions in observational cosmology: the {it missing baryon} problem, the density of matter in the universe and the non-thermal energy in galaxy clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MASSIMILIANO BONAMENTE | USA | 3 | AO3 | SOFT EXCESS, HARD EXCESS AND THERMAL EMISSION IN ABELL 3112 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803054010/ | Quick Look | ![]() |
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132 | SHAPLEY OFF-FILAMENT | 201.0894 | -30.5701 | 200.390777 | -30.309695 | 211.196223 | -20.080758 | 311.26734846 | 31.76827748 | 298.8248 | 54666.4273958333 | 2008-07-19 10:15:27 | 54670.1905439815 | 2008-07-23 04:34:23 | 803068010 | 143.4669 | 140 | 143.4749 | 143.4749 | 0 | 143.4669 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110.8111 | 110.8111 | 325.0858 | 2 | PROCESSED | 57543.1803240741 | 2016-06-04 04:19:40 | 55073 | 2009-08-30 00:00:00 | 54707.3575694444 | 2008-08-29 08:34:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031451 | It is, in principle, possible to search for the signature of the Warm-Hot Intergalactic Medium (WHIM) in regions between clusters, where WHIM filaments are expected. However, the complexity of the filament network and the distance between clusters makes this approach very difficult (if not impossible), except in few cases where several clusters are sufficiently close together, such as within a supercluster. We propose an investigation using Suzaku of a region within the Shapley Supercluster where, following the cluster network, a filament is expected and a ROSAT PSPC investigation has found excess emission. Suzaku s characteristics will allow a clear detection and characterization of the filament. A second observation in an empty region nearby will be used as control field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MASSIMILIANO GALEAZZI | USA | 3 | AO3 | FILAMENTARY X-RAY STRUCTURE IN THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803068010/ | Quick Look | ![]() |
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133 | DEM L 205 | 82.0576 | -67.4229 | 82.080975 | -67.461346 | 340.764256 | -86.78514 | 277.64219696 | -32.8462006 | 9.9744 | 55005.3430092593 | 2009-06-23 08:13:56 | 55006.4578472222 | 2009-06-24 10:59:18 | 804010010 | 41.3433 | 40 | 41.3492 | 41.3492 | 0 | 41.3433 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3829 | 37.3829 | 96.3078 | 3 | PROCESSED | 57547.6717361111 | 2016-06-08 16:07:18 | 55381 | 2010-07-04 00:00:00 | 55015.1437268518 | 2009-07-03 03:26:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040009 | The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYA YAMAGUCHI | JAP | 4 | AO4 | DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804010010/ | Quick Look | ![]() |
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134 | A2390 | 328.3984 | 17.7035 | 327.804289 | 17.467151 | 337.435653 | 28.529496 | 73.96308198 | -27.80512015 | 79.9886 | 54955.5395486111 | 2009-05-04 12:56:57 | 54957.6939583333 | 2009-05-06 16:39:18 | 804012010 | 96.4645 | 90 | 96.4645 | 96.473 | 0 | 96.4725 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 85.5386 | 85.5386 | 186.1119 | 1 | PROCESSED | 57546.5371990741 | 2016-06-07 12:53:34 | 55343 | 2010-05-27 00:00:00 | 54976.1695023148 | 2009-05-25 04:04:05 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040011 | We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAOMI OTA | JAP | 4 | AO4 | SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804012010/ | Quick Look | ![]() |
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135 | FERMI_0265 | 187.8001 | -14.1665 | 187.150388 | -13.890445 | 192.786887 | -9.914495 | 295.53023761 | 48.41419063 | 294.2648 | 55020.9540277778 | 2009-07-08 22:53:48 | 55021.5418981482 | 2009-07-09 13:00:20 | 804017010 | 26.3115 | 80 | 26.3115 | 26.3115 | 0 | 26.3115 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.8463 | 22.8463 | 50.7879 | 1 | PROCESSED | 57547.7938773148 | 2016-06-08 19:03:11 | 55422 | 2010-08-14 00:00:00 | 55034.2333217593 | 2009-07-22 05:35:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804017010/ | Quick Look | ![]() |
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136 | FERMI_0459 | 304.3461 | 6.0496 | 303.729476 | 5.893761 | 308.253181 | 25.044638 | 48.6197877 | -16.02859504 | 257.4741 | 55131.4269097222 | 2009-10-27 10:14:45 | 55132.2224189815 | 2009-10-28 05:20:17 | 804020010 | 32.8128 | 30 | 32.8128 | 32.8128 | 0 | 32.8128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.6251 | 28.6251 | 68.7259 | 0 | PROCESSED | 57549.0265046296 | 2016-06-10 00:38:10 | 55513 | 2010-11-13 00:00:00 | 55149.4269791667 | 2009-11-14 10:14:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804020010/ | Quick Look | ![]() |
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137 | A2029_4 | 228.0053 | 5.6496 | 227.385284 | 5.836972 | 223.833276 | 22.612919 | 6.60771448 | 50.27207577 | 112.9543 | 55225.6146180556 | 2010-01-29 14:45:03 | 55226.2501388889 | 2010-01-30 06:00:12 | 804024040 | 25.6584 | 22 | 25.6584 | 25.6824 | 0 | 25.6664 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.446 | 19.446 | 54.9019 | 0 | PROCESSED | 57550.4263657407 | 2016-06-11 10:13:58 | 55637 | 2011-03-17 00:00:00 | 55271.0446064815 | 2010-03-16 01:04:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required 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 breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024040/ | Quick Look | ![]() |
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138 | NGC 669 | 26.8113 | 35.5683 | 26.082401 | 35.319076 | 38.038857 | 22.814409 | 135.52840833 | -25.9346715 | 67.5273 | 55017.2207523148 | 2009-07-05 05:17:53 | 55018.4377777778 | 2009-07-06 10:30:24 | 804049010 | 50.2528 | 50 | 50.2608 | 50.2528 | 0 | 50.2608 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45.4023 | 45.4023 | 105.1199 | 11 | PROCESSED | 57547.7727430556 | 2016-06-08 18:32:45 | 55395 | 2010-07-18 00:00:00 | 55029.2656944444 | 2009-07-17 06:22:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041504 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JOEL BREGMAN | USA | 4 | AO4 | THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804049010/ | Quick Look | ![]() |
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139 | RXJ1159+5531 | 179.953 | 55.611 | 179.309735 | 55.889319 | 149.803846 | 49.191232 | 137.55848692 | 60.02702904 | 317.8793 | 54953.4172222222 | 2009-05-02 10:00:48 | 54955.52875 | 2009-05-04 12:41:24 | 804051010 | 85.4892 | 75 | 85.4972 | 85.4892 | 0 | 85.4972 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.4128 | 82.4128 | 182.4218 | 2 | PROCESSED | 57546.517974537 | 2016-06-07 12:25:53 | 55343 | 2010-05-27 00:00:00 | 54976.1055439815 | 2009-05-25 02:31:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041514 | We propose a 75ks observation of the galaxy group RXJ1159+5531 to place definitive constraints on its gas out to the virial radius (Rvir). These unprecedented measurements will enable us to study the entropy profile at scales near the region in which accretion shocks become important, and will reveal whether its flattening outside the core of the group extends as far as Rvir. Furthermore, we will obtain the mass profile and test the validity of the NFW model in the outer parts of the halo. Due to its high surface brightness and favourable distance, RXJ1159+5531 is the ideal target with which to carry out this study. It will constitute a textbook case for constraining the feedback and other nongravitational processes which shape the distribution of hot gas in galaxy groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | PHILIP HUMPHREY | USA | 4 | AO4 | GAS IN A GALAXY GROUP AT THE VIRIAL RADIUS: RXJ1159+5531, A TEXTBOOK EXAMPLE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804051010/ | Quick Look | ![]() |
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140 | NGC741MOSAICE_P1 | 29.7199 | 5.461 | 29.066489 | 5.218433 | 29.574235 | -6.258595 | 152.014798 | -53.55912322 | 71.7248 | 55053.8433796296 | 2009-08-10 20:14:28 | 55054.0834837963 | 2009-08-11 02:00:13 | 804052010 | 10.8302 | 10 | 10.8342 | 10.8302 | 0 | 10.8381 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.8627 | 7.8627 | 20.74 | 0 | PROCESSED | 57548.1137847222 | 2016-06-09 02:43:51 | 55448 | 2010-09-09 00:00:00 | 55081.2096875 | 2009-09-07 05:01:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052010/ | Quick Look | ![]() |
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141 | NGC741MOSAICS_P4 | 29.2193 | 5.0492 | 28.567063 | 4.805449 | 28.959637 | -6.470888 | 151.55342081 | -54.14565062 | 71.7599 | 55053.1534259259 | 2009-08-10 03:40:56 | 55053.3759143518 | 2009-08-10 09:01:19 | 804054040 | 10.589 | 10 | 10.597 | 10.589 | 0 | 10.589 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.9689 | 9.9689 | 19.1919 | 0 | PROCESSED | 57548.09625 | 2016-06-09 02:18:36 | 55451 | 2010-09-12 00:00:00 | 55084.9935763889 | 2009-09-10 23:50:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054040/ | Quick Look | ![]() |
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142 | ABELL 426 E1 | 50.3027 | 41.5257 | 49.474155 | 41.346372 | 58.885391 | 22.278944 | 150.79331238 | -13.10366228 | 89.0025 | 55041.5144560185 | 2009-07-29 12:20:49 | 55041.7141666667 | 2009-07-29 17:08:24 | 804056010 | 9.696 | 10 | 9.696 | 9.696 | 0 | 9.696 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.856 | 7.856 | 17.2479 | 0 | PROCESSED | 57547.9587268518 | 2016-06-08 23:00:34 | 55419 | 2010-08-11 00:00:00 | 55050.256400463 | 2009-08-07 06:09:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804056010/ | Quick Look | ![]() |
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143 | ABELL 426 E5 | 51.7975 | 41.5108 | 50.964978 | 41.337079 | 60.044403 | 21.962427 | 151.74947693 | -12.48443224 | 87.0002 | 55042.7485069444 | 2009-07-30 17:57:51 | 55043.2932175926 | 2009-07-31 07:02:14 | 804060010 | 21.649 | 20 | 21.649 | 21.9423 | 0 | 21.929 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22.1391 | 22.1391 | 47.0481 | 0 | PROCESSED | 57548.0130208333 | 2016-06-09 00:18:45 | 55427 | 2010-08-19 00:00:00 | 55060.702349537 | 2009-08-17 16:51:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804060010/ | Quick Look | ![]() |
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144 | ABELL 426 N3 | 49.4023 | 42.2033 | 48.571812 | 42.020646 | 58.391407 | 23.116315 | 149.83616068 | -12.90614214 | 59.9986 | 55062.4722106482 | 2009-08-19 11:19:59 | 55062.7542708333 | 2009-08-19 18:06:09 | 804065010 | 12.2498 | 10 | 12.2498 | 12.2498 | 0 | 12.2498 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.8582 | 11.8582 | 24.3619 | 0 | PROCESSED | 57548.2751157407 | 2016-06-09 06:36:10 | 55441 | 2010-09-02 00:00:00 | 55074.9931597222 | 2009-08-31 23:50:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804065010/ | Quick Look | ![]() |
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145 | ABELL 426 N7 | 48.6285 | 43.1676 | 47.793828 | 42.98212 | 58.096043 | 24.202758 | 148.81295674 | -12.39950143 | 59.9993 | 55064.6340509259 | 2009-08-21 15:13:02 | 55065.4329166667 | 2009-08-22 10:23:24 | 804069010 | 36.4901 | 30 | 36.4901 | 36.5101 | 0 | 36.5021 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.3696 | 30.3696 | 69.018 | 0 | PROCESSED | 57548.3120486111 | 2016-06-09 07:29:21 | 55441 | 2010-09-02 00:00:00 | 55075.0667708333 | 2009-09-01 01:36:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804069010/ | Quick Look | ![]() |
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146 | RCS0928+3646 | 142.0898 | 36.7798 | 141.319732 | 36.998258 | 132.498761 | 20.704213 | 186.98438508 | 46.37223207 | 116.6063 | 55148.3222800926 | 2009-11-13 07:44:05 | 55149.1064699074 | 2009-11-14 02:33:19 | 804080010 | 36.5167 | 30 | 36.5327 | 36.5167 | 0 | 36.5327 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.0584 | 27.0584 | 67.7439 | 1 | PROCESSED | 57549.3099652778 | 2016-06-10 07:26:21 | 55546 | 2010-12-16 00:00:00 | 55180.0365972222 | 2009-12-15 00:52:42 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041525 | Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 4 | AO4 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804080010/ | Quick Look | ![]() |
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147 | A1795_FAR_NORTHEAST | 207.4803 | 26.8793 | 206.904436 | 27.126887 | 194.02783 | 35.343989 | 35.17669327 | 76.97815393 | 300.5693 | 55010.6105439815 | 2009-06-28 14:39:11 | 55011.5556712963 | 2009-06-29 13:20:10 | 804082010 | 40.0263 | 35 | 40.0263 | 40.0263 | 0 | 40.0263 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57547.6967476852 | 2016-06-08 16:43:19 | 55395 | 2010-07-18 00:00:00 | 55026.4466087963 | 2009-07-14 10:43:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804082010/ | Quick Look | ![]() |
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148 | A1795_FAR_WEST | 206.824 | 26.695 | 206.246184 | 26.94403 | 193.479611 | 34.924294 | 34.12189199 | 77.54661564 | 300.5663 | 55008.5840625 | 2009-06-26 14:01:03 | 55009.4634143518 | 2009-06-27 11:07:19 | 804084010 | 35.4763 | 35 | 35.4843 | 35.4763 | 0 | 35.4843 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.3466 | 30.3466 | 75.9378 | 1 | PROCESSED | 57547.7077662037 | 2016-06-08 16:59:11 | 55395 | 2010-07-18 00:00:00 | 55022.2936458333 | 2009-07-10 07:02:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804084010/ | Quick Look | ![]() |
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149 | A478 OFFSET C | 63.6328 | 10.5074 | 62.946361 | 10.382264 | 63.629527 | -10.552687 | 182.59008129 | -28.04907037 | 259.6787 | 55604.2488888889 | 2011-02-12 05:58:24 | 55605.3522685185 | 2011-02-13 08:27:16 | 805003010 | 47.1486 | 45 | 47.1646 | 47.1486 | 0 | 47.1646 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.9898 | 39.9898 | 95.3198 | 2 | PROCESSED | 57600.9430671296 | 2016-07-31 22:38:01 | 55983 | 2012-02-26 00:00:00 | 55617.4134490741 | 2011-02-25 09:55:22 | 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/ver3.0/805003010/ | Quick Look | ![]() |
150 | RXCJ0013.2-4905 | 3.3206 | -49.1017 | 2.696864 | -49.379799 | 337.855034 | -45.122753 | 318.93482177 | -66.82406097 | 263.5597 | 55565.2569328704 | 2011-01-04 06:09:59 | 55565.4036689815 | 2011-01-04 09:41:17 | 805023010 | 8.432 | 10 | 8.432 | 8.432 | 0 | 8.432 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57600.5421875 | 2016-07-31 13:00:45 | 56016 | 2012-03-30 00:00:00 | 55627.5157638889 | 2011-03-07 12:22:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050021 | We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 5 | AO5 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805023010/ | Quick Look | ![]() |
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151 | A2199 EAST OFFSET | 246.7666 | 40.2374 | 246.342386 | 40.34813 | 232.073247 | 60.652123 | 63.87682573 | 44.00920476 | 240.0015 | 55458.2941666667 | 2010-09-19 07:03:36 | 55459.7155324074 | 2010-09-20 17:10:22 | 805042010 | 58.4398 | 60 | 58.4399 | 58.4398 | 0 | 58.4398 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52.5076 | 52.5076 | 122.7919 | 1 | PROCESSED | 57553.4778935185 | 2016-06-14 11:28:10 | 55836 | 2011-10-02 00:00:00 | 55470.1049884259 | 2010-10-01 02:31:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050081 | We propose to observe the virial radius region of the cluster of galaxies A2199 (z=0.0309) over the virial radius. This cluster lies in the Great Wall, and a cosmic filament runs from north to south. We aim to explore possible influence from the filament gives onto the formation process of the cluster, by comparing the hot-gas density and temperature around the virial radius in parallel and vertical directions to the filament. With the high sensitivity of XIS to faint extended emission, we expect to detect denser and hotter gas in the filement even outside the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROKI AKAMATSU | JAP | 5 | AO5 | TEMPERATURE OVER THE VIRIAL RADIUS OF ABELL 2199, AND INFLUENCE OF THE LARGE-SCALE STRUCTURE. | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805042010/ | Quick Look | ![]() |
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152 | VIRGOHI 21 | 184.472 | 14.7597 | 183.83671 | 15.037342 | 178.086194 | 15.290258 | 268.97789082 | 75.3718003 | 123.3105 | 55535.5218518518 | 2010-12-05 12:31:28 | 55537.7911574074 | 2010-12-07 18:59:16 | 805054010 | 103.1915 | 100 | 103.3995 | 103.1915 | 0 | 103.3995 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.9209 | 81.9209 | 196.0168 | 4 | PROCESSED | 57554.4175694444 | 2016-06-15 10:01:18 | 55916 | 2011-12-21 00:00:00 | 55550.3035185185 | 2010-12-20 07:17:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050114 | We propose a 100 ksec observation of "VIRGOHI 21" in the Virgo galaxy cluster. VIRGOHI 21 with no optical counterpart, is called a "dark galaxy" from the presence of velocity informed gas clouds with 21-cm observations somewhat like a disk galaxy. Origins are said to be traces of density fluctuation at cluster birth, or gas stripped from galaxies, but nothing clear is yet not introduced. Using the energy resolution of the XIS, we would like to explain the origin, deciding heavy element abundances of VIRGOHI 21. Extremely low abundance will give us the first "dark galaxy". Discovery of a "dark galaxy" with its information of prehistoric universe, will lead us to not just galaxy evolution, but also mighty mechanisms to understand cosmology, giving great impact to astrophysics itself. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RYO IIZUKA | JAP | 5 | AO5 | X-RAY SEARCH FOR A DARK GALAXY IN THE VIRGO CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805054010/ | Quick Look | ![]() |
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153 | A2204_FIELD_2 | 248.1003 | 5.3993 | 247.484152 | 5.504515 | 245.364183 | 26.985557 | 20.85022945 | 33.23419381 | 260.9996 | 55435.6212615741 | 2010-08-27 14:54:37 | 55436.6744675926 | 2010-08-28 16:11:14 | 805057010 | 39.7312 | 40 | 39.7392 | 39.7312 | 0 | 39.7421 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.3157 | 35.3157 | 90.9818 | 1 | PROCESSED | 57553.2244444445 | 2016-06-14 05:23:12 | 55287 | 2010-04-01 00:00:00 | 55449.2310416667 | 2010-09-10 05:32:42 | 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/ver3.0/805057010/ | Quick Look | ![]() |
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154 | A1413_FIELD_1 | 178.851 | 23.2234 | 178.207267 | 23.50167 | 169.288709 | 20.757468 | 226.97411288 | 76.74388731 | 303.0003 | 55345.0808333333 | 2010-05-29 01:56:24 | 55346.139849537 | 2010-05-30 03:21:23 | 805059010 | 40.2041 | 40 | 40.2041 | 40.2041 | 0 | 40.2041 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.564 | 34.564 | 91.4919 | 1 | PROCESSED | 57551.6776041667 | 2016-06-12 16:15:45 | 55287 | 2010-04-01 00:00:00 | 55365.2529513889 | 2010-06-18 06:04:15 | 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/ver3.0/805059010/ | Quick Look | ![]() |
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155 | NGC5129 OFF-CENTER2 | 201.1253 | 13.7341 | 200.509035 | 13.994301 | 194.045924 | 20.91983 | 334.52733324 | 74.54035563 | 127.8098 | 55548.7900810185 | 2010-12-18 18:57:43 | 55549.42875 | 2010-12-19 10:17:24 | 805073010 | 30.7651 | 30 | 30.7811 | 30.7651 | 0 | 30.7811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.2475 | 25.2475 | 55.168 | 0 | PROCESSED | 57554.4510416667 | 2016-06-15 10:49:30 | 55960 | 2012-02-03 00:00:00 | 55593.1036805556 | 2011-02-01 02:29:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805073010/ | Quick Look | ![]() |
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156 | NGC5129 BACKGROUND | 201.7433 | 13.5725 | 201.127421 | 13.831619 | 194.704871 | 21.009611 | 336.16988197 | 74.1046924 | 116.4041 | 55547.7947106482 | 2010-12-17 19:04:23 | 55548.0397106482 | 2010-12-18 00:57:11 | 805074010 | 12.2767 | 10 | 12.2767 | 12.2847 | 0 | 12.2927 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7811 | 10.7811 | 21.16 | 0 | PROCESSED | 57554.4321180556 | 2016-06-15 10:22:15 | 55960 | 2012-02-03 00:00:00 | 55592.9616435185 | 2011-01-31 23:04:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805074010/ | Quick Look | ![]() |
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157 | ESO3060170 OFFSET | 85.0343 | -41.2366 | 84.63691 | -41.261684 | 81.30371 | -64.529199 | 246.8664627 | -30.36071331 | 321.0164 | 55326.497025463 | 2010-05-10 11:55:43 | 55327.7204166667 | 2010-05-11 17:17:24 | 805076010 | 78.6782 | 80 | 78.6782 | 78.6862 | 0 | 78.6862 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.7827 | 69.7827 | 105.6858 | 1 | PROCESSED | 57551.4828240741 | 2016-06-12 11:35:16 | 55707 | 2011-05-26 00:00:00 | 55341.5427893518 | 2010-05-25 13:01:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051513 | We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 5 | AO5 | HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805076010/ | Quick Look | ![]() |
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158 | PKS 0745-191 | 116.7033 | -18.9048 | 116.14781 | -18.780899 | 123.330634 | -39.304661 | 236.01965558 | 3.07990407 | 294.0011 | 55315.865462963 | 2010-04-29 20:46:16 | 55316.6418518518 | 2010-04-30 15:24:16 | 805084010 | 34.8356 | 35 | 34.8356 | 34.8356 | 0 | 34.8356 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.5067 | 29.5067 | 67.0759 | 1 | PROCESSED | 57551.3211458333 | 2016-06-12 07:42:27 | 55696 | 2011-05-15 00:00:00 | 55330.1469675926 | 2010-05-14 03:31:38 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805084010/ | Quick Look | ![]() |
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159 | RCS2343-3517 | 355.9933 | -35.2927 | 355.337628 | -35.570369 | 340.879701 | -30.492367 | 359.21699124 | -73.45928386 | 237.6557 | 55523.8239930556 | 2010-11-23 19:46:33 | 55525.0418171296 | 2010-11-25 01:00:13 | 805088010 | 48.3167 | 61 | 48.3167 | 48.3167 | 0 | 48.3167 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.1454 | 40.1454 | 105.1859 | 1 | PROCESSED | 57554.2088078704 | 2016-06-15 05:00:41 | 55903 | 2011-12-08 00:00:00 | 55537.0179861111 | 2010-12-07 00:25:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051527 | Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 5 | AO5 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805088010/ | Quick Look | ![]() |
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160 | NGC 1332 | 51.5732 | -21.333 | 51.017829 | -21.507123 | 42.191625 | -38.615675 | 212.17958034 | -54.36451308 | 243.6482 | 55581.2509027778 | 2011-01-20 06:01:18 | 55584.0883333333 | 2011-01-23 02:07:12 | 805095010 | 101.423 | 100 | 101.423 | 101.423 | 0 | 101.423 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.9683 | 89.9683 | 245.1259 | 2 | PROCESSED | 57600.7603935185 | 2016-07-31 18:14:58 | 55965 | 2012-02-08 00:00:00 | 55599.216724537 | 2011-02-07 05:12:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 054502 | Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients. The broad peaks of Fe abundance indicate (turbulent) diffusion of metals possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku XIS, we have found similar gradients in three lower mass (virial mass 5-10E12 Msun) elliptical galaxies, which has important implications for models of feedback and chemical enrichment. We propose to observe another two carefully chosen galaxies, thus starting to build a sample for determining the frequency and properties of such abundance gradients in early-type galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | PHILIP HUMPHREY | RYO NAGINO | USJ | 5 | AO5 | ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805095010/ | Quick Look | ![]() |
161 | ABELL 426 S4 | 49.6689 | 40.4337 | 48.849146 | 40.252043 | 58.065773 | 21.361001 | 151.00436531 | -14.27811504 | 87.9984 | 55425.804849537 | 2010-08-17 19:18:59 | 55426.0731018518 | 2010-08-18 01:45:16 | 805099010 | 12.3072 | 10 | 12.3072 | 12.3072 | 0 | 12.3072 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.95 | 9.95 | 23.1699 | 0 | PROCESSED | 57553.1090277778 | 2016-06-14 02:37:00 | 55287 | 2010-04-01 00:00:00 | 55439.1353009259 | 2010-08-31 03:14:50 | 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/ver3.0/805099010/ | Quick Look | ![]() |
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162 | ABELL 426 W4 | 48.4696 | 41.6016 | 47.645739 | 41.415563 | 57.483228 | 22.736303 | 149.56812051 | -13.78700029 | 86.9981 | 55429.3049884259 | 2010-08-21 07:19:11 | 55429.5696527778 | 2010-08-21 13:40:18 | 805106010 | 10.3652 | 10 | 10.3652 | 10.3732 | 0 | 10.3732 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.68 | 9.68 | 22.8559 | 0 | PROCESSED | 57553.1536111111 | 2016-06-14 03:41:12 | 55287 | 2010-04-01 00:00:00 | 55445.2490509259 | 2010-09-06 05:58:38 | 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/ver3.0/805106010/ | Quick Look | ![]() |
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163 | SNR B0532-675 | 83.0766 | -67.535 | 83.105131 | -67.568522 | 336.894388 | -87.135778 | 277.71335978 | -32.44457154 | 140.0497 | 55871.6295601852 | 2011-11-06 15:06:34 | 55874.1570601852 | 2011-11-09 03:46:10 | 806007010 | 82.4909 | 80 | 82.4909 | 82.4909 | 0 | 82.4909 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.4573 | 77.4573 | 218.3547 | 4 | PROCESSED | 57603.7734027778 | 2016-08-03 18:33:42 | 56257 | 2012-11-26 00:00:00 | 55890.6997337963 | 2011-11-25 16:47:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060025 | Interstellar medium (ISM) heated by a forward shock of supernova remnants (SNRs) gives us a unique opportunity to study local metal abundance and density. Systematic study of the shock-heated ISM in a galaxy unveils its overall metal distribution and provides a key to understand its chemical evolution. On the basis of this idea, we have performed observations of SNRs in the Large Magellanic Cloud (LMC). We here propose to observe the LMC SNR B0532-675 for 80 ks. Since it locates near the star formation region LH76, we expect that we can study the process of metal diffusion from a star forming region by utilizing the result from another SNR DEM L241 near LH76 already observed. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KENTARO SOMEYA | JAP | 6 | AO6 | STUDY OF CHEMICAL EVOLUTION OF THE LARGE MAGELLANIC CLOUD WITH SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806007010/ | Quick Look | ![]() |
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164 | XMMU 2235.3-2557 | 338.8435 | -25.9657 | 338.152793 | -26.224773 | 330.62189 | -15.821353 | 27.27021923 | -59.64080614 | 244.5944 | 55878.6378125 | 2011-11-13 15:18:27 | 55881.5577777778 | 2011-11-16 13:23:12 | 806013010 | 101.1227 | 100 | 101.1227 | 101.1227 | 0 | 101.1227 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90.6244 | 90.6244 | 252.2417 | 4 | PROCESSED | 57603.8656481482 | 2016-08-03 20:46:32 | 56257 | 2012-11-26 00:00:00 | 55890.7014583333 | 2011-11-25 16:50:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060038 | Galaxy clusters at high redshift are useful as a cosmological probe that have a potential to constrain the inflation theory via its mass function. A massive cluster, XMMU 2235.3-2557 found at z=1.4 is especially important because the presence itself should be quite rare if the standard theory with the Gaussian random field is correct. However, there can be a lot of systematic errors of the mass estimates, that is, the temperature measurement of the cluster. Hence, we propose an independent measurement of X-ray spectroscopic temperature by SUZAKU. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HAJIME KAWAHARA | JAP | 6 | AO6 | TEMPERATURE MEASUREMENT OF A MASSIVE HIGH-Z CLUSTER XMMU 2235.3-2557 BY SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806013010/ | Quick Look | ![]() |
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165 | ABELL 773 | 139.2619 | 51.6127 | 138.389122 | 51.822209 | 124.54102 | 33.911668 | 166.27594696 | 43.26641657 | 277.0001 | 55684.0736342593 | 2011-05-03 01:46:02 | 55684.909212963 | 2011-05-03 21:49:16 | 806027030 | 47.578 | 50 | 47.578 | 47.578 | 0 | 47.578 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1095 | 44.1095 | 72.1819 | 0 | PROCESSED | 57601.9127083333 | 2016-08-01 21:54:18 | 55652 | 2011-04-01 00:00:00 | 55697.2793518518 | 2011-05-16 06:42:16 | 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/ver3.0/806027030/ | Quick Look | ![]() |
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166 | ABELL 1068 | 160.1718 | 40.1411 | 159.449793 | 40.402342 | 145.494968 | 29.227943 | 178.75085582 | 60.06234552 | 130.0011 | 55860.7020601852 | 2011-10-26 16:50:58 | 55861.8821527778 | 2011-10-27 21:10:18 | 806028010 | 51.9826 | 50 | 51.9906 | 51.9826 | 0 | 51.9826 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.5347 | 44.5347 | 101.9378 | 1 | PROCESSED | 57603.6168981482 | 2016-08-03 14:48:20 | 55652 | 2011-04-01 00:00:00 | 55874.1455324074 | 2011-11-09 03:29:34 | 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/ver3.0/806028010/ | Quick Look | ![]() |
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167 | ABELL 2667 | 358.0843 | -26.1324 | 357.438238 | -26.410641 | 347.261091 | -23.090967 | 33.89369276 | -76.76238411 | 64.8814 | 55725.7013773148 | 2011-06-13 16:49:59 | 55726.9814351852 | 2011-06-14 23:33:16 | 806029040 | 51.7936 | 50 | 51.7936 | 51.8161 | 0 | 51.8016 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.6427 | 43.6427 | 110.5818 | 1 | PROCESSED | 57602.3116319444 | 2016-08-02 07:28:45 | 55652 | 2011-04-01 00:00:00 | 55757.7024652778 | 2011-07-15 16:51:33 | 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/ver3.0/806029040/ | Quick Look | ![]() |
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168 | COMA OUTSKIRTS1 | 196.4834 | 28.9037 | 195.885803 | 29.171019 | 182.42683 | 32.834582 | 62.80265316 | 86.34142243 | 115.9997 | 55900.1880092593 | 2011-12-05 04:30:44 | 55901.4341203704 | 2011-12-06 10:25:08 | 806020010 | 48.334 | 50 | 48.334 | 48.334 | 0 | 48.334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.2514 | 42.2514 | 107.6538 | 0 | PROCESSED | 57604.0541898148 | 2016-08-04 01:18:02 | 56282 | 2012-12-21 00:00:00 | 55914.2892013889 | 2011-12-19 06:56:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806020010/ | Quick Look | ![]() |
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169 | COMA OUTSKIRTS4 | 193.3444 | 28.9037 | 192.738609 | 29.174872 | 179.533604 | 31.586326 | 109.48887466 | 88.17367696 | 116.0002 | 55902.7178125 | 2011-12-07 17:13:39 | 55903.9105324074 | 2011-12-08 21:51:10 | 806023010 | 51.6563 | 50 | 51.6643 | 51.6563 | 0 | 51.6713 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.0198 | 49.0198 | 103.0419 | 1 | PROCESSED | 57604.0840972222 | 2016-08-04 02:01:06 | 56284 | 2012-12-23 00:00:00 | 55915.2433449074 | 2011-12-20 05:50:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806023010/ | Quick Look | ![]() |
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170 | COMA E4 | 196.1292 | 27.8947 | 195.52895 | 28.162497 | 182.637315 | 31.793754 | 48.48781449 | 87.00057059 | 279.9984 | 55729.6868287037 | 2011-06-17 16:29:02 | 55730.3355671296 | 2011-06-18 08:03:13 | 806033010 | 20.2023 | 20 | 20.2023 | 20.2103 | 0 | 20.2183 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.516 | 20.516 | 56.0419 | 1 | PROCESSED | 57602.3427199074 | 2016-08-02 08:13:31 | 55652 | 2011-04-01 00:00:00 | 55770.1680092593 | 2011-07-28 04:01:56 | 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/ver3.0/806033010/ | Quick Look | ![]() |
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171 | BEYOND VIRGO 1 | 187.7129 | 16.0953 | 187.082675 | 16.371354 | 180.479874 | 17.795652 | 278.48728746 | 77.9786094 | 118.4704 | 55905.1491666667 | 2011-12-10 03:34:48 | 55905.8431828704 | 2011-12-10 20:14:11 | 806060010 | 22.2598 | 20 | 22.2678 | 22.2678 | 0 | 22.2598 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.63 | 20.63 | 59.9539 | 1 | PROCESSED | 57604.1022569444 | 2016-08-04 02:27:15 | 56284 | 2012-12-23 00:00:00 | 55917.0698958333 | 2011-12-22 01:40:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806060010/ | Quick Look | ![]() |
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172 | BEYOND VIRGO 2 | 187.7135 | 16.3643 | 187.083459 | 16.640353 | 180.363309 | 18.040696 | 277.98453264 | 78.22684296 | 118.4711 | 55905.8436574074 | 2011-12-10 20:14:52 | 55906.3980439815 | 2011-12-11 09:33:11 | 806061010 | 21.4115 | 20 | 21.4275 | 21.4115 | 0 | 21.4335 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.1816 | 19.1816 | 47.872 | 1 | PROCESSED | 57604.0951041667 | 2016-08-04 02:16:57 | 56284 | 2012-12-23 00:00:00 | 55917.0723842593 | 2011-12-22 01:44:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806061010/ | Quick Look | ![]() |
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173 | BEYOND VIRGO 6 | 187.7152 | 17.4312 | 187.085892 | 17.70725 | 179.897096 | 19.011602 | 275.76419982 | 79.20143703 | 118.777 | 55919.8968287037 | 2011-12-24 21:31:26 | 55920.9286574074 | 2011-12-25 22:17:16 | 806065010 | 39.5769 | 40 | 39.6169 | 39.5769 | 0 | 39.6169 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 33.7703 | 33.7703 | 89.136 | 2 | PROCESSED | 57604.2337962963 | 2016-08-04 05:36:40 | 56339 | 2013-02-16 00:00:00 | 55972.6645833333 | 2012-02-15 15:57:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806065010/ | Quick Look | ![]() |
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174 | LOCK-365 | 161.9095 | 57.7105 | 161.128548 | 57.974475 | 136.113511 | 45.200495 | 149.74973686 | 52.48617693 | 106.5217 | 55897.0768981482 | 2011-12-02 01:50:44 | 55900.1780439815 | 2011-12-05 04:16:23 | 806077010 | 149.9102 | 150 | 149.9422 | 149.9102 | 0 | 149.9422 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131.1259 | 131.1259 | 267.9076 | 0 | PROCESSED | 57604.1079050926 | 2016-08-04 02:35:23 | 56065 | 2012-05-18 00:00:00 | 55914.3640393518 | 2011-12-19 08:44:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806077010/ | Quick Look | ![]() |
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175 | RCS051838-4324.9 | 79.6593 | -43.4168 | 79.277976 | -43.467716 | 71.171582 | -66.18535 | 248.71475233 | -34.61566895 | 286.4929 | 56016.4337268518 | 2012-03-30 10:24:34 | 56018.0001388889 | 2012-04-01 00:00:12 | 806083010 | 67.6666 | 75 | 67.6906 | 67.6666 | 0 | 67.6906 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.511 | 57.511 | 135.2938 | 1 | PROCESSED | 57605.0718402778 | 2016-08-05 01:43:27 | 56399 | 2013-04-17 00:00:00 | 56027.1518287037 | 2012-04-10 03:38:38 | 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 | C | 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/ver3.0/806083010/ | Quick Look | ![]() |
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176 | A3526 | 191.7105 | -40.5689 | 191.023079 | -40.2959 | 208.274178 | -32.365083 | 301.98862911 | 22.29443097 | 109.9992 | 55942.9777314815 | 2012-01-16 23:27:56 | 55943.2362847222 | 2012-01-17 05:40:15 | 806086010 | 13.6391 | 12 | 13.6471 | 13.6471 | 0 | 13.6391 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.41 | 11.41 | 22.3279 | 0 | PROCESSED | 57604.3734606482 | 2016-08-04 08:57:47 | 56352 | 2013-03-01 00:00:00 | 55985.0806944444 | 2012-02-28 01:56:12 | 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/ver3.0/806086010/ | Quick Look | ![]() |
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177 | ABELL 426 SW2 | 49.3858 | 41.1787 | 48.562066 | 40.995997 | 58.067168 | 22.136253 | 150.39892317 | -13.77223683 | 94.9997 | 55800.6450115741 | 2011-08-27 15:28:49 | 55800.8411111111 | 2011-08-27 20:11:12 | 806100010 | 9.0043 | 10 | 9.0043 | 9.0123 | 0 | 9.0203 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.933 | 8.933 | 16.934 | 0 | PROCESSED | 57602.9794791667 | 2016-08-02 23:30:27 | 55652 | 2011-04-01 00:00:00 | 55818.1552083333 | 2011-09-14 03:43:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806100010/ | Quick Look | ![]() |
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178 | ABELL 426 SW4 | 48.8197 | 40.8139 | 47.99987 | 40.629138 | 57.514249 | 21.906179 | 150.23286022 | -14.31045471 | 88.4993 | 55801.606724537 | 2011-08-28 14:33:41 | 55801.8501388889 | 2011-08-28 20:24:12 | 806104010 | 13.203 | 10 | 13.203 | 13.203 | 0 | 13.203 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.335 | 13.335 | 21.0079 | 0 | PROCESSED | 57602.9897685185 | 2016-08-02 23:45:16 | 55652 | 2011-04-01 00:00:00 | 55826.0785763889 | 2011-09-22 01:53:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806104010/ | Quick Look | ![]() |
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179 | ABELL 426 SW5.5 | 48.3936 | 40.5388 | 47.576679 | 40.352499 | 57.096428 | 21.733914 | 150.10390207 | -14.71606913 | 88.4991 | 55802.4900694445 | 2011-08-29 11:45:42 | 55802.8161458333 | 2011-08-29 19:35:15 | 806107010 | 15.1951 | 15 | 15.1951 | 15.1991 | 0 | 15.2121 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.8247 | 14.8247 | 28.17 | 0 | PROCESSED | 57603.0002083333 | 2016-08-03 00:00:18 | 55652 | 2011-04-01 00:00:00 | 55826.144224537 | 2011-09-22 03:27:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806107010/ | Quick Look | ![]() |
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180 | ABELL 426 SW7 | 47.984 | 40.268 | 47.169889 | 40.080231 | 56.691635 | 21.563368 | 149.97996332 | -15.11138755 | 88.498 | 55803.3012037037 | 2011-08-30 07:13:44 | 55803.5903935185 | 2011-08-30 14:10:10 | 806110010 | 10.409 | 10 | 10.409 | 10.409 | 0 | 10.409 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.72 | 9.72 | 24.9599 | 0 | PROCESSED | 57603.007662037 | 2016-08-03 00:11:02 | 55652 | 2011-04-01 00:00:00 | 55826.1493287037 | 2011-09-22 03:35:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806110010/ | Quick Look | ![]() |
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181 | ABELL 426 SE3 | 50.6611 | 40.9157 | 49.835576 | 40.737712 | 58.985501 | 21.618486 | 151.37300481 | -13.45928131 | 89.561 | 55798.1679398148 | 2011-08-25 04:01:50 | 55798.4321990741 | 2011-08-25 10:22:22 | 806114010 | 11.7919 | 10 | 11.7999 | 11.7919 | 0 | 11.7999 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.2468 | 9.2468 | 22.8239 | 1 | PROCESSED | 57602.9457407407 | 2016-08-02 22:41:52 | 55652 | 2011-04-01 00:00:00 | 55855.1445949074 | 2011-10-21 03:28:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806114010/ | Quick Look | ![]() |
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182 | ABELL 426 SE3.5 | 50.7904 | 40.8069 | 49.965238 | 40.629396 | 59.055043 | 21.487263 | 151.51904657 | -13.49435734 | 89.5614 | 55798.4325347222 | 2011-08-25 10:22:51 | 55798.7085763889 | 2011-08-25 17:00:21 | 806115010 | 11.9045 | 10 | 11.9125 | 11.9045 | 0 | 11.9205 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.3326 | 11.3326 | 23.8479 | 0 | PROCESSED | 57602.9521643518 | 2016-08-02 22:51:07 | 55652 | 2011-04-01 00:00:00 | 55855.1551157407 | 2011-10-21 03:43:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806115010/ | Quick Look | ![]() |
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183 | ABELL 426 NNE1 | 50.001 | 41.7793 | 49.17162 | 41.598852 | 58.726624 | 22.584898 | 150.45648036 | -13.01724466 | 60.4921 | 55803.8286805556 | 2011-08-30 19:53:18 | 55804.0543171296 | 2011-08-31 01:18:13 | 806135010 | 11.392 | 10 | 11.392 | 11.392 | 0 | 11.392 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.824 | 9.824 | 19.4879 | 0 | PROCESSED | 57603.0136574074 | 2016-08-03 00:19:40 | 55652 | 2011-04-01 00:00:00 | 55830.2051273148 | 2011-09-26 04:55:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806135010/ | Quick Look | ![]() |
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184 | ABELL 426 NNE4 | 50.2584 | 42.5938 | 49.422813 | 42.414295 | 59.170643 | 23.314758 | 150.15840734 | -12.23290919 | 60.4999 | 55805.0005902778 | 2011-09-01 00:00:51 | 55805.2398263889 | 2011-09-01 05:45:21 | 806140010 | 11.8082 | 10 | 11.8082 | 11.8082 | 0 | 11.8082 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.2361 | 7.2361 | 20.656 | 1 | PROCESSED | 57603.0290509259 | 2016-08-03 00:41:50 | 55652 | 2011-04-01 00:00:00 | 55871.8764583333 | 2011-11-06 21:02:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806140010/ | Quick Look | ![]() |
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185 | ABELL 426 NNE4.5 | 50.2947 | 42.7325 | 49.458059 | 42.553128 | 59.240445 | 23.440644 | 150.10266361 | -12.10259839 | 60.4962 | 55806.265 | 2011-09-02 06:21:36 | 55806.5613078704 | 2011-09-02 13:28:17 | 806141010 | 11.085 | 10 | 11.085 | 11.085 | 0 | 11.085 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.0954 | 11.0954 | 25.5959 | 1 | PROCESSED | 57603.0357060185 | 2016-08-03 00:51:25 | 55652 | 2011-04-01 00:00:00 | 55845.2700578704 | 2011-10-11 06:28:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806141010/ | Quick Look | ![]() |
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186 | ABELL 426 NNE5 | 50.3399 | 42.8692 | 49.502189 | 42.689995 | 59.316492 | 23.562815 | 150.05355099 | -11.97038799 | 60.497 | 55806.5616898148 | 2011-09-02 13:28:50 | 55806.8931944444 | 2011-09-02 21:26:12 | 806142010 | 16.3359 | 15 | 16.3471 | 16.3359 | 0 | 16.3359 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.0342 | 17.0342 | 28.638 | 0 | PROCESSED | 57603.0391898148 | 2016-08-03 00:56:26 | 55652 | 2011-04-01 00:00:00 | 55845.258900463 | 2011-10-11 06:12:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806142010/ | Quick Look | ![]() |
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187 | A3581_CEN | 211.9083 | -27.0199 | 211.193684 | -26.782616 | 219.008869 | -13.266139 | 323.17769244 | 32.83870198 | 117.8993 | 56308.5541782407 | 2013-01-16 13:18:01 | 56310.7078356482 | 2013-01-18 16:59:17 | 807026010 | 80.408 | 80 | 80.416 | 80.416 | 0 | 80.408 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.1715 | 70.1715 | 186.0419 | 1 | PROCESSED | 57608.5784259259 | 2016-08-08 13:52:56 | 56711 | 2014-02-23 00:00:00 | 56345.6637384259 | 2013-02-22 15:55:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070064 | We propose to study the metallicity of Abell 3581 to the outer region beyond 0.5 r180. Abell 3581 is a very useful system for investigating the history of the chemical evolution of groups and clusters, because the temperature of the intra-cluster medium is about 1.7 keV, which is intermediate between groups and clusters of galaxies. Suzaku will enable us to measure for the first time the metal distributions to such outer regions of the clusters, because of the significantly lower background level and higher sensitivity below ~1 keV. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 7 | AO7 | SEARCH FOR THE METALLICITY OF ABELL 3581 TO THE OUTER REGION BEYOND 0.5 R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807026010/ | Quick Look | ![]() |
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188 | A2061_2 | 230.6122 | 30.8661 | 230.100044 | 31.043682 | 216.595507 | 47.269453 | 48.57175305 | 56.92431824 | 121.1842 | 56307.485625 | 2013-01-15 11:39:18 | 56308.5460185185 | 2013-01-16 13:06:16 | 807030010 | 41.788 | 40 | 41.788 | 41.788 | 0 | 41.788 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.7529 | 37.7529 | 91.6018 | 1 | PROCESSED | 57608.5263888889 | 2016-08-08 12:38:00 | 56707 | 2014-02-19 00:00:00 | 56338.5482291667 | 2013-02-15 13:09:27 | 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/ver3.0/807030010/ | Quick Look | ![]() |
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189 | FG04 | 121.8798 | 33.9978 | 121.078663 | 34.143156 | 116.761327 | 13.47104 | 187.39667673 | 29.69857824 | 274.999 | 56053.6835648148 | 2012-05-06 16:24:20 | 56053.9411921296 | 2012-05-06 22:35:19 | 807053010 | 10.821 | 10 | 10.821 | 10.821 | 0 | 10.821 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0766 | 11.0766 | 22.2559 | 0 | PROCESSED | 57605.3537268518 | 2016-08-05 08:29:22 | 56435 | 2013-05-23 00:00:00 | 56068.6337152778 | 2012-05-21 15:12:33 | 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/ver3.0/807053010/ | Quick Look | ![]() |
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190 | RXJ1416.4+2315 | 214.0475 | 23.1701 | 213.473378 | 23.401516 | 202.507315 | 34.451007 | 25.95045598 | 70.44211392 | 293.1172 | 56123.5919675926 | 2012-07-15 14:12:26 | 56124.3335300926 | 2012-07-16 08:00:17 | 807065010 | 23.7192 | 120 | 23.7272 | 23.7192 | 0 | 23.7272 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.6028 | 22.6028 | 64.0639 | 1 | PROCESSED | 57606.624537037 | 2016-08-06 14:59:20 | 56598 | 2013-11-02 00:00:00 | 56144.9996180556 | 2012-08-05 23:59:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071514 | Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID BUOTE | USA | 7 | AO7 | RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065010/ | Quick Look | ![]() |
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191 | NGC 5044 NORTH 30' | 199.0992 | -15.8941 | 198.433238 | -15.630477 | 203.627041 | -7.241957 | 311.67530339 | 46.55349501 | 110.0017 | 55220.5889814815 | 2010-01-24 14:08:08 | 55222.2571064815 | 2010-01-26 06:10:14 | 804013010 | 62.8482 | 60 | 62.8562 | 62.8482 | 0 | 62.8562 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.5926 | 44.5926 | 144.0998 | 1 | PROCESSED | 57550.396099537 | 2016-06-11 09:30:23 | 55602 | 2011-02-10 00:00:00 | 55235.338587963 | 2010-02-08 08:07:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040013 | Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804013010/ | Quick Look | ![]() |
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192 | ANTLIA E4 | 158.9815 | -35.3293 | 158.412243 | -35.069878 | 177.109135 | -40.308725 | 274.02289995 | 19.82417732 | 279.0004 | 56094.1885532407 | 2012-06-16 04:31:31 | 56095.3688888889 | 2012-06-17 08:51:12 | 807069010 | 46.5031 | 45 | 46.5031 | 46.5195 | 0 | 46.5111 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.6185 | 38.6185 | 101.9699 | 0 | PROCESSED | 57605.7108564815 | 2016-08-05 17:03:38 | 56477 | 2013-07-04 00:00:00 | 56111.0445023148 | 2012-07-03 01:04:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807069010/ | Quick Look | ![]() |
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193 | ABELL 2597 | 351.5123 | -12.2071 | 350.862263 | -12.482246 | 347.371921 | -7.852378 | 65.46064183 | -65.03980804 | 250.0004 | 56263.5374884259 | 2012-12-02 12:53:59 | 56264.7744907407 | 2012-12-03 18:35:16 | 807073030 | 50.2983 | 50 | 50.3063 | 50.2983 | 0 | 50.2983 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.3364 | 42.3364 | 106.8558 | 0 | PROCESSED | 57608.190625 | 2016-08-08 04:34:30 | 56018 | 2012-04-01 00:00:00 | 56279.6896180556 | 2012-12-18 16:33:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073030/ | Quick Look | ![]() |
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194 | RCS022456-0348.8 | 36.2382 | -3.8143 | 35.608784 | -4.039767 | 32.599151 | -17.199331 | 170.77871975 | -57.71972182 | 253.341 | 56324.4414814815 | 2013-02-01 10:35:44 | 56325.9579282407 | 2013-02-02 22:59:25 | 807078010 | 50.8118 | 49 | 50.8227 | 50.8147 | 0 | 50.8118 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.195 | 46.195 | 131.0078 | 0 | PROCESSED | 57610.5290509259 | 2016-08-10 12:41:50 | 56711 | 2014-02-23 00:00:00 | 56345.5401967593 | 2013-02-22 12:57:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | 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 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807078010/ | Quick Look | ![]() |
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195 | VIRGO W2 | 187.236 | 12.0886 | 186.602607 | 12.36495 | 181.750104 | 13.952177 | 282.50975725 | 74.06175724 | 285.4993 | 56110.9396180556 | 2012-07-02 22:33:03 | 56111.2640509259 | 2012-07-03 06:20:14 | 807095010 | 12.4847 | 10 | 12.4927 | 12.4847 | 0 | 12.5007 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.3335 | 12.3335 | 28.0259 | 1 | PROCESSED | 57606.5414583333 | 2016-08-06 12:59:42 | 56018 | 2012-04-01 00:00:00 | 56139.0870717593 | 2012-07-31 02:05:23 | 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/ver3.0/807095010/ | Quick Look | ![]() |
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196 | VIRGO W10 | 185.0059 | 10.7782 | 184.369631 | 11.055649 | 180.246148 | 11.867747 | 277.10217205 | 72.05623626 | 99.9987 | 56276.4098263889 | 2012-12-15 09:50:09 | 56276.9828935185 | 2012-12-15 23:35:22 | 807103010 | 27.9677 | 24 | 27.9677 | 27.9677 | 0 | 27.9677 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.7604 | 25.7604 | 49.5039 | 0 | PROCESSED | 57608.287974537 | 2016-08-08 06:54:41 | 56018 | 2012-04-01 00:00:00 | 56315.5187037037 | 2013-01-23 12:26:56 | 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/ver3.0/807103010/ | Quick Look | ![]() |
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197 | VIRGO N3 | 187.7014 | 13.8904 | 187.06968 | 14.166465 | 181.417647 | 15.781989 | 281.91864672 | 75.91344863 | 313.997 | 56098.2612037037 | 2012-06-20 06:16:08 | 56098.5176388889 | 2012-06-20 12:25:24 | 807108010 | 12.266 | 10 | 12.266 | 12.266 | 0 | 12.266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6997 | 12.6997 | 22.1399 | 1 | PROCESSED | 57605.7217013889 | 2016-08-05 17:19:15 | 56018 | 2012-04-01 00:00:00 | 56214.9569907407 | 2012-10-14 22:58:04 | 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/ver3.0/807108010/ | Quick Look | ![]() |
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198 | VIRGO S11 | 187.5325 | 8.9432 | 186.897427 | 9.219378 | 183.326019 | 11.193327 | 286.45864166 | 71.13028831 | 122.0016 | 56269.7576851852 | 2012-12-08 18:11:04 | 56270.1612384259 | 2012-12-09 03:52:11 | 807125010 | 17.2823 | 16 | 17.2823 | 17.2823 | 0 | 17.2823 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.5627 | 18.5627 | 34.82 | 0 | PROCESSED | 57608.2142013889 | 2016-08-08 05:08:27 | 56018 | 2012-04-01 00:00:00 | 56336.4686111111 | 2013-02-13 11:14:48 | 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/ver3.0/807125010/ | Quick Look | ![]() |
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199 | VIRGO S16 | 187.3813 | 7.0531 | 186.744958 | 7.329373 | 183.956748 | 9.401927 | 287.41240339 | 69.26194594 | 122.0008 | 56271.6277314815 | 2012-12-10 15:03:56 | 56272.0709722222 | 2012-12-11 01:42:12 | 807130010 | 21.6482 | 18 | 21.6482 | 21.6482 | 0 | 21.6482 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.3081 | 21.3081 | 38.2679 | 1 | PROCESSED | 57608.2349652778 | 2016-08-08 05:38:21 | 56018 | 2012-04-01 00:00:00 | 56330.5084837963 | 2013-02-07 12:12:13 | 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/ver3.0/807130010/ | Quick Look | ![]() |
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200 | A401EAST | 45.0348 | 13.3366 | 44.348124 | 13.13869 | 46.452106 | -3.5684 | 164.66710088 | -38.88860633 | 71.9996 | 56530.5043055556 | 2013-08-26 12:06:12 | 56531.6841782407 | 2013-08-27 16:25:13 | 808006010 | 51.6628 | 50 | 51.6868 | 51.6628 | 0 | 51.6868 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.8099 | 47.8099 | 101.9238 | 1 | PROCESSED | 57612.4270138889 | 2016-08-12 10:14:54 | 56956 | 2014-10-26 00:00:00 | 56587.515474537 | 2013-10-22 12:22:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHITAKA ISHISAKI | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808006010/ | Quick Look | ![]() |
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201 | COMA SUBHALO3 | 193.9804 | 27.7549 | 193.374568 | 28.025359 | 180.724315 | 30.814588 | 65.39722549 | 88.82429581 | 314.9967 | 56453.0272569444 | 2013-06-10 00:39:15 | 56453.5912384259 | 2013-06-10 14:11:23 | 808021010 | 24.0441 | 20 | 24.0521 | 24.0441 | 0 | 24.0521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.5334 | 25.5334 | 48.6979 | 0 | PROCESSED | 57611.5202199074 | 2016-08-11 12:29:07 | 56872 | 2014-08-03 00:00:00 | 56506.7633101852 | 2013-08-02 18:19:10 | 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/ver3.0/808021010/ | Quick Look | ![]() |
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202 | COMA NW3 | 194.5571 | 28.6697 | 193.954123 | 28.93948 | 180.77176 | 31.860187 | 79.10101688 | 87.84902047 | 319.997 | 55732.646099537 | 2011-06-20 15:30:23 | 55732.9793865741 | 2011-06-20 23:30:19 | 806040010 | 10.469 | 10 | 10.469 | 10.469 | 0 | 10.469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.1768 | 10.1768 | 28.7899 | 0 | PROCESSED | 57602.3615856482 | 2016-08-02 08:40:41 | 55652 | 2011-04-01 00:00:00 | 55768.2657523148 | 2011-07-26 06:22:41 | 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/ver3.0/806040010/ | Quick Look | ![]() |
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203 | A2255_NW | 258.0206 | 64.3236 | 257.946874 | 64.381524 | 198.635574 | 84.547798 | 94.26240936 | 34.95584628 | 200.0017 | 56613.0157060185 | 2013-11-17 00:22:37 | 56613.9467476852 | 2013-11-17 22:43:19 | 808039010 | 43.7688 | 40 | 43.7688 | 43.7688 | 0 | 43.7688 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.8557 | 41.8557 | 80.4121 | 0 | PROCESSED | 57613.3414814815 | 2016-08-13 08:11:44 | 56991 | 2014-11-30 00:00:00 | 56625.6806481482 | 2013-11-29 16:20:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080047 | We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROKO YOSHIDA | JAP | 8 | AO8 | MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808039010/ | Quick Look | ![]() |
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204 | BULLET-OFFSET2 | 104.4232 | -55.8309 | 104.179615 | -55.762127 | 129.485135 | -77.282926 | 265.86935635 | -21.32349548 | 287.0017 | 56419.6209722222 | 2013-05-07 14:54:12 | 56422.4605439815 | 2013-05-10 11:03:11 | 808056010 | 101.3855 | 100 | 101.3935 | 101.3935 | 0 | 101.3855 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.6767 | 93.6767 | 245.3058 | 2 | PROCESSED | 57611.3171643518 | 2016-08-11 07:36:43 | 56799 | 2014-05-22 00:00:00 | 56433.6998958333 | 2013-05-21 16:47:51 | 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/ver3.0/808056010/ | Quick Look | ![]() |
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205 | ESO318-021 | 163.2697 | -40.3328 | 162.69794 | -40.066534 | 184.394245 | -42.926152 | 279.73310675 | 17.14745123 | 111.1499 | 56639.0964467593 | 2013-12-13 02:18:53 | 56643.3605902778 | 2013-12-17 08:39:15 | 808063010 | 152.2198 | 150 | 152.2198 | 152.2198 | 0 | 152.2198 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132.9733 | 132.9733 | 368.3777 | 4 | PROCESSED | 57613.6558101852 | 2016-08-13 15:44:22 | 57050 | 2015-01-28 00:00:00 | 56680.7667476852 | 2014-01-23 18:24:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAVID BUOTE | USA | 8 | AO8 | THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808063010/ | Quick Look | ![]() |
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206 | RXJ1416.4+2315 | 214.0623 | 23.3458 | 213.488767 | 23.577175 | 202.437112 | 34.617457 | 26.46691952 | 70.47697816 | 292.671 | 56496.6431712963 | 2013-07-23 15:26:10 | 56499.3349074074 | 2013-07-26 08:02:16 | 808064010 | 122.9317 | 120 | 122.9317 | 122.9317 | 0 | 122.9317 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116.8226 | 116.8226 | 232.5474 | 2 | PROCESSED | 57612.032650463 | 2016-08-12 00:47:01 | 56953 | 2014-10-23 00:00:00 | 56587.4880671296 | 2013-10-22 11:42:49 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081511 | Our preliminary analysis of AO7 XIS data of the fossil cluster RXJ 1416.4+2315 does not find evidence for the gas clumping invoked to explain the flat entropy profiles and large gas fractions found near r_vir in several nearby clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation as we found previously for the fossil group/cluster RXJ 1159+5531, which may reflect that hydrostatic equilibrium is very accurate in these highly evolved fossil systems. Therefore, we propose a Suzaku observation in a different azimuthal direction to double the azimuthal coverage at r_vir (from ~30% to ~60%) in order to test for the presence of azimuthal ICM variations expected for clusters that grow by accretion along large-scale filaments. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAVID BUOTE | USA | 8 | AO8 | VERIFYING RELAXED ICM AT THE VIRIAL RADIUS IN A FOSSIL GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808064010/ | Quick Look | ![]() |
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207 | MKW-N2 | 181.1507 | 2.5267 | 180.510236 | 2.805064 | 180.047061 | 2.775514 | 276.44275792 | 62.96433079 | 120.2659 | 56663.6701967593 | 2014-01-06 16:05:05 | 56666.0195023148 | 2014-01-09 00:28:05 | 808067010 | 99.7883 | 100 | 99.7883 | 99.7883 | 0 | 99.7883 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.9362 | 99.9362 | 202.9537 | 4 | PROCESSED | 57613.8221643518 | 2016-08-13 19:43:55 | 57096 | 2015-03-15 00:00:00 | 56730.5704166667 | 2014-03-14 13:41:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808067010/ | Quick Look | ![]() |
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208 | A133_FIELD_2 | 15.4723 | -21.5865 | 14.860654 | -21.855252 | 5.175152 | -25.865615 | 146.72727626 | -83.96930246 | 231.9996 | 56646.6689583333 | 2013-12-20 16:03:18 | 56647.8294212963 | 2013-12-21 19:54:22 | 808082010 | 50.6406 | 50 | 50.6646 | 50.6566 | 0 | 50.6406 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.4338 | 46.4338 | 100.2559 | 1 | PROCESSED | 57613.6561921296 | 2016-08-13 15:44:55 | 57061 | 2015-02-08 00:00:00 | 56695.6286689815 | 2014-02-07 15:05:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808082010/ | Quick Look | ![]() |
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209 | ABELL 1689 (OFFSET) | 198.1816 | -1.2688 | 197.539227 | -1.003818 | 197.250037 | 5.95631 | 314.01012466 | 61.14421574 | 293.5484 | 56470.3775578704 | 2013-06-27 09:03:41 | 56473.3751273148 | 2013-06-30 09:00:11 | 808089010 | 105.7518 | 396 | 105.7598 | 105.7518 | 0 | 105.7518 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95.0477 | 95.0477 | 258.9556 | 4 | PROCESSED | 57611.7314930556 | 2016-08-11 17:33:21 | 56383 | 2013-04-01 00:00:00 | 56523.7467708333 | 2013-08-19 17:55:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089010/ | Quick Look | ![]() |
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210 | ABELL 1689 (OFFSET) | 198.1818 | -1.2687 | 197.539427 | -1.003718 | 197.250185 | 5.956479 | 314.01056832 | 61.14428006 | 293.5484 | 56473.3751388889 | 2013-06-30 09:00:12 | 56475.3022916667 | 2013-07-02 07:15:18 | 808089020 | 67.8003 | 396 | 67.8083 | 67.8003 | 0 | 67.8083 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.9649 | 60.9649 | 166.4698 | 5 | PROCESSED | 57611.6944907407 | 2016-08-11 16:40:04 | 56383 | 2013-04-01 00:00:00 | 56491.6594675926 | 2013-07-18 15:49:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089020/ | Quick Look | ![]() |
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211 | A2877-NORTH | 17.5135 | -45.1865 | 16.956259 | -45.452478 | 352.566996 | -47.330769 | 292.51418745 | -71.56330592 | 266.5006 | 56649.9225810185 | 2013-12-23 22:08:31 | 56651.7884027778 | 2013-12-25 18:55:18 | 808102010 | 72.629 | 70 | 72.637 | 72.629 | 0 | 72.645 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.2641 | 69.2641 | 161.1857 | 0 | PROCESSED | 57613.7012615741 | 2016-08-13 16:49:49 | 57033 | 2015-01-11 00:00:00 | 56665.7969097222 | 2014-01-08 19:07:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082014 | We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BHARADWAJ VIJAYSARATHY | EUR | 8 | AO8 | INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808102010/ | Quick Look | ![]() |
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212 | VIRGO E12 | 191.1366 | 14.3009 | 190.509391 | 14.574322 | 184.414539 | 17.520905 | 295.44935056 | 77.07241976 | 285.0012 | 56485.8160185185 | 2013-07-12 19:35:04 | 56486.2634143518 | 2013-07-13 06:19:19 | 808127010 | 20.5979 | 20 | 20.6139 | 20.5979 | 0 | 20.6139 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.42 | 17.42 | 38.6479 | 0 | PROCESSED | 57611.9024768518 | 2016-08-11 21:39:34 | 56383 | 2013-04-01 00:00:00 | 56498.6479976852 | 2013-07-25 15:33:07 | 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/ver3.0/808127010/ | Quick Look | ![]() |
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213 | THE MOON | 142.9426 | 9.1926 | 142.274308 | 9.413777 | 142.279358 | -5.167487 | 223.99367078 | 39.68355518 | 285.4008 | 56784.5840162037 | 2014-05-07 14:00:59 | 56784.7155555556 | 2014-05-07 17:10:24 | 809001090 | 4.7558 | 45 | 4.7558 | 4.7558 | 0 | 4.7558 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.6674 | 4.6674 | 11.358 | 0 | PROCESSED | 57615.0740277778 | 2016-08-15 01:46:36 | 57162 | 2015-05-20 00:00:00 | 56796.5977546296 | 2014-05-19 14:20:46 | 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/ver3.0/809001090/ | Quick Look | ![]() |
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214 | THE MOON | 29.2087 | 11.3221 | 28.541439 | 11.078317 | 31.138176 | -0.585907 | 147.49986562 | -48.40533826 | 73.8007 | 56857.4028472222 | 2014-07-19 09:40:06 | 56857.5265856482 | 2014-07-19 12:38:17 | 809001170 | 5.6621 | 45 | 5.6701 | 5.6621 | 0 | 5.6701 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4102314815 | 2016-08-15 09:50:44 | 57239 | 2015-08-05 00:00:00 | 56869.612974537 | 2014-07-31 14:42:41 | 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/ver3.0/809001170/ | Quick Look | ![]() |
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215 | THE MOON | 30.7597 | 12.0224 | 30.089346 | 11.782342 | 32.8056 | -0.451848 | 149.17525918 | -47.16814979 | 73.8003 | 56857.5278009259 | 2014-07-19 12:40:02 | 56857.5974189815 | 2014-07-19 14:20:17 | 809001180 | 3.4386 | 45 | 3.4466 | 3.4386 | 0 | 3.4546 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4120601852 | 2016-08-15 09:53:22 | 57239 | 2015-08-05 00:00:00 | 56869.6134953704 | 2014-07-31 14:43:26 | 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/ver3.0/809001180/ | Quick Look | ![]() |
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216 | THE MOON | 138.5418 | 11.2369 | 137.863994 | 11.444435 | 137.511885 | -4.561937 | 219.19555273 | 36.72863641 | 105.699 | 56975.1999768518 | 2014-11-14 04:47:58 | 56975.3237615741 | 2014-11-14 07:46:13 | 809001200 | 3.3796 | 45 | 3.3796 | 3.3796 | 0 | 3.3796 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7701041667 | 2016-08-16 18:28:57 | 57358 | 2015-12-02 00:00:00 | 56992.4114699074 | 2014-12-01 09:52:31 | 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/ver3.0/809001200/ | Quick Look | ![]() |
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217 | THE MOON | 141.4013 | 10.2837 | 140.728619 | 10.500242 | 140.487309 | -4.611146 | 221.84323525 | 38.83162783 | 105.6986 | 56975.4499305556 | 2014-11-14 10:47:54 | 56975.5834143518 | 2014-11-14 14:00:07 | 809001220 | 4.2552 | 45 | 4.2552 | 4.2632 | 0 | 4.2632 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7742592593 | 2016-08-16 18:34:56 | 57358 | 2015-12-02 00:00:00 | 56992.4140625 | 2014-12-01 09:56:15 | 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/ver3.0/809001220/ | Quick Look | ![]() |
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218 | THE MOON | 145.8331 | 9.4283 | 145.16599 | 9.657722 | 144.909334 | -4.019227 | 225.49397113 | 42.31232043 | 105.6985 | 56975.8485300926 | 2014-11-14 20:21:53 | 56975.9376388889 | 2014-11-14 22:30:12 | 809001250 | 4.244 | 45 | 4.244 | 4.308 | 0 | 4.324 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7786574074 | 2016-08-16 18:41:16 | 57358 | 2015-12-02 00:00:00 | 56992.4181828704 | 2014-12-01 10:02:11 | 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/ver3.0/809001250/ | Quick Look | ![]() |
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219 | THE MOON | 335.3702 | -6.281 | 334.716283 | -6.533427 | 334.875812 | 3.693556 | 56.37004308 | -48.74864005 | 248.3898 | 56990.2098148148 | 2014-11-29 05:02:08 | 56990.3474768518 | 2014-11-29 08:20:22 | 809001310 | 6.2242 | 45 | 6.2242 | 6.2242 | 0 | 6.2242 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4106481482 | 2016-08-17 09:51:20 | 57415 | 2016-01-28 00:00:00 | 57002.4438541667 | 2014-12-11 10:39:09 | 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/ver3.0/809001310/ | Quick Look | ![]() |
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220 | THE MOON | 340.8235 | -5.0226 | 340.1744 | -5.285051 | 340.39289 | 2.857324 | 63.09935011 | -52.32405661 | 251.0714 | 56990.6104513889 | 2014-11-29 14:39:03 | 56990.733587963 | 2014-11-29 17:36:22 | 809001340 | 6.3566 | 45 | 6.3566 | 6.3566 | 0 | 6.3566 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4124537037 | 2016-08-17 09:53:56 | 57415 | 2016-01-28 00:00:00 | 57007.4026041667 | 2014-12-16 09:39:45 | 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/ver3.0/809001340/ | Quick Look | ![]() |
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221 | THE MOON | 342.4216 | -4.2139 | 341.77438 | -4.478841 | 342.17578 | 3.00393 | 65.81829296 | -53.01188957 | 247.9474 | 56990.7354513889 | 2014-11-29 17:39:03 | 56990.8683101852 | 2014-11-29 20:50:22 | 809001350 | 6.3196 | 45 | 6.3196 | 6.3196 | 0 | 6.3196 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4131018518 | 2016-08-17 09:54:52 | 57415 | 2016-01-28 00:00:00 | 57006.4014699074 | 2014-12-15 09:38:07 | 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/ver3.0/809001350/ | Quick Look | ![]() |
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222 | A1413 | 178.8303 | 23.6485 | 178.18646 | 23.926767 | 169.076487 | 21.133974 | 225.18767075 | 76.86550896 | 123.0348 | 53689.8362847222 | 2005-11-15 20:04:15 | 53692.5939699074 | 2005-11-18 14:15:19 | 800001010 | 107.8672 | 100 | 107.8672 | 108.0032 | 107.9472 | 107.9103 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 102.4315 | 102.4315 | 238.2397 | 7 | PROCESSED | 57528.0427546296 | 2016-05-20 01:01:34 | 54247 | 2007-05-27 00:00:00 | 54038.1136689815 | 2006-10-30 02:43:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001010 | No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | J. HENRY | JAP | 0 | SWG | CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800001010/ | Quick Look | ![]() |
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223 | FORNAX A WEST LOBE | 50.4184 | -37.1645 | 49.940428 | -37.342839 | 32.47574 | -52.998531 | 240.1258488 | -56.89722719 | 219.7525 | 54092.8700462963 | 2006-12-23 20:52:52 | 54095.6113888889 | 2006-12-26 14:40:24 | 801014010 | 93.3093 | 100 | 93.3093 | 93.3093 | 0 | 93.3093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.3716 | 96.3716 | 236.8358 | 5 | PROCESSED | 57536.4597569444 | 2016-05-28 11:02:03 | 54735 | 2008-09-26 00:00:00 | 54111.6821875 | 2007-01-11 16:22:21 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010029 | We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO TASHIRO | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801014010/ | Quick Look | ![]() |
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224 | A262 E2 | 28.9415 | 35.8688 | 28.205018 | 35.624348 | 39.895398 | 22.433371 | 137.29682221 | -25.20210685 | 249.9999 | 56695.375625 | 2014-02-07 09:00:54 | 56696.1043518518 | 2014-02-08 02:30:16 | 808113010 | 33.0569 | 32 | 33.0609 | 33.0569 | 0 | 33.0649 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8024884259 | 2016-08-13 19:15:35 | 57074 | 2015-02-21 00:00:00 | 56709.7139814815 | 2014-02-21 17:08:08 | 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/ver3.0/808113010/ | Quick Look | ![]() |
225 | A3112BG | 50.3198 | -44.6958 | 49.891219 | -44.874421 | 26.077848 | -59.651808 | 253.38706356 | -55.37551095 | 204.9994 | 57009.69125 | 2014-12-18 16:35:24 | 57010.2550462963 | 2014-12-19 06:07:16 | 809028020 | 18.3545 | 15 | 18.3545 | 18.3545 | 0 | 18.3545 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5354166667 | 2016-08-17 12:51:00 | 57394 | 2016-01-07 00:00:00 | 57027.3975 | 2015-01-05 09:32:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809028020/ | Quick Look | ![]() |
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226 | PKS 0558-504 VIC 1 | 90.9582 | -50.6414 | 90.657059 | -50.637494 | 92.232149 | -74.075703 | 258.29690544 | -27.96668923 | 6.4262 | 56825.0805208333 | 2014-06-17 01:55:57 | 56826.8543518518 | 2014-06-18 20:30:16 | 809034010 | 52.0132 | 60 | 52.0132 | 52.0132 | 0 | 52.0132 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.4874 | 50.4874 | 153.2479 | 0 | PROCESSED | 57615.2996180556 | 2016-08-15 07:11:27 | 57233 | 2015-07-30 00:00:00 | 56867.5608912037 | 2014-07-29 13:27:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090086 | We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAZUHIRO SAKAI | JAP | 9 | AO9 | IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809034010/ | Quick Look | ![]() |
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227 | NGC 953 | 37.7955 | 29.584 | 37.059252 | 29.362946 | 44.923297 | 13.943505 | 147.58231113 | -28.46974369 | 250.5565 | 57059.5397222222 | 2015-02-06 12:57:12 | 57063.4376157407 | 2015-02-10 10:30:10 | 809055010 | 150.8191 | 150 | 150.8191 | 150.8671 | 0 | 150.8671 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6137037037 | 2016-08-17 14:43:44 | 56748 | 2014-04-01 00:00:00 | 57107.4400578704 | 2015-03-26 10:33:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^13 m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAVID BUOTE | USA | 9 | AO9 | THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809055010/ | Quick Look | ![]() |
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228 | FG10 | 163.7228 | 55.3656 | 162.966111 | 55.632252 | 139.04941 | 43.748241 | 151.60913312 | 54.78459511 | 121.1085 | 56973.8939467593 | 2014-11-12 21:27:17 | 56975.0737615741 | 2014-11-14 01:46:13 | 809061010 | 61.1085 | 60 | 61.1085 | 61.2978 | 0 | 61.2978 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7792361111 | 2016-08-16 18:42:06 | 57444 | 2016-02-26 00:00:00 | 57076.4143865741 | 2015-02-23 09:56:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ELENA D'ONGHIA | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809061010/ | Quick Look | ![]() |
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229 | ABELL 2259 | 259.9722 | 27.8097 | 259.476075 | 27.85934 | 255.895749 | 50.75928 | 50.52312942 | 31.25775464 | 109.9997 | 57081.1636458333 | 2015-02-28 03:55:39 | 57082.4113194445 | 2015-03-01 09:52:18 | 809081010 | 42.2203 | 42.5 | 42.2203 | 43.0443 | 0 | 43.1003 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6840509259 | 2016-08-17 16:25:02 | 57465 | 2016-03-18 00:00:00 | 57091.4611226852 | 2015-03-10 11:04:01 | 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/ver3.0/809081010/ | Quick Look | ![]() |
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230 | ABELL 2259 | 260.1067 | 27.5543 | 259.609076 | 27.603301 | 256.126173 | 50.518333 | 50.27658806 | 31.07091189 | 109.9997 | 57083.6006018518 | 2015-03-02 14:24:52 | 57084.7258564815 | 2015-03-03 17:25:14 | 809081030 | 44.2468 | 42.5 | 44.2468 | 44.2548 | 0 | 44.2548 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7027314815 | 2016-08-17 16:51:56 | 57475 | 2016-03-28 00:00:00 | 57107.4892476852 | 2015-03-26 11:44:31 | 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/ver3.0/809081030/ | Quick Look | ![]() |
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231 | IC1262 | 263.2444 | 43.7719 | 262.868526 | 43.80553 | 257.468416 | 66.917452 | 69.53148075 | 32.08557503 | 39.6325 | 56784.7266319444 | 2014-05-07 17:26:21 | 56784.9377777778 | 2014-05-07 22:30:24 | 809103010 | 8.569 | 10 | 8.569 | 8.569 | 0 | 8.569 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.943 | 8.943 | 18.2319 | 0 | PROCESSED | 57615.0791898148 | 2016-08-15 01:54:02 | 57166 | 2015-05-24 00:00:00 | 56800.6274537037 | 2014-05-23 15:03:32 | 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 | B | 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/ver3.0/809103010/ | Quick Look | ![]() |
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232 | NGC 7556 | 348.9407 | -2.3789 | 348.297581 | -2.651844 | 348.895625 | 2.187169 | 76.06549974 | -56.282291 | 247.7522 | 56983.6865972222 | 2014-11-22 16:28:42 | 56984.009837963 | 2014-11-23 00:14:10 | 809109010 | 15.119 | 15 | 15.119 | 15.119 | 0 | 15.119 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8029861111 | 2016-08-16 19:16:18 | 57365 | 2015-12-09 00:00:00 | 57009.4127777778 | 2014-12-18 09:54:24 | 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/ver3.0/809109010/ | Quick Look | ![]() |
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233 | NGC4325 | 185.7751 | 10.6242 | 185.139474 | 10.901318 | 181.016229 | 12.032879 | 279.57257446 | 72.19853871 | 120.2615 | 56997.2271990741 | 2014-12-06 05:27:10 | 56997.680775463 | 2014-12-06 16:20:19 | 809110010 | 17.4681 | 15 | 17.4761 | 17.4681 | 0 | 17.4761 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.8093 | 16.8093 | 39.184 | 0 | PROCESSED | 57617.4727083333 | 2016-08-17 11:20:42 | 57376 | 2015-12-20 00:00:00 | 57010.1165162037 | 2014-12-19 02:47:47 | 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/ver3.0/809110010/ | Quick Look | ![]() |
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234 | M82 N1 | 148.6748 | 70.0409 | 147.627175 | 70.277324 | 118.519213 | 52.349642 | 141.10131259 | 40.27429686 | 283.7057 | 57159.0836921296 | 2015-05-17 02:00:31 | 57160.4702546296 | 2015-05-18 11:17:10 | 809122010 | 59.5055 | 60 | 59.5055 | 59.5055 | 0 | 59.5135 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6721759259 | 2016-08-18 16:07:56 | 57538 | 2016-05-30 00:00:00 | 57171.5244212963 | 2015-05-29 12:35:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091701 | We propose to carry out joint Chandra and Suzaku observations of the starburst galaxy M82. We will search for extended clumps similar to the Northern Cap out to 45 kpc. We will also constrain the density and temperature profiles of the tenuous 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, hydrostatic halo model, shocked clouds in a wind, etc. The excellent Chandra spatial resolution combining with the low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | KA-WAH WONG | USA | 9 | AO9 | SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809122010/ | Quick Look | ![]() |
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235 | ABELL 2255 CENTER | 258.2484 | 64.1467 | 258.17067 | 64.203551 | 200.767912 | 84.543322 | 94.02951141 | 34.88778486 | 111.176 | 55234.3014814815 | 2010-02-07 07:14:08 | 55235.405775463 | 2010-02-08 09:44:19 | 804041010 | 44.5337 | 50 | 44.5337 | 44.5417 | 0 | 44.5417 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43.339 | 43.339 | 95.3759 | 1 | PROCESSED | 57550.5171180556 | 2016-06-11 12:24:39 | 55617 | 2011-02-25 00:00:00 | 55250.1645601852 | 2010-02-23 03:56:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040091 | Suzaku discovered an supra thermal component in the plasma of Abell 3667 which exceeds 13 keV. In order to establish this component in merging clusters, we propose two pointing observations of Abell 2255, which hosts a huge radio halo and a radio relic. With these two pointings, we aim at roughly spotting the location of the supra thermal plasma. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 4 | AO4 | PROBING SUPRA THERMAL PLASMA IN ABELL 2255 WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804041010/ | Quick Look | ![]() |
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236 | OPHIUCHUS CLUSTER 1 | 258.2981 | -23.3868 | 257.539766 | -23.328523 | 259.261866 | -0.380707 | 0.65649186 | 9.12279372 | 88.7031 | 54180.6159953704 | 2007-03-21 14:47:02 | 54181.1398611111 | 2007-03-22 03:21:24 | 801022010 | 24.067 | 15 | 24.075 | 24.067 | 0 | 24.075 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.8213 | 21.8213 | 45.254 | 1 | PROCESSED | 57537.7417476852 | 2016-05-29 17:48:07 | 54736 | 2008-09-27 00:00:00 | 54186.192650463 | 2007-03-27 04:37:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801022010/ | Quick Look | ![]() |
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237 | COMA OUTSKIRTS6 | 193.974 | 28.5108 | 193.369273 | 28.781265 | 180.320045 | 31.486616 | 87.70306179 | 88.30207114 | 115.9975 | 55904.7228703704 | 2011-12-09 17:20:56 | 55905.1452662037 | 2011-12-10 03:29:11 | 806025010 | 21.503 | 20 | 21.503 | 21.503 | 0 | 21.503 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.265 | 20.265 | 36.4719 | 0 | PROCESSED | 57604.0827083333 | 2016-08-04 01:59:06 | 56284 | 2012-12-23 00:00:00 | 55915.2118402778 | 2011-12-20 05:05:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806025010/ | Quick Look | ![]() |
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238 | AWM7 | 43.631 | 41.5933 | 42.82175 | 41.390486 | 53.723626 | 23.815753 | 146.34082925 | -15.61629549 | 90.4997 | 53954.2348842593 | 2006-08-07 05:38:14 | 53954.71625 | 2006-08-07 17:11:24 | 801035010 | 18.9858 | 20 | 18.9858 | 18.9858 | 18.9858 | 18.9858 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.5542 | 17.5542 | 41.588 | 0 | PROCESSED | 57535.2434953704 | 2016-05-27 05:50:38 | 54422 | 2007-11-18 00:00:00 | 54020.7471759259 | 2006-10-12 17:55:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801035010/ | Quick Look | ![]() |
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239 | NGC 4631 | 190.5387 | 32.5478 | 189.929771 | 32.821718 | 174.99352 | 33.703009 | 142.74124336 | 84.2191655 | 139.0678 | 54067.1412615741 | 2006-11-28 03:23:25 | 54068.9133217593 | 2006-11-29 21:55:11 | 801019010 | 81.0761 | 80 | 81.0841 | 81.0761 | 0 | 81.0841 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74.4358 | 74.4358 | 153.07 | 0 | PROCESSED | 57536.2568865741 | 2016-05-28 06:09:55 | 54735 | 2008-09-26 00:00:00 | 54088.6914699074 | 2006-12-19 16:35:43 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010062 | We propose to observe a edge-on nearby starburst galaxy, NGC 4631 for an exposure time of 80 ksec. This observation will give us a ``template'' of ejecta from type II SNe with less than 30% accuracy of abandance of alpha elemements. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORIKO YAMASAKI | JAP | 1 | AO1 | OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801019010/ | Quick Look | ![]() |
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240 | THE MOON | 138.793 | 11.1278 | 138.115741 | 11.336148 | 137.780525 | -4.592174 | 219.45159127 | 36.90361182 | 285.3988 | 56784.1992939815 | 2014-05-07 04:46:59 | 56784.3233101852 | 2014-05-07 07:45:34 | 809001060 | 6.4 | 45 | 6.4 | 6.4 | 0 | 6.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.2762 | 6.2762 | 10.7119 | 0 | PROCESSED | 57615.0611805556 | 2016-08-15 01:28:06 | 57218 | 2015-07-15 00:00:00 | 56852.5717708333 | 2014-07-14 13:43:21 | 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/ver3.0/809001060/ | Quick Look | ![]() |
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241 | CIZA J2242.8+5301 | 340.7602 | 53.1616 | 340.242904 | 52.89922 | 13.612188 | 54.382245 | 104.28022824 | -4.9963098 | 17.994 | 55770.5553703704 | 2011-07-28 13:19:44 | 55772.8210185185 | 2011-07-30 19:42:16 | 806001010 | 122.9419 | 120 | 122.9499 | 122.9499 | 0 | 122.9419 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134.8043 | 134.8043 | 195.7079 | 1 | PROCESSED | 57602.7365393518 | 2016-08-02 17:40:37 | 56162 | 2012-08-23 00:00:00 | 55792.3410069445 | 2011-08-19 08:11:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060014 | Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | SHO NISHINO | JAP | 6 | AO6 | SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806001010/ | Quick Look | ![]() |
242 | A2319NORTH | 290.2404 | 44.0121 | 289.851853 | 43.916672 | 305.965056 | 64.946826 | 75.73364984 | 13.56775034 | 191.4804 | 55925.1947222222 | 2011-12-30 04:40:24 | 55927.5001273148 | 2012-01-01 12:00:11 | 806014010 | 104.7893 | 100 | 104.8293 | 104.7893 | 0 | 104.8293 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 1.8661 | 0 | PROCESSED | 57604.2771064815 | 2016-08-04 06:39:02 | 56340 | 2013-02-17 00:00:00 | 55973.7475115741 | 2012-02-16 17:56:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060044 | We propose the observations of the north subgroup region in the A2319 cluster with Suzaku to investigate dynamical status and particle acceleration process in the intracluster medium (ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will determine the radial velocity of the ICM in the north subgroup region, and compare it with that in the central region which has been already determined from the AO1 data (Sugawara et al. 2009). Using these results and optical observational data of member galaxies, we will determine dynamical status of the ICM and get implications on the particle acceleration process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MOTOKAZU TAKIZAWA | JAP | 6 | AO6 | DYNAMICAL STATUS OF THE HOT GAS AROUND THE NORTH SUBGROUP IN THE A2319 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806014010/ | Quick Look | ![]() |
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243 | COMA OUTSKIRTS2 | 195.8535 | 28.5112 | 195.253601 | 28.779358 | 182.053697 | 32.234375 | 61.20140467 | 87.01280614 | 116.0004 | 55901.4349189815 | 2011-12-06 10:26:17 | 55901.9223842593 | 2011-12-06 22:08:14 | 806021010 | 20.3577 | 20 | 20.3617 | 20.3577 | 0 | 20.3648 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.1946 | 19.1946 | 42.114 | 0 | PROCESSED | 57604.0414351852 | 2016-08-04 00:59:40 | 56282 | 2012-12-21 00:00:00 | 55914.2609375 | 2011-12-19 06:15:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806021010/ | Quick Look | ![]() |
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244 | ABELL 3341 | 81.3893 | -31.5876 | 80.918035 | -31.630439 | 77.271182 | -54.650323 | 235.16288585 | -31.086571 | 266.8997 | 57094.3290393518 | 2015-03-13 07:53:49 | 57094.5780092593 | 2015-03-13 13:52:20 | 809104010 | 11.439 | 10 | 11.439 | 11.439 | 0 | 11.439 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7607407407 | 2016-08-17 18:15:28 | 57478 | 2016-03-31 00:00:00 | 57108.4097685185 | 2015-03-27 09:50:04 | 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 | B | 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/ver3.0/809104010/ | Quick Look | ![]() |
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245 | A3112 | 49.3536 | -44.4489 | 48.920211 | -44.631107 | 25.15452 | -59.09191 | 253.34827073 | -56.10640985 | 209.0009 | 57000.6762037037 | 2014-12-09 16:13:44 | 57003.8439351852 | 2014-12-12 20:15:16 | 809116010 | 107.9651 | 200 | 107.9651 | 107.9651 | 0 | 107.9651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.1487 | 8.1487 | 33.9079 | 1 | PROCESSED | 57617.53125 | 2016-08-17 12:45:00 | 57387 | 2015-12-31 00:00:00 | 57016.2346180556 | 2014-12-25 05:37:51 | 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 | KOSUKE SATO | 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/ver3.0/809116010/ | Quick Look | ![]() |
246 | THE MOON | 19.4299 | 8.4288 | 18.775956 | 8.165731 | 21.110635 | 0.205257 | 134.00151394 | -53.87712274 | 73.8016 | 56856.6577777778 | 2014-07-18 15:47:12 | 56856.7905439815 | 2014-07-18 18:58:23 | 809001110 | 6.3696 | 45 | 6.3856 | 6.3696 | 0 | 6.3936 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3999305556 | 2016-08-15 09:35:54 | 57233 | 2015-07-30 00:00:00 | 56867.740474537 | 2014-07-29 17:46:17 | 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/ver3.0/809001110/ | Quick Look | ![]() |
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247 | THE MOON | 20.9888 | 9.1871 | 20.332488 | 8.926606 | 22.823039 | 0.333671 | 136.29340358 | -52.83899755 | 73.8 | 56856.7918055556 | 2014-07-18 19:00:12 | 56856.8877662037 | 2014-07-18 21:18:23 | 809001120 | 4.2623 | 45 | 4.2703 | 4.2623 | 0 | 4.2783 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.400775463 | 2016-08-15 09:37:07 | 57233 | 2015-07-30 00:00:00 | 56867.7339930556 | 2014-07-29 17:36:57 | 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/ver3.0/809001120/ | Quick Look | ![]() |
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248 | RXCJ0018.9-4051 | 4.7354 | -40.8551 | 4.113382 | -41.132744 | 344.925025 | -38.685562 | 326.87167276 | -74.72717506 | 232.4175 | 55161.0142708333 | 2009-11-26 00:20:33 | 55161.4169444444 | 2009-11-26 10:00:24 | 804004010 | 19.3278 | 10 | 19.3278 | 19.3278 | 0 | 19.3278 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.3198 | 13.3198 | 34.7839 | 1 | PROCESSED | 57549.5606481482 | 2016-06-10 13:27:20 | 55553 | 2010-12-23 00:00:00 | 55182.6506712963 | 2009-12-17 15:36:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804004010/ | Quick Look | ![]() |
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249 | PERSEUS OFFSET-H | 50.3251 | 41.6598 | 49.495605 | 41.480554 | 58.942633 | 22.403293 | 150.73113668 | -12.9828544 | 270.0006 | 55595.9611458333 | 2011-02-03 23:04:03 | 55596.3536805556 | 2011-02-04 08:29:18 | 805048010 | 18.241 | 25 | 18.249 | 18.249 | 0 | 18.241 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.88 | 14.88 | 33.9039 | 0 | PROCESSED | 57600.8294560185 | 2016-07-31 19:54:25 | 55979 | 2012-02-22 00:00:00 | 55610.233287037 | 2011-02-18 05:35:56 | 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/ver3.0/805048010/ | Quick Look | ![]() |
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250 | ABELL 2667 | 357.9715 | -25.9262 | 357.325218 | -26.204419 | 347.258509 | -22.861194 | 34.71945037 | -76.63317585 | 64.8859 | 55721.5923611111 | 2011-06-09 14:13:00 | 55722.9050925926 | 2011-06-10 21:43:20 | 806029010 | 51.2214 | 50 | 51.2294 | 51.2294 | 0 | 51.2214 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.4843 | 40.4843 | 113.4098 | 1 | PROCESSED | 57602.2712962963 | 2016-08-02 06:30:40 | 55652 | 2011-04-01 00:00:00 | 55757.6995486111 | 2011-07-15 16:47:21 | 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/ver3.0/806029010/ | Quick Look | ![]() |
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251 | PERSEUS W1_2 | 49.5978 | 41.5445 | 48.771099 | 41.36257 | 58.342724 | 22.443076 | 150.3304489 | -13.378921 | 258.3807 | 56328.3362615741 | 2013-02-05 08:04:13 | 56329.0106018518 | 2013-02-06 00:15:16 | 807022010 | 28.9492 | 25 | 28.9492 | 28.9732 | 0 | 28.9492 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.2751 | 26.2751 | 58.2559 | 0 | PROCESSED | 57610.5207523148 | 2016-08-10 12:29:53 | 56715 | 2014-02-27 00:00:00 | 56349.5185648148 | 2013-02-26 12:26:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | 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 will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807022010/ | Quick Look | ![]() |
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252 | PERSEUS G_2 | 50.329 | 41.3745 | 49.501378 | 41.195271 | 58.861053 | 22.128129 | 150.89645322 | -13.21839457 | 259.7649 | 56325.9651157407 | 2013-02-02 23:09:46 | 56326.3181828704 | 2013-02-03 07:38:11 | 807023010 | 14.2445 | 15 | 14.2445 | 14.2525 | 0 | 14.2525 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.5822 | 20.5822 | 30.4839 | 0 | PROCESSED | 57610.4949074074 | 2016-08-10 11:52:40 | 56711 | 2014-02-23 00:00:00 | 56345.4909953704 | 2013-02-22 11:47:02 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | 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 will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807023010/ | Quick Look | ![]() |
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253 | COMA SW1 | 194.4352 | 27.7266 | 193.830461 | 27.996528 | 181.158138 | 30.970186 | 56.45564066 | 88.47880121 | 314.5924 | 55735.5408796296 | 2011-06-23 12:58:52 | 55735.8654166667 | 2011-06-23 20:46:12 | 806047010 | 8.9948 | 10 | 9.0028 | 8.9948 | 0 | 9.0108 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.5423 | 8.5423 | 28.0339 | 1 | PROCESSED | 57602.3938773148 | 2016-08-02 09:27:11 | 55652 | 2011-04-01 00:00:00 | 55794.9989583333 | 2011-08-21 23:58:30 | 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/ver3.0/806047010/ | Quick Look | ![]() |
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254 | COMA SW6 | 193.5264 | 26.9952 | 192.918358 | 27.266175 | 180.700954 | 29.954854 | 20.45636346 | 89.39137704 | 314.5991 | 55736.3040393518 | 2011-06-24 07:17:49 | 55736.5884259259 | 2011-06-24 14:07:20 | 806049010 | 15.6938 | 15 | 15.6938 | 15.7258 | 0 | 15.7098 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.0934 | 13.0934 | 24.5599 | 0 | PROCESSED | 57602.3988657407 | 2016-08-02 09:34:22 | 55652 | 2011-04-01 00:00:00 | 55795.0033333333 | 2011-08-22 00:04:48 | 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/ver3.0/806049010/ | Quick Look | ![]() |
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255 | COMA SW6.5 | 193.4098 | 26.8733 | 192.801305 | 27.144404 | 180.65639 | 29.799393 | 5.58469416 | 89.44734556 | 314.5984 | 55736.5887615741 | 2011-06-24 14:07:49 | 55737.1238773148 | 2011-06-25 02:58:23 | 806050010 | 16.5376 | 15 | 16.5616 | 16.5536 | 0 | 16.5376 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6623 | 16.6623 | 46.208 | 2 | PROCESSED | 57602.4126157407 | 2016-08-02 09:54:10 | 55652 | 2011-04-01 00:00:00 | 55795.0480324074 | 2011-08-22 01:09:10 | 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/ver3.0/806050010/ | Quick Look | ![]() |
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256 | DDO 120 | 185.3167 | 45.8198 | 184.701182 | 46.097069 | 161.957395 | 43.126416 | 138.73502996 | 70.37152611 | 129.0479 | 56256.0169444444 | 2012-11-25 00:24:24 | 56258.4271990741 | 2012-11-27 10:15:10 | 807044010 | 101.7414 | 100 | 101.7414 | 101.7414 | 0 | 101.7414 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.0864 | 91.0864 | 208.1839 | 0 | PROCESSED | 57608.1579861111 | 2016-08-08 03:47:30 | 56644 | 2013-12-18 00:00:00 | 56275.7410648148 | 2012-12-14 17:47:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070107 | We propose to observe an irregular dwarf galaxy DDO120 to detect a hot interstellar medium associated with the dwarf galaxy. The study of the temperature and density of the gas will give us important information about the pollution of the intergalactic medium from galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RYO YAMAMOTO | JAP | 7 | AO7 | SEARCH FOR HOT INTERSTELLAR MEDIUM OF AN IRREGULAR DWARF GALAXY DDO 120 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807044010/ | Quick Look | ![]() |
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257 | UGC03957 NORTH | 114.9138 | 55.8102 | 113.899292 | 55.925218 | 106.552165 | 33.791456 | 161.76581362 | 28.79157051 | 294.9973 | 56006.0767939815 | 2012-03-20 01:50:35 | 56007.0710532407 | 2012-03-21 01:42:19 | 806091010 | 41.3662 | 45 | 41.3662 | 41.3662 | 0 | 41.3662 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.6312 | 40.6312 | 85.9019 | 1 | PROCESSED | 57604.9833217593 | 2016-08-04 23:35:59 | 56389 | 2013-04-07 00:00:00 | 56022.2738888889 | 2012-04-05 06:34:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BRENDA MIRANDA OCEJO | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806091010/ | Quick Look | ![]() |
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258 | UGC03957 SOUTH | 115.5259 | 55.024 | 114.524001 | 55.141747 | 107.151159 | 33.092194 | 162.70412876 | 29.04503782 | 294.9967 | 56007.0719907407 | 2012-03-21 01:43:40 | 56008.1328125 | 2012-03-22 03:11:15 | 806092010 | 48.8159 | 45 | 48.8159 | 48.8159 | 0 | 48.8159 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.4169 | 46.4169 | 91.6439 | 3 | PROCESSED | 57604.9862731482 | 2016-08-04 23:40:14 | 56389 | 2013-04-07 00:00:00 | 56022.2514930556 | 2012-04-05 06:02:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BRENDA MIRANDA OCEJO | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806092010/ | Quick Look | ![]() |
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259 | A1750C | 202.6943 | -1.8873 | 202.05036 | -1.629855 | 201.691973 | 7.074913 | 322.57262201 | 59.47596371 | 293.5241 | 55766.9371064815 | 2011-07-24 22:29:26 | 55767.8814814815 | 2011-07-25 21:09:20 | 806095010 | 41.4893 | 40 | 41.5049 | 41.4893 | 0 | 41.5049 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0991 | 41.0991 | 81.5778 | 0 | PROCESSED | 57602.6723148148 | 2016-08-02 16:08:08 | 56219 | 2012-10-19 00:00:00 | 55851.4572106482 | 2011-10-17 10:58:23 | 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/ver3.0/806095010/ | Quick Look | ![]() |
260 | M31 | 10.6944 | 41.2627 | 10.010045 | 40.988882 | 27.852586 | 33.34214 | 121.18191229 | -21.57961988 | 231.6592 | 54115.6775578704 | 2007-01-15 16:15:41 | 54117.4572222222 | 2007-01-17 10:58:24 | 801043010 | 99.8723 | 100 | 99.8723 | 99.8723 | 0 | 99.8723 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.9124 | 103.9124 | 153.7238 | 1 | PROCESSED | 57536.8902777778 | 2016-05-28 21:22:00 | 54744 | 2008-10-05 00:00:00 | 54132.9457291667 | 2007-02-01 22:41:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010089 | We propose the 100 ks Suzaku observation of the central region of Andromeda Nebula (M31). Our gaol is to detect 3 components (cool, hot and hard) of galactic diffuse X-ray emission (GDXE) with the XIS and HXD. This detection shows the existance of the GDXE hot and hard component in the extragalactic normal spiral galaxy, for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROMITSU TAKAHASHI | JAP | 1 | AO1 | DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801043010/ | Quick Look | ![]() |
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261 | ANTLIA E1 | 157.8782 | -35.3295 | 157.312453 | -35.072071 | 176.074864 | -40.746998 | 273.21530285 | 19.3432713 | 277.4995 | 56091.5629398148 | 2012-06-13 13:30:38 | 56092.2633912037 | 2012-06-14 06:19:17 | 807066010 | 25.747 | 23 | 25.755 | 25.747 | 0 | 25.755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.9291 | 22.9291 | 60.5139 | 1 | PROCESSED | 57605.6597106482 | 2016-08-05 15:49:59 | 56473 | 2013-06-30 00:00:00 | 56107.272650463 | 2012-06-29 06:32:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807066010/ | Quick Look | ![]() |
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262 | A133_E | 15.9075 | -21.8935 | 15.297134 | -22.16169 | 5.436545 | -26.315725 | 151.49316881 | -84.07673835 | 44.9955 | 55356.7284953704 | 2010-06-09 17:29:02 | 55358.0015393518 | 2010-06-11 00:02:13 | 805021010 | 51.5523 | 50 | 51.5641 | 51.5603 | 0 | 51.5523 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.2547 | 46.2547 | 109.984 | 1 | PROCESSED | 57551.9411458333 | 2016-06-12 22:35:15 | 55737 | 2011-06-25 00:00:00 | 55375.7548842593 | 2010-06-28 18:07:02 | 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/ver3.0/805021010/ | Quick Look | ![]() |
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263 | COMA NW6.5 | 194.0774 | 29.5523 | 193.474522 | 29.822643 | 179.856398 | 32.45513 | 99.36309014 | 87.34957637 | 319.9974 | 55734.7422685185 | 2011-06-22 17:48:52 | 55735.2522569444 | 2011-06-23 06:03:15 | 806045010 | 15.5013 | 15 | 15.5013 | 15.5151 | 0 | 15.5093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.3764 | 17.3764 | 44.0599 | 0 | PROCESSED | 57602.3928587963 | 2016-08-02 09:25:43 | 55652 | 2011-04-01 00:00:00 | 55768.3250231482 | 2011-07-26 07:48:02 | 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/ver3.0/806045010/ | Quick Look | ![]() |
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264 | ABELL 1795 | 207.2241 | 26.601 | 206.646901 | 26.849155 | 193.922602 | 34.994161 | 33.84733119 | 77.1817764 | 130.8638 | 53714.5034259259 | 2005-12-10 12:04:56 | 53714.7752199074 | 2005-12-10 18:36:19 | 800012010 | 13.0982 | 120 | 13.1062 | 13.0982 | 13.1062 | 13.1062 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10.3759 | 10.3759 | 23.4639 | 1 | PROCESSED | 57532.3922453704 | 2016-05-24 09:24:50 | 54247 | 2007-05-27 00:00:00 | 54038.7903703704 | 2006-10-30 18:58:08 | 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/ver3.0/800012010/ | Quick Look | ![]() |
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265 | Z8852 | 347.6318 | 7.5789 | 346.999079 | 7.307292 | 351.631711 | 11.858062 | 84.17423864 | -47.55525942 | 260.3346 | 54065.5867013889 | 2006-11-26 14:04:51 | 54066.1543287037 | 2006-11-27 03:42:14 | 801074010 | 14.8526 | 15 | 14.8526 | 14.8526 | 0 | 14.8526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.9834 | 13.9834 | 49.0379 | 0 | PROCESSED | 57536.1918402778 | 2016-05-28 04:36:15 | 54695 | 2008-08-17 00:00:00 | 54088.6000694444 | 2006-12-19 14:24:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801074010/ | Quick Look | ![]() |
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266 | PERSEUS H_2 | 50.3295 | 41.6532 | 49.500037 | 41.47397 | 58.944091 | 22.396043 | 150.73770492 | -12.98651547 | 259.0589 | 56327.8720949074 | 2013-02-04 20:55:49 | 56328.3355092593 | 2013-02-05 08:03:08 | 807021010 | 20.3456 | 20 | 20.3636 | 20.3456 | 0 | 20.3536 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.8776 | 21.8776 | 40.034 | 0 | PROCESSED | 57610.5111921296 | 2016-08-10 12:16:07 | 56715 | 2014-02-27 00:00:00 | 56349.4892708333 | 2013-02-26 11:44:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | 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 will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807021010/ | Quick Look | ![]() |
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267 | A2495 | 342.5662 | 10.9218 | 341.941655 | 10.656649 | 348.262816 | 16.910805 | 81.19678392 | -41.92445268 | 65.1354 | 54260.5857523148 | 2007-06-09 14:03:29 | 54261.1668287037 | 2007-06-10 04:00:14 | 801080020 | 25.7806 | 18 | 25.7806 | 25.7806 | 0 | 25.7806 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.9762 | 20.9762 | 50.1959 | 2 | PROCESSED | 57538.8757291667 | 2016-05-30 21:01:03 | 54695 | 2008-08-17 00:00:00 | 54270.430625 | 2007-06-19 10:20:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801080020/ | Quick Look | ![]() |
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268 | CENTAURUS CLUSTER | 192.2012 | -41.3132 | 191.510497 | -41.040677 | 209.072585 | -32.853902 | 302.40029759 | 21.55583076 | 106.2442 | 53731.2579050926 | 2005-12-27 06:11:23 | 53732.1808333333 | 2005-12-28 04:20:24 | 800014010 | 36.5192 | 30 | 36.5192 | 36.5464 | 36.5464 | 36.5224 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32.1498 | 32.1498 | 79.7399 | 0 | PROCESSED | 57532.5349652778 | 2016-05-24 12:50:21 | 54247 | 2007-05-27 00:00:00 | 54039.373900463 | 2006-10-31 08:58:25 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800014010/ | Quick Look | ![]() |
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269 | HCG62_W | 192.9973 | -9.0837 | 192.347013 | -8.812069 | 195.480643 | -3.238715 | 303.16227701 | 53.78780217 | 292.9782 | 55405.1509953704 | 2010-07-28 03:37:26 | 55406.9773611111 | 2010-07-29 23:27:24 | 805031010 | 66.947 | 60 | 66.955 | 66.955 | 0 | 66.947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.9972 | 52.9972 | 157.7758 | 1 | PROCESSED | 57552.8094675926 | 2016-06-13 19:25:38 | 55808 | 2011-09-04 00:00:00 | 55441.3150925926 | 2010-09-02 07:33:44 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050034 | We propose offset observations of groups of galaxies to study the metal distributions up to ~0.5 times of the virial radius. Metal mass to galaxy light ratios (MLRs) for groups are much smaller than those for clusters of galaxies. In order to solve the problem which is important to understand the chemical history of the universe, we need much information of the metal abundance and distributions to the outer region of the groups. Suzaku firstly enable us to measure the metals to such an outer region of groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 5 | AO5 | SEARCH FOR THE METAL DISTRIBUTIONS OF GROUPS OF GALAXIES TO 0.5 R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805031010/ | Quick Look | ![]() |
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270 | BEYOND VIRGO 4 | 187.7154 | 16.9006 | 187.085728 | 17.176651 | 180.130581 | 18.529302 | 276.92044319 | 78.71921322 | 118.472 | 55915.331099537 | 2011-12-20 07:56:47 | 55916.0466666667 | 2011-12-21 01:07:12 | 806063010 | 30.1361 | 30 | 30.1361 | 30.1361 | 0 | 30.1361 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.7334 | 22.7334 | 61.818 | 0 | PROCESSED | 57604.1732407407 | 2016-08-04 04:09:28 | 56299 | 2013-01-07 00:00:00 | 55932.1295949074 | 2012-01-06 03:06:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806063010/ | Quick Look | ![]() |
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271 | RCS215222-0503.9 | 328.0881 | -5.0633 | 327.433899 | -5.298799 | 328.489701 | 7.382957 | 52.1030598 | -42.03624594 | 70.7002 | 55696.1248842593 | 2011-05-15 02:59:50 | 55696.8398263889 | 2011-05-15 20:09:21 | 806081010 | 30.6482 | 30 | 30.6482 | 30.6482 | 0 | 30.6482 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 25.3728 | 25.3728 | 61.744 | 0 | PROCESSED | 57602.0507986111 | 2016-08-02 01:13:09 | 56072 | 2012-05-25 00:00:00 | 55705.2063310185 | 2011-05-24 04:57:07 | 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/ver3.0/806081010/ | Quick Look | ![]() |
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272 | A3526 | 191.8847 | -40.8272 | 191.196139 | -40.554367 | 208.554246 | -32.533282 | 302.13618529 | 22.03852437 | 109.9993 | 55942.6812037037 | 2012-01-16 16:20:56 | 55942.9772569444 | 2012-01-16 23:27:15 | 806085010 | 15.0057 | 11 | 15.0097 | 15.0057 | 0 | 15.0116 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.9297 | 14.9297 | 25.576 | 0 | PROCESSED | 57604.3736805556 | 2016-08-04 08:58:06 | 56331 | 2013-02-08 00:00:00 | 55960.1598726852 | 2012-02-03 03:50:13 | 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/ver3.0/806085010/ | Quick Look | ![]() |
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273 | ABELL 426 SW1 | 49.6666 | 41.3604 | 48.840906 | 41.178725 | 58.340814 | 22.251887 | 150.47849352 | -13.50469455 | 88.4985 | 55803.5918402778 | 2011-08-30 14:12:15 | 55803.8230671296 | 2011-08-30 19:45:13 | 806099010 | 11.5592 | 10 | 11.5752 | 11.5592 | 0 | 11.5752 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.5421 | 11.5421 | 19.9701 | 0 | PROCESSED | 57603.0124189815 | 2016-08-03 00:17:53 | 55652 | 2011-04-01 00:00:00 | 55826.1721875 | 2011-09-22 04:07:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806099010/ | Quick Look | ![]() |
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274 | A1060 | 159.1744 | -27.531 | 158.58579 | -27.271265 | 172.752913 | -33.32931 | 269.60056717 | 26.48279097 | 103.6438 | 53696.6258796296 | 2005-11-22 15:01:16 | 53697.7211111111 | 2005-11-23 17:18:24 | 800003010 | 39.139 | 40 | 39.139 | 39.147 | 39.155 | 39.155 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34.6024 | 34.6024 | 94.6259 | 1 | PROCESSED | 57528.0675462963 | 2016-05-20 01:37:16 | 54247 | 2007-05-27 00:00:00 | 54037.8583449074 | 2006-10-29 20:36:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001021 | A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800003010/ | Quick Look | ![]() |
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275 | NGC720 | 28.2529 | -13.7362 | 27.644452 | -13.982164 | 20.9363 | -23.62893 | 173.01572713 | -70.35499124 | 242.5294 | 53734.3673611111 | 2005-12-30 08:49:00 | 53739.5627546296 | 2006-01-04 13:30:22 | 800009010 | 177.1929 | 100 | 177.1929 | 177.1929 | 177.1929 | 177.1929 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.6621 | 9.6621 | 47.5408 | 0 | PROCESSED | 57532.602962963 | 2016-05-24 14:28:16 | 54247 | 2007-05-27 00:00:00 | 54039.6651736111 | 2006-10-31 15:57:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001031 | We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800009010/ | Quick Look | ![]() |
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276 | A2104N | 235.0318 | -3.1802 | 234.37876 | -3.019346 | 233.471257 | 15.936264 | 2.94593816 | 39.29281704 | 117.689 | 54119.2779166667 | 2007-01-19 06:40:12 | 54119.7522337963 | 2007-01-19 18:03:13 | 801002010 | 18.8424 | 20 | 18.8424 | 18.8424 | 0 | 18.8424 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.6448 | 13.6448 | 40.9779 | 1 | PROCESSED | 57536.8705439815 | 2016-05-28 20:53:35 | 54735 | 2008-09-26 00:00:00 | 54133.3893518518 | 2007-02-02 09:20:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801002010/ | Quick Look | ![]() |
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277 | NGC 507 | 20.9105 | 33.2598 | 20.206045 | 32.999169 | 32.202982 | 22.611804 | 130.6367604 | -29.12969375 | 54.0771 | 53944.6189351852 | 2006-07-28 14:51:16 | 53946.5544444444 | 2006-07-30 13:18:24 | 801017010 | 79.5013 | 80 | 79.5253 | 79.5013 | 79.5253 | 79.5253 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 80.2867 | 80.2867 | 167.17 | 2 | PROCESSED | 57535.1047222222 | 2016-05-27 02:30:48 | 54394 | 2007-10-21 00:00:00 | 53955.7736689815 | 2006-08-08 18:34:05 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010061 | We propose to observe luminous elliptical galaxies NGC 507 and NGC 499 for 80 and 100 ksec, respectively, to study abundance distribution of Fe and O. The good energy resolution and low background of the XIS instrument is crucial for this study, and we can perform the first reliable measurement of O distribution around elliptical galaxies. Comparison of O and Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. Comparison of NGC 507 and NGC 499 will show us how much metal production process differ with galaxy size. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 1 | AO1 | CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801017010/ | Quick Look | ![]() |
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278 | ABELL 426 SE4.5 | 51.0328 | 40.5957 | 50.208366 | 40.419106 | 59.183999 | 21.234356 | 151.7976658 | -13.56504097 | 89.5625 | 55798.9213657407 | 2011-08-25 22:06:46 | 55799.1758912037 | 2011-08-26 04:13:17 | 806117010 | 12.0196 | 10 | 12.0196 | 12.0196 | 0 | 12.0356 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.4959 | 10.4959 | 21.9839 | 0 | PROCESSED | 57602.9577893518 | 2016-08-02 22:59:13 | 55652 | 2011-04-01 00:00:00 | 55855.1616435185 | 2011-10-21 03:52:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806117010/ | Quick Look | ![]() |
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279 | OPHIUCHUS CLUSTER 2 | 257.7375 | -23.3864 | 256.979428 | -23.325463 | 258.749053 | -0.422802 | 0.3572282 | 9.54416529 | 94.9391 | 54181.1423726852 | 2007-03-22 03:25:01 | 54181.825162037 | 2007-03-22 19:48:14 | 801023010 | 24.6782 | 15 | 24.7022 | 24.6942 | 0 | 24.6782 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.2781 | 21.2781 | 58.9879 | 1 | PROCESSED | 57537.9744097222 | 2016-05-29 23:23:09 | 54736 | 2008-09-27 00:00:00 | 54209.5433217593 | 2007-04-19 13:02:23 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801023010/ | Quick Look | ![]() |
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280 | ABELL 426 NE2.5 | 50.6676 | 41.9537 | 49.835188 | 41.775725 | 59.295588 | 22.616024 | 150.78054856 | -12.59654862 | 89.499 | 55808.8756134259 | 2011-09-04 21:00:53 | 55809.0717592593 | 2011-09-05 01:43:20 | 806125010 | 9.7394 | 10 | 9.7554 | 9.7394 | 0 | 9.7634 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.3671 | 7.3671 | 16.9439 | 0 | PROCESSED | 57603.064224537 | 2016-08-03 01:32:29 | 55652 | 2011-04-01 00:00:00 | 55865.9792361111 | 2011-10-31 23:30:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806125010/ | Quick Look | ![]() |
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281 | ABELL 426 NE4.5 | 51.271 | 42.2915 | 50.434611 | 42.115781 | 59.862037 | 22.81958 | 150.96498821 | -12.06556882 | 89.4971 | 55809.84625 | 2011-09-05 20:18:36 | 55810.0452662037 | 2011-09-06 01:05:11 | 806129010 | 10.381 | 10 | 10.381 | 10.381 | 0 | 10.381 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.933 | 8.933 | 17.184 | 0 | PROCESSED | 57603.0777777778 | 2016-08-03 01:52:00 | 55652 | 2011-04-01 00:00:00 | 55866.1125462963 | 2011-11-01 02:42:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806129010/ | Quick Look | ![]() |
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282 | ABELL 426 NE5.5 | 51.5754 | 42.4541 | 50.737042 | 42.279527 | 60.14462 | 22.915633 | 151.06006994 | -11.8041168 | 89.4991 | 55810.5422569444 | 2011-09-06 13:00:51 | 55810.8217361111 | 2011-09-06 19:43:18 | 806131010 | 14.8458 | 15 | 14.8618 | 14.8618 | 0 | 14.8458 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.2198 | 16.2198 | 24.1439 | 0 | PROCESSED | 57603.0838310185 | 2016-08-03 02:00:43 | 55652 | 2011-04-01 00:00:00 | 55866.1408101852 | 2011-11-01 03:22:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806131010/ | Quick Look | ![]() |
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283 | ABELL 426 NNE3.5 | 50.2092 | 42.4612 | 49.374656 | 42.281515 | 59.092741 | 23.197382 | 150.20252687 | -12.36344342 | 60.4978 | 55804.7853125 | 2011-08-31 18:50:51 | 55805.0002546296 | 2011-09-01 00:00:22 | 806139010 | 10.02 | 10 | 10.02 | 10.02 | 0 | 10.02 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.507 | 9.507 | 18.5599 | 0 | PROCESSED | 57603.0247916667 | 2016-08-03 00:35:42 | 55652 | 2011-04-01 00:00:00 | 55830.1973958333 | 2011-09-26 04:44:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806139010/ | Quick Look | ![]() |
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284 | A2319CENTER | 290.3341 | 43.878 | 289.944223 | 43.782148 | 306.012819 | 64.798086 | 75.63759851 | 13.45022652 | 251.6652 | 54035.9326041667 | 2006-10-27 22:22:57 | 54038.1466898148 | 2006-10-30 03:31:14 | 801040010 | 99.5332 | 100 | 99.5492 | 99.5412 | 99.5332 | 99.5492 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93.9548 | 93.9548 | 191.268 | 2 | PROCESSED | 57535.9905555556 | 2016-05-27 23:46:24 | 54735 | 2008-09-26 00:00:00 | 54063.5741666667 | 2006-11-24 13:46:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010085 | We propose the observations of the A2319 cluster with the Suzaku HXD and XIS to investigate particle acceleration processes in the intracluster medium(ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will detect non-thermal hard X-ray with HXD, and determine the velocity difference between the two subclusters with XIS. With these results, we will determine dynamical status of the ICM and get implications on the particle acceleration processes. We will compare the results with theoretical models, numerical simulations, and radio and optical observations to get an overall picture of particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MOTOKAZU TAKIZAWA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE A2319 CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801040010/ | Quick Look | ![]() |
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285 | PERSEUS CL OFFSET | 50.5735 | 41.8053 | 49.742345 | 41.626976 | 59.178685 | 22.492416 | 150.80595618 | -12.75877318 | 65.9956 | 53982.1426736111 | 2006-09-04 03:25:27 | 53982.4377893518 | 2006-09-04 10:30:25 | 801049040 | 10.4206 | 30 | 10.4206 | 10.4206 | 10.4206 | 10.4206 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7.5402 | 7.5402 | 25.4679 | 1 | PROCESSED | 57535.4390856482 | 2016-05-27 10:32:17 | 54526 | 2008-03-01 00:00:00 | 54021.0033680556 | 2006-10-13 00:04:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049040/ | Quick Look | ![]() |
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286 | NGC3923 | 177.7599 | -28.8047 | 177.126048 | -28.526534 | 190.367331 | -27.106442 | 287.27787622 | 32.22445477 | 293.1988 | 53899.8430671296 | 2006-06-13 20:14:01 | 53902.7293287037 | 2006-06-16 17:30:14 | 801054010 | 115.82 | 120 | 115.828 | 115.82 | 115.828 | 115.828 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 107.7313 | 107.7313 | 249.3528 | 3 | PROCESSED | 57534.7187731482 | 2016-05-26 17:15:02 | 54394 | 2007-10-21 00:00:00 | 53927.2880902778 | 2006-07-11 06:54:51 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010100 | We propose to observe an isolated elliptical galaxy NGC3923, to meaasure a dark matter distribution. The large effective area and stable low background of XIS enable us to measure a faint extended X-ray emission such as the periphery of elliptical galaxies more accurately than ever. Since X-ray bright elliptical galaxies have been found to be surrounded by group-scale emission, X-ray faint elliptical galaxies are the best to investigate the dark matter associated with the galaxy itself. The dark matter around galaxies is a key to resolve the problem of why X-ray bright and faint elliptical galaxies exist. The oxygen abundance distribution is also useful to probe the above issue. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YASUSHI FUKAZAWA | JAP | 1 | AO1 | ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801054010/ | Quick Look | ![]() |
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287 | A2199 OFFSET10 | 245.7785 | 38.4489 | 245.339389 | 38.564051 | 231.762092 | 58.713673 | 61.35085602 | 44.73212253 | 143.0073 | 55922.3113541667 | 2011-12-27 07:28:21 | 55923.0174074074 | 2011-12-28 00:25:04 | 806156010 | 32.686 | 30 | 32.686 | 32.686 | 0 | 32.686 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.452 | 30.452 | 60.9959 | 1 | PROCESSED | 57604.2399074074 | 2016-08-04 05:45:28 | 55652 | 2011-04-01 00:00:00 | 55972.658599537 | 2012-02-15 15:48:23 | 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/ver3.0/806156010/ | Quick Look | ![]() |
288 | A2199 OFFSET13 | 247.4008 | 39.9951 | 246.975742 | 40.102999 | 233.166969 | 60.575403 | 63.55387948 | 43.51978117 | 252.5011 | 55815.2934375 | 2011-09-11 07:02:33 | 55815.9266203704 | 2011-09-11 22:14:20 | 806159010 | 28.648 | 20 | 28.648 | 29.3429 | 0 | 29.3589 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.7831 | 26.7831 | 54.6959 | 0 | PROCESSED | 57603.1066087963 | 2016-08-03 02:33:31 | 55652 | 2011-04-01 00:00:00 | 55851.4378703704 | 2011-10-17 10:30:32 | 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/ver3.0/806159010/ | Quick Look | ![]() |
289 | A1631_N | 193.3404 | -15.1138 | 192.682958 | -14.842526 | 198.153884 | -8.661195 | 303.62251983 | 47.75536925 | 113.0007 | 56303.6628356482 | 2013-01-11 15:54:29 | 56304.4904861111 | 2013-01-12 11:46:18 | 807003010 | 28.0433 | 20 | 28.183 | 28.183 | 0 | 28.0433 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 25.3059 | 25.3059 | 71.48 | 1 | PROCESSED | 57608.4621296296 | 2016-08-08 11:05:28 | 56703 | 2014-02-15 00:00:00 | 56337.5115393518 | 2013-02-14 12:16:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807003010/ | Quick Look | ![]() |
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290 | NGC 4472 | 187.4441 | 8.005 | 186.80838 | 8.281234 | 183.627851 | 10.299036 | 286.9163593 | 70.20028227 | 117.8054 | 54072.8427893518 | 2006-12-03 20:13:37 | 54075.7014699074 | 2006-12-06 16:50:07 | 801064010 | 121.0358 | 120 | 121.0358 | 121.0358 | 0 | 121.0358 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.4464 | 103.4464 | 246.9548 | 6 | PROCESSED | 57536.3089467593 | 2016-05-28 07:24:53 | 54702 | 2008-08-24 00:00:00 | 54089.1857523148 | 2006-12-20 04:27:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801064010/ | Quick Look | ![]() |
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291 | NGC 4649 | 190.9148 | 11.557 | 190.284732 | 11.830628 | 185.371113 | 14.926523 | 295.86493189 | 74.32191724 | 113.3108 | 54098.4203703704 | 2006-12-29 10:05:20 | 54104.1473263889 | 2007-01-04 03:32:09 | 801065010 | 224.0304 | 120 | 224.0304 | 224.0304 | 0 | 224.0304 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3042 | 26.3042 | 69.2898 | 1 | PROCESSED | 57536.4300578704 | 2016-05-28 10:19:17 | 54743 | 2008-10-04 00:00:00 | 54132.9809027778 | 2007-02-01 23:32:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801065010/ | Quick Look | ![]() |
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292 | UGC03957 | 115.2433 | 55.429 | 114.235063 | 55.545488 | 106.863653 | 33.455815 | 162.22286538 | 28.93195726 | 271.243 | 53841.9927314815 | 2006-04-16 23:49:32 | 53842.2828587963 | 2006-04-17 06:47:19 | 801072010 | 10.7714 | 12 | 10.7794 | 10.7794 | 10.7874 | 10.7714 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9.642 | 9.642 | 25.0079 | 0 | PROCESSED | 57533.4729166667 | 2016-05-25 11:21:00 | 54401 | 2007-10-28 00:00:00 | 53906.7753240741 | 2006-06-20 18:36:28 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801072010/ | Quick Look | ![]() |
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293 | A272 | 28.7603 | 33.9026 | 28.031098 | 33.657734 | 38.955118 | 20.665911 | 137.73606223 | -27.1341127 | 64.9465 | 53943.0449537037 | 2006-07-27 01:04:44 | 53943.6842476852 | 2006-07-27 16:25:19 | 801084010 | 22.2455 | 21 | 22.2535 | 22.2535 | 22.2455 | 22.2535 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24.6035 | 24.6035 | 55.2319 | 0 | PROCESSED | 57535.0602430556 | 2016-05-27 01:26:45 | 54401 | 2007-10-28 00:00:00 | 53955.6516782407 | 2006-08-08 15:38:25 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801084010/ | Quick Look | ![]() |
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294 | A566 | 106.0915 | 63.2647 | 104.91759 | 63.339113 | 99.420321 | 40.34898 | 152.76309519 | 25.45548296 | 285.637 | 54178.3128587963 | 2007-03-19 07:30:31 | 54178.8029976852 | 2007-03-19 19:16:19 | 801085010 | 22.2711 | 20 | 22.2711 | 22.2711 | 0 | 22.2711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.1523 | 22.1523 | 42.3399 | 0 | PROCESSED | 57537.7151157407 | 2016-05-29 17:09:46 | 54695 | 2008-08-17 00:00:00 | 54185.9799305556 | 2007-03-26 23:31:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801085010/ | Quick Look | ![]() |
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295 | RXJ 0658 | 104.704 | -55.933 | 104.461428 | -55.862903 | 130.333928 | -77.302143 | 266.02429497 | -21.20357002 | 164.9362 | 54095.6181597222 | 2006-12-26 14:50:09 | 54098.4099421296 | 2006-12-29 09:50:19 | 801089010 | 101.3845 | 100 | 101.3845 | 101.3845 | 0 | 101.3845 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.3679 | 84.3679 | 241.1547 | 2 | PROCESSED | 57637.5971180556 | 2016-09-06 14:19:51 | 54702 | 2008-08-24 00:00:00 | 54111.5842013889 | 2007-01-11 14:01:15 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011448 | We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | VAHE PETROSIAN | USA | 1 | AO1 | HARD X-RAY EMISSION FROM CLUSTER RXJ0658 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801089010/ | Quick Look | ![]() |
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296 | SEGUE 1 | 151.7658 | 16.0862 | 151.086487 | 16.330668 | 148.083031 | 4.208593 | 220.47149585 | 50.42674703 | 110.8027 | 56248.0740625 | 2012-11-17 01:46:39 | 56250.3182291667 | 2012-11-19 07:38:15 | 807046010 | 85.4391 | 85 | 85.4622 | 85.4431 | 0 | 85.4391 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.5645 | 77.5645 | 193.8419 | 4 | PROCESSED | 57608.0603240741 | 2016-08-08 01:26:52 | 56641 | 2013-12-15 00:00:00 | 56275.5584490741 | 2012-12-14 13:24:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071502 | Our ongoing dedicated X-ray search for dark matter targeting dwarf spheroidal galaxies set new constraints on the mass and mixing angle of the sterile neutrino -- a plausible dark matter candidate that emits an X-ray via radiative decay. We have proposed a new well-motivated candidate -- moduli dark matter, that also produces a detectable X-ray line. We propose Suzaku observations of the Segue 1 dwarf spheroidal -- the most dark matter dominated galaxy known. Its extreme nature implies that it provides the tightest constraints on sterile neutrino and moduli parameters in the event of a detection, and best limits in the absence of one. The resulting spectrum is optimal for exploring new physics, such as string theory compactification or supersymmetry breaking, and as a legacy for Astro-H. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MICHAEL LOEWENSTEIN | USA | 7 | AO7 | SEARCH FOR DARK MATTER WITH SUZAKU OBSERVATIONS OF THE MOST DARK MATTER DOMINATED GALAXY IN THE UNIVERSE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807046010/ | Quick Look | ![]() |
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297 | COMA RADIO HALO | 194.9267 | 27.9061 | 194.323466 | 28.175433 | 181.517491 | 31.325949 | 56.39742233 | 88.00849705 | 295.2687 | 53886.8435300926 | 2006-05-31 20:14:41 | 53890.7439699074 | 2006-06-04 17:51:19 | 801097010 | 178.6572 | 180 | 178.6892 | 178.6572 | 178.7132 | 178.6892 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 167.4506 | 167.4506 | 336.9758 | 7 | PROCESSED | 57534.5953472222 | 2016-05-26 14:17:18 | 54401 | 2007-10-28 00:00:00 | 53926.6760416667 | 2006-07-10 16:13:30 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014446 | We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | CRAIG SARAZIN | KYOKO MATSUSHITA | USJ | 1 | AO1 | NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801097010/ | Quick Look | ![]() |
298 | A963S | 154.2641 | 38.9388 | 153.524075 | 39.18875 | 141.373211 | 26.246798 | 182.75442962 | 55.85527134 | 107.1093 | 54432.4435300926 | 2007-11-28 10:38:41 | 54432.9584953704 | 2007-11-28 23:00:14 | 802012010 | 27.7172 | 25 | 27.7252 | 27.7252 | 0 | 27.7172 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.6546 | 25.6546 | 44.492 | 1 | PROCESSED | 57540.6110185185 | 2016-06-01 14:39:52 | 54811 | 2008-12-11 00:00:00 | 54440.9716319444 | 2007-12-06 23:19:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020018 | 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 10% precision in a few arcmin scale, which has not been done before to any cluster. 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 | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802012010/ | Quick Look | ![]() |
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299 | ABELL 2744 | 3.5397 | -30.3446 | 2.908232 | -30.62262 | 349.980606 | -28.995561 | 9.24871336 | -81.22170813 | 53.4742 | 54239.5874652778 | 2007-05-19 14:05:57 | 54243.7709953704 | 2007-05-23 18:30:14 | 802033010 | 153.2332 | 150 | 153.2412 | 153.2412 | 0 | 153.2332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 133.8631 | 133.8631 | 361.4398 | 2 | PROCESSED | 57538.8170138889 | 2016-05-30 19:36:30 | 54745 | 2008-10-06 00:00:00 | 54248.6974074074 | 2007-05-28 16:44:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020077 | We propose a 150 ks Suzaku observation of Abell 2744 aiming at non-thermal hard X-ray detection. It has a red-shift of 0.3, a radio-halo flux of 57 mJy at 1.4 GHz and ICM temperature of 9 keV. Our strategy here is to observe a luminous merging cluster hosting a bright radio halo, whilst avoiding the thermal ICM emission to overwhelm the 10-40 keV band, in which the HXD has the best sensitivity. The key is to look for relatively high red-shift cluster. Since the CMB density increases as (1+z)^4, the inverse Compton emission relative to the radio flux increases typically as (1+z)^2, while the thermal ICM emission is red-shifted. We believe this is one of the best method to utilize the Suzaku power for cluster hard X-ray survey. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 2 | AO2 | HARD X-RAY VIEW OF A DISTANT RADIO-HALO CLUSTER ABELL2744 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802033010/ | Quick Look | ![]() |
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300 | NGC4636_GALACTIC_1 | 192.513 | 5.4558 | 191.878088 | 5.727905 | 189.348778 | 9.962987 | 301.99802564 | 68.32503562 | 300.0459 | 54268.8414930556 | 2007-06-17 20:11:45 | 54269.9307175926 | 2007-06-18 22:20:14 | 802039010 | 41.4997 | 30 | 41.5157 | 41.5077 | 0 | 41.4997 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3371 | 34.3371 | 94.0479 | 0 | PROCESSED | 57553.0490393518 | 2016-06-14 01:10:37 | 54695 | 2008-08-17 00:00:00 | 54319.4765740741 | 2007-08-07 11:26:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802039010/ | Quick Look | ![]() |
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301 | FORNAX_GALACTIC_2 | 49.9904 | -32.0719 | 49.483389 | -32.25188 | 35.195492 | -48.193254 | 230.76086762 | -57.49880076 | 52.7651 | 54280.3368518518 | 2007-06-29 08:05:04 | 54280.9897453704 | 2007-06-29 23:45:14 | 802040010 | 21.0746 | 20 | 21.0826 | 21.0826 | 0 | 21.0746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.131 | 20.131 | 56.3939 | 1 | PROCESSED | 57539.0651967593 | 2016-05-31 01:33:53 | 54696 | 2008-08-18 00:00:00 | 54322.4474537037 | 2007-08-10 10:44:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802040010/ | Quick Look | ![]() |
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302 | DRACO | 260.0265 | 57.929 | 259.823545 | 57.97767 | 237.171171 | 80.222303 | 86.38548758 | 34.73420948 | 52.1224 | 54196.7611458333 | 2007-04-06 18:16:03 | 54198.2216898148 | 2007-04-08 05:19:14 | 802051010 | 63.3232 | 67 | 63.3232 | 63.3232 | 0 | 63.3232 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.9572 | 64.9572 | 126.1818 | 2 | PROCESSED | 57538.1232291667 | 2016-05-30 02:57:27 | 54829 | 2008-12-29 00:00:00 | 54203.3603703704 | 2007-04-13 08:38:56 | 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/ver3.0/802051010/ | Quick Look | ![]() |
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303 | SDSS J0854+3524 | 133.7386 | 35.4192 | 132.953536 | 35.610263 | 126.168595 | 17.306871 | 188.0033984 | 39.53150085 | 111.2842 | 56214.3546527778 | 2012-10-14 08:30:42 | 56214.8244560185 | 2012-10-14 19:47:13 | 807063010 | 20.6148 | 20 | 20.6148 | 20.6148 | 0 | 20.6148 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.084 | 18.084 | 40.56 | 0 | PROCESSED | 57607.7601157407 | 2016-08-07 18:14:34 | 56598 | 2013-11-02 00:00:00 | 56232.4365856482 | 2012-11-01 10:28:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807063010/ | Quick Look | ![]() |
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304 | BOOTES GROUP 30 | 219.4427 | 33.5107 | 218.918921 | 33.726455 | 202.46828 | 45.823682 | 55.01212205 | 66.25629851 | 308.903 | 54276.6949189815 | 2007-06-25 16:40:41 | 54277.5271875 | 2007-06-26 12:39:09 | 802056010 | 38.5045 | 38 | 38.5045 | 38.5045 | 0 | 38.5045 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.7473 | 35.7473 | 71.8979 | 1 | PROCESSED | 57539.0466782407 | 2016-05-31 01:07:13 | 54702 | 2008-08-24 00:00:00 | 54333.4389583333 | 2007-08-21 10:32:06 | 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 | B | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802056010/ | Quick Look | ![]() |
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305 | RXJ1159+5531 | 179.9637 | 55.4123 | 179.320531 | 55.690619 | 149.995673 | 49.037125 | 137.70641489 | 60.21165624 | 302.8269 | 56074.0600694445 | 2012-05-27 01:26:30 | 56075.6800578704 | 2012-05-28 16:19:17 | 807064010 | 82.2339 | 100 | 82.2419 | 82.2419 | 0 | 82.2339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.6011 | 98.6011 | 139.964 | 1 | PROCESSED | 57605.5596875 | 2016-08-05 13:25:57 | 56657 | 2013-12-31 00:00:00 | 56086.0194328704 | 2012-06-08 00:27:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071513 | With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | PHILIP HUMPHREY | USA | 7 | AO7 | RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064010/ | Quick Look | ![]() |
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306 | PKS 0745-191 | 116.7966 | -19.5079 | 116.243978 | -19.383587 | 123.623714 | -39.870751 | 236.58636127 | 2.85363493 | 294.0004 | 54234.0374884259 | 2007-05-14 00:53:59 | 54234.8446643518 | 2007-05-14 20:16:19 | 802062050 | 33.4146 | 30 | 33.4146 | 33.4226 | 0 | 33.4226 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.3065 | 31.3065 | 69.7239 | 1 | PROCESSED | 57538.6567708333 | 2016-05-30 15:45:45 | 54695 | 2008-08-17 00:00:00 | 54245.5456712963 | 2007-05-25 13:05:46 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062050/ | Quick Look | ![]() |
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307 | N1550_OFFSET | 65.2479 | 2.4086 | 64.596961 | 2.290593 | 63.774789 | -18.807983 | 191.20173857 | -31.56876902 | 90.0005 | 54693.1139351852 | 2008-08-15 02:44:04 | 54694.185 | 2008-08-16 04:26:24 | 803018010 | 41.1447 | 40 | 41.1447 | 41.1447 | 0 | 41.1447 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29.9469 | 29.9469 | 92.508 | 0 | PROCESSED | 57543.3286226852 | 2016-06-04 07:53:13 | 55079 | 2009-09-05 00:00:00 | 54711.3163310185 | 2008-09-02 07:35:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030070 | We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 3 | AO3 | OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803018010/ | Quick Look | ![]() |
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308 | SHAPLEY OFFSET | 204.9135 | -29.8943 | 204.20662 | -29.641044 | 214.142611 | -18.17761 | 315.23466303 | 31.82297967 | 289.7009 | 54665.2119907407 | 2008-07-18 05:05:16 | 54666.4244675926 | 2008-07-19 10:11:14 | 803021010 | 47.2435 | 40 | 47.2435 | 47.2435 | 0 | 47.2435 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.3578 | 38.3578 | 104.7418 | 0 | PROCESSED | 57543.0903356482 | 2016-06-04 02:10:05 | 55049 | 2009-08-06 00:00:00 | 54682.1908680556 | 2008-08-04 04:34:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030089 | We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 3 | AO3 | SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803021010/ | Quick Look | ![]() |
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309 | TRIANGULUM_AUSTRALIS | 249.6225 | -64.3477 | 248.441517 | -64.24803 | 258.335963 | -41.727543 | 324.61952374 | -11.529112 | 306.6841 | 54750.3809143518 | 2008-10-11 09:08:31 | 54752.6453587963 | 2008-10-13 15:29:19 | 803028010 | 86.0101 | 80 | 86.0421 | 86.0101 | 0 | 86.0481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.9675 | 76.9675 | 195.6378 | 1 | PROCESSED | 57544.1744560185 | 2016-06-05 04:11:13 | 55148 | 2009-11-13 00:00:00 | 54780.7199768518 | 2008-11-10 17:16:46 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030101 | We propose an 80 ks pointed observation of one of the brightest near-by hot and merging galaxy cluster, Triangulum Australis. Recent Suzaku wide-band spectroscopy reveals a very hot (kT >20 keV) thermal component in several merging clusters (RXJ1347, Abell 3667 and so on). On the other hand, relaxed cluster (such as Abell 1060 and Centaurus) show no evidence of such component. These results suggests that the very-hot component is the key aspects of merging cluster. Triangulum Australis is a bright (f ~ 1e-10 cgs), mildly hot (kT ~ 9 keV) and relatively compact (size ~20x20 arcmin2) shaped cluster. ASCA detected a hot region in the center and to the east (Markevitch et al. 1996). Combination of these characteristics makes this cluster the best candidate for our research. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SHO OKUYAMA | JAP | 3 | AO3 | SEARCH FOR VERY-HIGH TEMPERATURE COMPONENT IN A NEAR-BY CLUSTER, TRIANGULUM AUSTRALIS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803028010/ | Quick Look | ![]() |
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310 | ABELL 665 | 127.3329 | 65.7462 | 126.195484 | 65.912794 | 110.615683 | 44.954956 | 149.92967896 | 34.55444535 | 289.9972 | 56027.8062847222 | 2012-04-10 19:21:03 | 56028.5592476852 | 2012-04-11 13:25:19 | 807072030 | 50.3486 | 50 | 50.3526 | 50.3486 | 0 | 50.3561 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.3856 | 47.3856 | 65.049 | 0 | PROCESSED | 57605.1517939815 | 2016-08-05 03:38:35 | 56018 | 2012-04-01 00:00:00 | 56044.1669791667 | 2012-04-27 04:00:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072030/ | Quick Look | ![]() |
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311 | NGC 3079 | 150.444 | 55.6163 | 149.59923 | 55.857396 | 130.078493 | 40.265138 | 157.91350273 | 48.36319014 | 294.1052 | 54590.7432407407 | 2008-05-04 17:50:16 | 54591.1147800926 | 2008-05-05 02:45:17 | 803039010 | 14.4083 | 100 | 14.4083 | 14.4083 | 0 | 14.4083 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.9538 | 12.9538 | 32.0799 | 0 | PROCESSED | 57542.4484027778 | 2016-06-03 10:45:42 | 54999 | 2009-06-17 00:00:00 | 54602.2023958333 | 2008-05-16 04:51:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031303 | We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID STRICKLAND | USA | 3 | AO3 | NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039010/ | Quick Look | ![]() |
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312 | CYGNUS A CLUSTER | 299.7609 | 40.7885 | 299.328588 | 40.65123 | 317.589132 | 59.411403 | 76.19456446 | 5.8531495 | 241.849 | 54785.9049537037 | 2008-11-15 21:43:08 | 54786.9154976852 | 2008-11-16 21:58:19 | 803050010 | 44.6587 | 45 | 44.6587 | 44.6587 | 0 | 44.6587 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.966 | 42.966 | 87.28 | 0 | PROCESSED | 57544.3868055556 | 2016-06-05 09:17:00 | 55167 | 2009-12-02 00:00:00 | 54796.9718981482 | 2008-11-26 23:19:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031426 | The radio galaxy Cygnus A lies in a cooling core cluster which is currently undergoing a cluster merger with a particularly simple geometry. We propose XIS spectra of the radio source/cooling core interaction region, merger shock region, and second subcluster. The Fe K emission line will be used to measure gas velocities in these 3 regions to determine the dynamics of the merger, and to constrain hydro/N-body simulations of the merger. Collisionless merger shocks may produce detectable non-equilibrium effects. We will also determine an upper limit for the rate of expansion of the X-ray bubble around the radio source, studying the interaction of the radio galaxy and X-ray gas in the only FR-II radio galaxy in a nearby cluster. HXD data will constrain inverse Compton from the radio source. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DANIEL WIK | USA | 3 | AO3 | PROPERTIES OF THE MERGER AND RADIO SOURCE INTERACTION IN THE CYGNUS A CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803050010/ | Quick Look | ![]() |
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313 | A2163 | 243.8156 | -6.2315 | 243.147928 | -6.107198 | 243.010913 | 14.789433 | 6.59879538 | 30.51803676 | 282.2871 | 54696.6726851852 | 2008-08-18 16:08:40 | 54700.4008449074 | 2008-08-22 09:37:13 | 803071010 | 135.7864 | 130 | 135.7944 | 135.7864 | 0 | 135.7944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122.1262 | 122.1262 | 322.0615 | 5 | PROCESSED | 57543.4331597222 | 2016-06-04 10:23:45 | 55080 | 2009-09-06 00:00:00 | 54713.5071875 | 2008-09-04 12:10:21 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032023 | Measurements of intracluster gas temperatures out to large radii, where much of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure robust temperatures at cluster virial radii failed. Here, we demonstrate that such measurements are feasible now for the first time with the Suzaku X-ray CCDs, using our observation of the cluster A2204, carefully treating background and PSF. To determine the temperature profile of the cluster population as a whole, more such observations are required. We show that A2163 is the optimal complementary target for such an investigation. We, therefore, propose to observe A2163 to measure the gas temperature to 15% accuracy out to the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | THOMAS REIPRICH | EUR | 3 | AO3 | GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS OF A2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803071010/ | Quick Look | ![]() |
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314 | ABELL 2597 | 351.1561 | -12.0446 | 350.50582 | -12.319475 | 347.114403 | -7.564991 | 65.23010074 | -64.66820365 | 250.0003 | 56262.3308680556 | 2012-12-01 07:56:27 | 56263.5369212963 | 2012-12-02 12:53:10 | 807073020 | 50.0345 | 50 | 50.0585 | 50.0425 | 0 | 50.0345 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44.785 | 44.785 | 104.1919 | 0 | PROCESSED | 57608.1666319444 | 2016-08-08 03:59:57 | 56018 | 2012-04-01 00:00:00 | 56336.4705902778 | 2013-02-13 11:17:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073020/ | Quick Look | ![]() |
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315 | A2029_3 | 227.6311 | 5.4874 | 227.010378 | 5.676114 | 223.4982 | 22.349991 | 6.05366388 | 50.47243927 | 112.9537 | 55224.9801041667 | 2010-01-28 23:31:21 | 55225.6140509259 | 2010-01-29 14:44:14 | 804024030 | 17.9095 | 22 | 17.9175 | 17.9255 | 0 | 17.9095 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.9268 | 8.9268 | 54.7659 | 0 | PROCESSED | 57550.4118865741 | 2016-06-11 09:53:07 | 55637 | 2011-03-17 00:00:00 | 55270.9888425926 | 2010-03-15 23:43:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required 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 breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024030/ | Quick Look | ![]() |
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316 | NGC 4125 | 182.0568 | 65.1777 | 181.434624 | 65.455888 | 140.391429 | 57.000336 | 130.16762444 | 51.33919783 | 175.9017 | 55103.512037037 | 2009-09-29 12:17:20 | 55105.4578009259 | 2009-10-01 10:59:14 | 804047010 | 104.0801 | 100 | 104.0801 | 104.0881 | 0 | 104.0961 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.7257 | 93.7257 | 168.0857 | 0 | PROCESSED | 57548.726712963 | 2016-06-09 17:26:28 | 55491 | 2010-10-22 00:00:00 | 55125.5744212963 | 2009-10-21 13:47:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041502 | Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients, indicating large-scale mixing of the gas, possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku, we have found similar gradients in two lower mass, galaxy-scale systems, which has important implications for models of feedback and chemical enrichment. We propose to observe two more isolated elliptical galaxies, thus starting to building a sample for determining the frequency and properties of such abundance gradients in early-type galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | PHILIP HUMPHREY | USA | 4 | AO4 | ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804047010/ | Quick Look | ![]() |
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317 | FILAMENT OF GALAXIES | 238.8797 | 27.1312 | 238.361126 | 27.276131 | 228.364873 | 46.172986 | 43.89595297 | 49.28386381 | 298.9982 | 55406.9857060185 | 2010-07-29 23:39:25 | 55408.8592939815 | 2010-07-31 20:37:23 | 805029010 | 73.9387 | 80 | 73.9501 | 73.9447 | 0 | 73.9387 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66.4045 | 66.4045 | 161.8557 | 1 | PROCESSED | 57552.8140972222 | 2016-06-13 19:32:18 | 55791 | 2011-08-18 00:00:00 | 55418.4520717593 | 2010-08-10 10:50:59 | 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/ver3.0/805029010/ | Quick Look | ![]() |
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318 | NGC6482 | 267.957 | 23.086 | 267.434837 | 23.097176 | 267.256842 | 46.506557 | 48.10607859 | 22.91404378 | 109.6205 | 55238.2645949074 | 2010-02-11 06:21:01 | 55239.2919444444 | 2010-02-12 07:00:24 | 804050010 | 46.5467 | 45 | 46.5467 | 46.5467 | 0 | 46.5467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.5166 | 28.5166 | 88.7438 | 0 | PROCESSED | 57550.5834143518 | 2016-06-11 14:00:07 | 55622 | 2011-03-02 00:00:00 | 55251.3186458333 | 2010-02-24 07:38:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041513 | Fossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and gas temperatures indicate potential wells deeper than that of normal groups. Their measured c200 are high indicating very early formation epochs, which is in contradiction with the lack of cooling cores observed. We can constrain their ages by looking at the distribution of the SN Ia and II ejecta near their core. If they are formed more recently than normal groups by galaxy merging near the core, the central gas should have a reduction of SN Ia dominance, differently from what is observed in normal groups. We propose to test this with the most optimal and nearest fossil group, NGC6482, matching very well the capabilities of Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RENATO DUPKE | USA | 4 | AO4 | DISCRIMINATING COMPETING MODELS FOR THE ORIGIN OF FOSSIL GROUPS OF GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804050010/ | Quick Look | ![]() |
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319 | NGC741MOSAICE_P4 | 29.8808 | 5.7741 | 29.226568 | 5.531917 | 29.834623 | -6.020542 | 152.02832852 | -53.20754513 | 71.8261 | 55054.5770138889 | 2009-08-11 13:50:54 | 55054.8084953704 | 2009-08-11 19:24:14 | 804052040 | 11.0257 | 10 | 11.0257 | 11.3217 | 0 | 11.3057 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 11.3902 | 11.3902 | 19.9959 | 0 | PROCESSED | 57548.1244328704 | 2016-06-09 02:59:11 | 55448 | 2010-09-09 00:00:00 | 55081.2593055556 | 2009-09-07 06:13:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052040/ | Quick Look | ![]() |
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320 | ABELL 426 E2 | 50.6767 | 41.5228 | 49.847142 | 41.344864 | 59.17553 | 22.199581 | 151.03351832 | -12.94989772 | 90.0008 | 55041.7150115741 | 2009-07-29 17:09:37 | 55041.9654976852 | 2009-07-29 23:10:19 | 804057010 | 12.9048 | 10 | 12.9048 | 12.9048 | 0 | 12.9048 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.962 | 12.962 | 21.6399 | 1 | PROCESSED | 57547.969849537 | 2016-06-08 23:16:35 | 55419 | 2010-08-11 00:00:00 | 55050.2440277778 | 2009-08-07 05:51:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804057010/ | Quick Look | ![]() |
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321 | ABELL 426 N6 | 48.8242 | 42.9264 | 47.990569 | 42.741631 | 58.170143 | 23.930613 | 149.06870737 | -12.52705179 | 59.999 | 55063.8243055556 | 2009-08-20 19:47:00 | 55064.6334837963 | 2009-08-21 15:12:13 | 804068010 | 36.5265 | 30 | 36.5345 | 36.5265 | 0 | 36.5425 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.8843 | 30.8843 | 69.9119 | 0 | PROCESSED | 57548.3037731482 | 2016-06-09 07:17:26 | 55441 | 2010-09-02 00:00:00 | 55075.1362037037 | 2009-09-01 03:16:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804068010/ | Quick Look | ![]() |
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322 | A76 WEST | 9.903 | 6.838 | 9.256884 | 6.56348 | 11.779086 | 2.367721 | 117.68922859 | -55.91332108 | 260 | 55183.8756481482 | 2009-12-18 21:00:56 | 55184.3334953704 | 2009-12-19 08:00:14 | 804088010 | 15.1164 | 15 | 15.1244 | 15.1164 | 0 | 15.1324 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.2066 | 14.2066 | 39.5479 | 0 | PROCESSED | 57549.8934722222 | 2016-06-10 21:26:36 | 55575 | 2011-01-14 00:00:00 | 55209.4668055556 | 2010-01-13 11:12:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042018 | In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HANS BOEHRINGER | EUR | 4 | AO4 | SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804088010/ | Quick Look | ![]() |
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323 | A478 OFFSET D | 63.1009 | 10.3754 | 62.415271 | 10.247963 | 63.081843 | -10.587617 | 182.33525373 | -28.5396849 | 259.0002 | 55612.7107986111 | 2011-02-20 17:03:33 | 55613.7362731482 | 2011-02-21 17:40:14 | 805004010 | 47.1066 | 45 | 47.1066 | 47.1066 | 0 | 47.1066 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 42.161 | 42.161 | 88.5959 | 1 | PROCESSED | 57601.0027314815 | 2016-08-01 00:03:56 | 56018 | 2012-04-01 00:00:00 | 55649.2441203704 | 2011-03-29 05:51:32 | 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/ver3.0/805004010/ | Quick Look | ![]() |
324 | A222/223 BRIDGE | 24.4438 | -12.9141 | 23.829522 | -13.168194 | 17.57702 | -21.440022 | 162.54430913 | -72.12239011 | 224.9995 | 55555.161099537 | 2010-12-25 03:51:59 | 55557.4654861111 | 2010-12-27 11:10:18 | 805035010 | 101.2149 | 100 | 101.2843 | 101.2149 | 0 | 101.2843 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.9171 | 88.9171 | 199.0699 | 4 | PROCESSED | 57554.5537268518 | 2016-06-15 13:17:22 | 55961 | 2012-02-04 00:00:00 | 55595.1387847222 | 2011-02-03 03:19:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050035 | We propose to observe the unusual X-ray bridge connecting the two clusters of galaxies Abell 222 and Abell 223 (z=0.21). XMM observation showed the temperature to be 0.9 keV, interpreted as due to WHIM. Suzaku will observe the temperature distribution over the bridge region, which will tell us the origin of the bridge to be either WHIM or merger onset. Merger process should indicate a characteristic temperature increase. Redshifted oxygen lines, if detected, will be the clear evidence of WHIM. Joint study with weak lensing analysis will show us spatial offset of the dark matter against baryons, helping us to constrain dark matter properties. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAORI HENMI | JAP | 5 | AO5 | ORIGIN OF THE X-RAY BRIDGE CONNECTING THE CLUSTERS OF GALAXIES ABELL 222 AND ABELL 223 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805035010/ | Quick Look | ![]() |
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325 | ABELL1835 OFFSET3 | 210.0673 | 2.8311 | 209.433725 | 3.072798 | 206.943622 | 14.143739 | 340.00426802 | 60.64916276 | 306.4895 | 55385.4673611111 | 2010-07-08 11:13:00 | 55386.9855555556 | 2010-07-09 23:39:12 | 805039010 | 53.6971 | 50 | 53.7201 | 53.7131 | 0 | 53.6971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.8377 | 44.8377 | 131.1598 | 3 | PROCESSED | 57552.5941087963 | 2016-06-13 14:15:31 | 55779 | 2011-08-06 00:00:00 | 55411.2395717593 | 2010-08-03 05:44:59 | 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/ver3.0/805039010/ | Quick Look | ![]() |
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326 | A1413_FIELD_3 | 179.0207 | 23.4251 | 178.377297 | 23.70339 | 169.347727 | 21.006295 | 226.37028623 | 76.95859752 | 302.9994 | 55347.1862037037 | 2010-05-31 04:28:08 | 55348.2079050926 | 2010-06-01 04:59:23 | 805061010 | 40.9225 | 40 | 40.9225 | 40.9385 | 0 | 40.9305 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.9944 | 32.9944 | 88.2578 | 0 | PROCESSED | 57553.3965856482 | 2016-06-14 09:31:05 | 55287 | 2010-04-01 00:00:00 | 55393.4280208333 | 2010-07-16 10:16:21 | 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/ver3.0/805061010/ | Quick Look | ![]() |
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327 | A383_FIELD_2 | 41.9447 | -3.4083 | 41.315431 | -3.616408 | 38.400744 | -18.662791 | 177.53047769 | -53.46482162 | 60.9996 | 55389.1380208333 | 2010-07-12 03:18:45 | 55390.062662037 | 2010-07-13 01:30:14 | 805063010 | 43.3415 | 40 | 43.3575 | 43.3415 | 0 | 43.3575 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.2589 | 39.2589 | 79.8749 | 0 | PROCESSED | 57552.6168055556 | 2016-06-13 14:48:12 | 55287 | 2010-04-01 00:00:00 | 55411.2445601852 | 2010-08-03 05:52:10 | 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/ver3.0/805063010/ | Quick Look | ![]() |
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328 | ABELL1835 OFFSET4 | 210.2225 | 3.0556 | 209.589504 | 3.296921 | 207.010904 | 14.408613 | 340.51868842 | 60.75430015 | 304.9986 | 55390.9913194444 | 2010-07-13 23:47:30 | 55392.4001736111 | 2010-07-15 09:36:15 | 805040010 | 48.8185 | 50 | 48.8265 | 48.8265 | 0 | 48.8185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.9631 | 43.9631 | 121.6839 | 4 | PROCESSED | 57552.6731828704 | 2016-06-13 16:09:23 | 55793 | 2011-08-20 00:00:00 | 55427.1333796296 | 2010-08-19 03:12:04 | 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/ver3.0/805040010/ | Quick Look | ![]() |
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329 | A1914_OFFSET2 | 216.7383 | 37.763 | 216.226328 | 37.986791 | 196.709268 | 48.583272 | 66.87630822 | 67.3091462 | 329.9943 | 55363.4747569444 | 2010-06-16 11:23:39 | 55364.3800115741 | 2010-06-17 09:07:13 | 805092010 | 28.5462 | 40 | 28.5542 | 28.5542 | 0 | 28.5462 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.8343 | 25.8343 | 78.204 | 0 | PROCESSED | 57552.3515856482 | 2016-06-13 08:26:17 | 55766 | 2011-07-24 00:00:00 | 55399.3275231482 | 2010-07-22 07:51:38 | 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/ver3.0/805092010/ | Quick Look | ![]() |
330 | CENA N LOBE 3 | 201.1567 | -39.315 | 200.435438 | -39.054679 | 215.153584 | -28.04573 | 309.90401242 | 23.10702351 | 110.949 | 56316.327349537 | 2013-01-24 07:51:23 | 56318.4140046296 | 2013-01-26 09:56:10 | 807134010 | 81.984 | 75 | 81.992 | 81.992 | 0 | 81.984 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.8838 | 73.8838 | 180.2478 | 2 | PROCESSED | 57608.6528356482 | 2016-08-08 15:40:05 | 56708 | 2014-02-20 00:00:00 | 56342.7001157407 | 2013-02-19 16:48:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070127 | Radio source Centaurus A is the closest active galaxy in the Universe (3.7 Mpc). It is surrounded by poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose Chandra follow-up of four regions in the Southern and Northern lobes where Suzaku time was allocated. We also propose joint Chandra-Suzaku observation toward interacting filamentary region where ASCA found a hint of X-ray emission. 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 inhomogeneous and multi-phase plasma. The obtained results are guaranteed to improve our knowledge regarding not only the Centaurus A, but all jetted active galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | YASUYUKI TANAKA | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES OF CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807134010/ | Quick Look | ![]() |
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331 | NGC 2300 OFFSET | 116.7261 | 85.6829 | 112.689891 | 85.799301 | 94.232742 | 62.638745 | 127.68344404 | 28.08274711 | 339.9009 | 55235.4123148148 | 2010-02-08 09:53:44 | 55235.7606365741 | 2010-02-08 18:15:19 | 804031010 | 19.196 | 20 | 19.196 | 19.196 | 0 | 19.196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.1477 | 17.1477 | 30.0879 | 0 | PROCESSED | 57550.5104282407 | 2016-06-11 12:15:01 | 55633 | 2011-03-13 00:00:00 | 55266.1898148148 | 2010-03-11 04:33:20 | 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/ver3.0/804031010/ | Quick Look | ![]() |
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332 | MKW 4-OFFSET1 | 181.1304 | 2.2289 | 180.489911 | 2.507266 | 180.147119 | 2.494288 | 276.66004128 | 62.68282085 | 114.5816 | 55528.2862847222 | 2010-11-28 06:52:15 | 55530.2501967593 | 2010-11-30 06:00:17 | 805081010 | 79.4261 | 80 | 79.4261 | 79.4261 | 0 | 79.4261 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68.2112 | 68.2112 | 169.6679 | 2 | PROCESSED | 57554.312025463 | 2016-06-15 07:29:19 | 55909 | 2011-12-14 00:00:00 | 55543.4043402778 | 2010-12-13 09:42:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051525 | We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIO GASTALDELLO | USA | 5 | AO5 | THE OUTSKIRTS OF MKW 4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805081010/ | Quick Look | ![]() |
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333 | PKS 0745-191 | 116.3632 | -19.0871 | 115.808852 | -18.964679 | 122.979801 | -39.556071 | 236.01662317 | 2.71025988 | 294.0001 | 55316.6424189815 | 2010-04-30 15:25:05 | 55317.3675231482 | 2010-05-01 08:49:14 | 805085010 | 34.9999 | 35 | 34.9999 | 34.9999 | 0 | 34.9999 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.7804 | 32.7804 | 62.6419 | 2 | PROCESSED | 57551.3324074074 | 2016-06-12 07:58:40 | 55696 | 2011-05-15 00:00:00 | 55330.1114236111 | 2010-05-14 02:40:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805085010/ | Quick Look | ![]() |
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334 | A1914_OFFSET4 | 216.4424 | 37.6372 | 215.928949 | 37.861845 | 196.491265 | 48.360248 | 66.78881215 | 67.57279807 | 134.0011 | 55566.4311574074 | 2011-01-05 10:20:52 | 55566.8258912037 | 2011-01-05 19:49:17 | 805094020 | 17.3531 | 12 | 17.3531 | 17.3611 | 0 | 17.3691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.0606 | 16.0606 | 34.1 | 0 | PROCESSED | 57600.564375 | 2016-07-31 13:32:42 | 55995 | 2012-03-09 00:00:00 | 55627.1583333333 | 2011-03-07 03:48:00 | 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 | 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/ver3.0/805094020/ | Quick Look | ![]() |
335 | ABELL 426 S2 | 49.8015 | 40.983 | 48.977877 | 40.801825 | 58.333099 | 21.861106 | 150.77920085 | -13.76419767 | 87.9994 | 55425.2999884259 | 2010-08-17 07:11:59 | 55425.5946527778 | 2010-08-17 14:16:18 | 805097010 | 10.9046 | 10 | 10.9347 | 10.9286 | 0 | 10.9046 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.2387 | 8.2387 | 25.4559 | 0 | PROCESSED | 57553.0977546296 | 2016-06-14 02:20:46 | 55287 | 2010-04-01 00:00:00 | 55439.1113888889 | 2010-08-31 02:40:24 | 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/ver3.0/805097010/ | Quick Look | ![]() |
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336 | OPHIUCHUS CLUSTER BG | 257.0147 | -25.0612 | 256.247464 | -24.996818 | 258.237934 | -2.148508 | 358.58755189 | 9.10838139 | 89.7146 | 54183.5662268518 | 2007-03-24 13:35:22 | 54183.9169444444 | 2007-03-24 22:00:24 | 801030010 | 15.2983 | 15 | 15.3063 | 15.3063 | 0 | 15.2983 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6351 | 14.6351 | 30.296 | 0 | PROCESSED | 57537.9841898148 | 2016-05-29 23:37:14 | 54736 | 2008-09-27 00:00:00 | 54209.5187384259 | 2007-04-19 12:26:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801030010/ | Quick Look | ![]() |
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337 | ABELL 426 S7 | 49.4762 | 39.609 | 48.662108 | 39.426644 | 57.669776 | 20.609139 | 151.34578769 | -15.04805542 | 88.0004 | 55427.7102430556 | 2010-08-19 17:02:45 | 55428.0731481482 | 2010-08-20 01:45:20 | 805102010 | 17.2093 | 15 | 17.2093 | 17.2333 | 0 | 17.2173 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.7954 | 13.7954 | 31.3479 | 0 | PROCESSED | 57553.1341550926 | 2016-06-14 03:13:11 | 55287 | 2010-04-01 00:00:00 | 55439.2187847222 | 2010-08-31 05:15:03 | 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/ver3.0/805102010/ | Quick Look | ![]() |
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338 | ABELL 426 W2 | 49.2188 | 41.5721 | 48.392989 | 41.388782 | 58.056414 | 22.549036 | 150.07049245 | -13.51031958 | 93.9951 | 55428.7403240741 | 2010-08-20 17:46:04 | 55428.9654513889 | 2010-08-20 23:10:15 | 805104010 | 9.9892 | 10 | 9.9972 | 9.9972 | 0 | 9.9892 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.2787 | 7.2787 | 19.4479 | 1 | PROCESSED | 57553.1453240741 | 2016-06-14 03:29:16 | 55287 | 2010-04-01 00:00:00 | 55460.9467708333 | 2010-09-21 22:43:21 | 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/ver3.0/805104010/ | Quick Look | ![]() |
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339 | ABELL 1795 Far South | 207.2227 | 26.2001 | 206.644395 | 26.44826 | 194.131601 | 34.631873 | 32.0541753 | 77.13779505 | 129.4115 | 53716.5361921296 | 2005-12-12 12:52:07 | 53717.4168865741 | 2005-12-13 10:00:19 | 800012050 | 40.1206 | 30 | 40.1366 | 40.1526 | 40.1206 | 40.1366 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.4373 | 39.4373 | 76.0819 | 1 | PROCESSED | 57532.4477314815 | 2016-05-24 10:44:44 | 54247 | 2007-05-27 00:00:00 | 54039.1460069445 | 2006-10-31 03:30:15 | 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/ver3.0/800012050/ | Quick Look | ![]() |
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340 | FORNAX OFFSET2 | 54.357 | -35.2813 | 53.876494 | -35.444531 | 38.536942 | -52.548461 | 236.43807346 | -53.85479755 | 63.6004 | 54663.2151388889 | 2008-07-16 05:09:48 | 54664.1793287037 | 2008-07-17 04:18:14 | 803007010 | 40.6477 | 30 | 40.678 | 40.6717 | 0 | 40.6477 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.8358 | 34.8358 | 83.2979 | 0 | PROCESSED | 57595.6271875 | 2016-07-26 15:03:09 | 55188 | 2009-12-23 00:00:00 | 54822.5201736111 | 2008-12-22 12:29:03 | 3.0.22.44 | 3 | 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/ver3.0/803007010/ | Quick Look | ![]() |
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341 | ABELL 3112 | 49.4982 | -44.2507 | 49.063827 | -44.432376 | 25.5219 | -58.972557 | 252.95298598 | -56.06981795 | 43.5004 | 56466.5743634259 | 2013-06-23 13:47:05 | 56468.5418055556 | 2013-06-25 13:00:12 | 808068010 | 119.1247 | 200 | 119.1247 | 119.1247 | 0 | 119.1247 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.5618 | 114.5618 | 169.9418 | 0 | PROCESSED | 57611.6340856482 | 2016-08-11 15:13:05 | 56848 | 2014-07-10 00:00:00 | 56481.8003356482 | 2013-07-08 19:12:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081522 | 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 | USA | 8 | AO8 | CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068010/ | Quick Look | ![]() |
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342 | RXCJ0243.6-4834 | 40.9015 | -48.5654 | 40.467277 | -48.776586 | 11.225079 | -59.344649 | 265.11995755 | -59.50535864 | 228.2843 | 55191.5472685185 | 2009-12-26 13:08:04 | 55192.0001967593 | 2009-12-27 00:00:17 | 804001010 | 13.2059 | 10 | 13.2139 | 13.2059 | 0 | 13.2219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.5448 | 10.5448 | 39.1299 | 0 | PROCESSED | 57549.9594097222 | 2016-06-10 23:01:33 | 55575 | 2011-01-14 00:00:00 | 55209.1119328704 | 2010-01-13 02:41:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804001010/ | Quick Look | ![]() |
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343 | ABELL 426 S6.5 | 49.508 | 39.7472 | 48.692971 | 39.56496 | 57.735719 | 20.735211 | 151.28830519 | -14.91915669 | 87.9995 | 55427.3325115741 | 2010-08-19 07:58:49 | 55427.7099537037 | 2010-08-19 17:02:20 | 805112010 | 15.7046 | 15 | 15.7126 | 15.7046 | 0 | 15.7205 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.4033 | 14.4033 | 32.6079 | 0 | PROCESSED | 57553.1322222222 | 2016-06-14 03:10:24 | 55287 | 2010-04-01 00:00:00 | 55439.1853587963 | 2010-08-31 04:26:55 | 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/ver3.0/805112010/ | Quick Look | ![]() |
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344 | ABELL2811 | 10.4703 | -28.5552 | 9.856516 | -28.82929 | 357.097887 | -30.138768 | 358.34166022 | -87.45073592 | 232.1065 | 53702.1678240741 | 2005-11-28 04:01:40 | 53702.8814699074 | 2005-11-28 21:09:19 | 800005010 | 30.6546 | 25 | 30.6626 | 30.6826 | 30.6546 | 30.6659 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28.3254 | 28.3254 | 61.656 | 0 | PROCESSED | 57528.0937268518 | 2016-05-20 02:14:58 | 54247 | 2007-05-27 00:00:00 | 54038.5109722222 | 2006-10-30 12:15:48 | 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/ver3.0/800005010/ | Quick Look | ![]() |
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345 | A2199 OFFSET9 | 246.619 | 38.9138 | 246.184603 | 39.025211 | 232.691568 | 59.360139 | 62.03199075 | 44.09189055 | 267.0002 | 55816.7374652778 | 2011-09-12 17:41:57 | 55817.4077546296 | 2011-09-13 09:47:10 | 806155010 | 28.1304 | 30 | 28.1304 | 28.1304 | 0 | 28.1304 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 27.0303 | 27.0303 | 57.8979 | 0 | PROCESSED | 57603.128287037 | 2016-08-03 03:04:44 | 55652 | 2011-04-01 00:00:00 | 55851.4428356482 | 2011-10-17 10:37:41 | 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/ver3.0/806155010/ | Quick Look | ![]() |
346 | ABELL 426 W4.5 | 48.2846 | 41.6054 | 47.461248 | 41.418696 | 57.340677 | 22.779589 | 149.44545041 | -13.85744176 | 86.9992 | 55429.5700347222 | 2010-08-21 13:40:51 | 55429.7800694444 | 2010-08-21 18:43:18 | 805114010 | 10.8576 | 10 | 10.8796 | 10.8656 | 0 | 10.8576 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.7343 | 7.7343 | 18.1439 | 0 | PROCESSED | 57553.1551388889 | 2016-06-14 03:43:24 | 55287 | 2010-04-01 00:00:00 | 55445.224224537 | 2010-09-06 05:22:53 | 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/ver3.0/805114010/ | Quick Look | ![]() |
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347 | ABELL 426 W6.5 | 47.5391 | 41.63 | 46.717762 | 41.440629 | 56.769366 | 22.964447 | 148.94387316 | -14.13011853 | 94.0011 | 55430.6970601852 | 2010-08-22 16:43:46 | 55431.0425578704 | 2010-08-23 01:01:17 | 805116010 | 15.4086 | 15 | 16.0162 | 15.4086 | 0 | 16.0482 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.5812 | 12.5812 | 29.8399 | 0 | PROCESSED | 57553.1669560185 | 2016-06-14 04:00:25 | 55287 | 2010-04-01 00:00:00 | 55449.2772916667 | 2010-09-10 06:39:18 | 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/ver3.0/805116010/ | Quick Look | ![]() |
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348 | MACSJ0717.5+3547 | 109.4283 | 37.7329 | 108.583729 | 37.823554 | 105.833167 | 15.353649 | 180.28338253 | 21.07400371 | 90.0014 | 55841.8814699074 | 2011-10-07 21:09:19 | 55844.0440046296 | 2011-10-10 01:03:22 | 806006010 | 100.5473 | 100 | 100.5473 | 100.5553 | 0 | 100.5553 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.847 | 93.847 | 186.8279 | 1 | PROCESSED | 57603.4085763889 | 2016-08-03 09:48:21 | 56240 | 2012-11-09 00:00:00 | 55872.2982523148 | 2011-11-07 07:09:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060016 | MACSJ0717.5+3547 is a forming hot cluster located at z=0.55. Chandra observation resolved a >20 keV hot component near its center, in addition to the average ICM temperature of 11.6 keV. With the most luminous radio halo observed to date, the cluster is in a moment of major merging event. It is also associated with a stream of galaxies oriented to the south east. We propose a Suzaku observation with an exposure of 100 ks, aiming at; confirming the bright > 20 keV component, the very hot component (e.g. Nakazawa+ 2010) evidencing the strong merger, and obtain temperature map of the dim diffuse X-ray observed to the south east and the south west to resolve the nature of these emission. With these observation, merging orientation and phase in this very hot cluster can be resolved. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAZUHIRO NAKAZAWA | JAP | 6 | AO6 | OBSERVING THE FORMATION EPOCH OF A HOT CLUSTER : SUZAKU OBSERVATION OF MACSJ0717.5+3547 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806006010/ | Quick Look | ![]() |
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349 | A426 | 49.9554 | 41.5039 | 49.127963 | 41.323287 | 58.608686 | 22.329679 | 150.58326426 | -13.26576669 | 260.2176 | 53767.568900463 | 2006-02-01 13:39:13 | 53768.5294560185 | 2006-02-02 12:42:25 | 800010010 | 50.3986 | 50 | 50.4066 | 50.4066 | 50.3986 | 50.4066 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54.4364 | 54.4364 | 82.9758 | 0 | PROCESSED | 57532.8781365741 | 2016-05-24 21:04:31 | 54247 | 2007-05-27 00:00:00 | 54041.0862152778 | 2006-11-02 02:04:09 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001036 | A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW FABIAN | JAP | 0 | SWG | THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800010010/ | Quick Look | ![]() |
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350 | COMA OUTSKIRTS5 | 193.6628 | 28.7109 | 193.057562 | 28.981718 | 179.928046 | 31.541197 | 98.9627641 | 88.26548083 | 115.9998 | 55903.9110532407 | 2011-12-08 21:51:55 | 55904.722349537 | 2011-12-09 17:20:11 | 806024010 | 31.635 | 30 | 31.659 | 31.651 | 0 | 31.635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.4491 | 29.4491 | 70.0899 | 0 | PROCESSED | 57604.0811226852 | 2016-08-04 01:56:49 | 56284 | 2012-12-23 00:00:00 | 55915.2478587963 | 2011-12-20 05:56:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806024010/ | Quick Look | ![]() |
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351 | ABELL 773 | 139.6415 | 51.5835 | 138.770726 | 51.794221 | 124.818527 | 33.970374 | 166.25628799 | 43.50358503 | 276.9979 | 55683.2110185185 | 2011-05-02 05:03:52 | 55684.0730208333 | 2011-05-03 01:45:09 | 806027020 | 47.2223 | 50 | 47.2303 | 47.2223 | 0 | 47.2383 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5115 | 46.5115 | 74.4719 | 0 | PROCESSED | 57601.9085185185 | 2016-08-01 21:48:16 | 55652 | 2011-04-01 00:00:00 | 55697.3168981482 | 2011-05-16 07:36:20 | 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/ver3.0/806027020/ | Quick Look | ![]() |
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352 | CENCL OFFSET2 | 192.2009 | -41.1804 | 191.510431 | -40.907877 | 208.999282 | -32.736275 | 302.39848339 | 21.68862024 | 106.52 | 53733.2507407407 | 2005-12-29 06:01:04 | 53734.3543865741 | 2005-12-30 08:30:19 | 800016010 | 43.2773 | 40 | 43.2853 | 43.2853 | 43.2773 | 43.2933 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35.2531 | 35.2531 | 95.332 | 1 | PROCESSED | 57532.5900578704 | 2016-05-24 14:09:41 | 54247 | 2007-05-27 00:00:00 | 54039.6041203704 | 2006-10-31 14:29:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800016010/ | Quick Look | ![]() |
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353 | NGC 4636 | 190.7243 | 2.7556 | 190.086173 | 3.029415 | 188.766391 | 6.778722 | 297.77503713 | 65.54179663 | 112.2967 | 53710.1073726852 | 2005-12-06 02:34:37 | 53711.9446643518 | 2005-12-07 22:40:19 | 800018010 | 79.201 | 80 | 79.201 | 79.201 | 79.201 | 79.201 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75.7771 | 75.7771 | 158.7278 | 2 | PROCESSED | 57532.4099421296 | 2016-05-24 09:50:19 | 54247 | 2007-05-27 00:00:00 | 54038.9551388889 | 2006-10-30 22:55:24 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001083 | We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ENECTALI FIGUEROA-FELICIANO | JAP | 0 | SWG | OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800018010/ | Quick Look | ![]() |
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354 | AWM7 WEST OFFSET | 43.2295 | 41.594 | 42.421509 | 41.389857 | 53.412323 | 23.911285 | 146.06522235 | -15.7568529 | 90.4999 | 53953.2407060185 | 2006-08-06 05:46:37 | 53954.2343171296 | 2006-08-07 05:37:25 | 801037010 | 39.8177 | 40 | 39.8497 | 39.8177 | 39.8497 | 39.8497 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38.1089 | 38.1089 | 85.8359 | 1 | PROCESSED | 57535.2509375 | 2016-05-27 06:01:21 | 54394 | 2007-10-21 00:00:00 | 54020.7562384259 | 2006-10-12 18:08:59 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801037010/ | Quick Look | ![]() |
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355 | ABELL 2667 | 357.7341 | -26.0226 | 357.087227 | -26.30077 | 347.004408 | -22.85609 | 34.17814736 | -76.43580815 | 64.8804 | 55722.9055208333 | 2011-06-10 21:43:57 | 55724.4196990741 | 2011-06-12 10:04:22 | 806029020 | 51.6577 | 50 | 51.6657 | 51.6577 | 0 | 51.6721 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.656 | 45.656 | 130.802 | 1 | PROCESSED | 57602.2808333333 | 2016-08-02 06:44:24 | 55652 | 2011-04-01 00:00:00 | 55757.7009027778 | 2011-07-15 16:49:18 | 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/ver3.0/806029020/ | Quick Look | ![]() |
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356 | COMA E6.5 | 196.9526 | 27.8857 | 196.354379 | 28.152377 | 183.408228 | 32.112773 | 45.6576416 | 86.29162208 | 279.9993 | 55731.5902199074 | 2011-06-19 14:09:55 | 55732.0578935185 | 2011-06-20 01:23:22 | 806037010 | 14.9596 | 15 | 14.9676 | 14.9596 | 0 | 14.9676 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.6142 | 13.6142 | 40.3999 | 0 | PROCESSED | 57602.3577314815 | 2016-08-02 08:35:08 | 55652 | 2011-04-01 00:00:00 | 55770.17125 | 2011-07-28 04:06:36 | 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/ver3.0/806037010/ | Quick Look | ![]() |
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357 | COMA SW7 | 193.2936 | 26.7739 | 192.684688 | 27.045132 | 180.600519 | 29.664204 | 350.54999025 | 89.47529971 | 314.5993 | 55737.124212963 | 2011-06-25 02:58:52 | 55737.4447106482 | 2011-06-25 10:40:23 | 806051010 | 15.4152 | 15 | 15.4152 | 15.4232 | 0 | 15.4232 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.0368 | 15.0368 | 27.6719 | 0 | PROCESSED | 57602.4087847222 | 2016-08-02 09:48:39 | 55652 | 2011-04-01 00:00:00 | 55795.0185763889 | 2011-08-22 00:26:45 | 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/ver3.0/806051010/ | Quick Look | ![]() |
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358 | A2256 | 256.0138 | 78.7112 | 256.73222 | 78.776756 | 102.386288 | 77.234603 | 111.08264828 | 31.72462704 | 207.9671 | 54049.8560069445 | 2006-11-10 20:32:39 | 54052.0834722222 | 2006-11-13 02:00:12 | 801061010 | 95.5111 | 100 | 95.5111 | 95.5111 | 0 | 95.5111 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103.5789 | 103.5789 | 192.4418 | 4 | PROCESSED | 57536.1203009259 | 2016-05-28 02:53:14 | 54456 | 2007-12-22 00:00:00 | 54089.4338425926 | 2006-12-20 10:24:44 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010139 | A2256 is a nearby (z=0.058) rich cluster with strong X-ray emission. The cluster has variety of indications of a on-going merger; two peaks separated by 3.5 arcmin are clearly visible near the center of X-ray emission, gas temperature map show sub structure and a cold front etc. The velocity distribution of member galaxies also exhibits two or three sub groups in this cluster. We measure the bulk motion of the hot gas using Suzaku XIS, in particular, about 2000km/s velocity difference between the main-cluster and the sub-cluster is the target. We also aim to search for hard X-ray emission claimed by previous missions with Suzaku HXD. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KIYOSHI HAYASHIDA | JAP | 1 | AO1 | BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801061010/ | Quick Look | ![]() |
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359 | 30 DORADUS | 84.6512 | -69.1008 | 84.737262 | -69.126573 | 305.902613 | -86.759222 | 279.46621821 | -31.68092384 | 162.7542 | 55895.6278472222 | 2011-11-30 15:04:06 | 55897.0640162037 | 2011-12-02 01:32:11 | 806052010 | 101.6448 | 100 | 101.6528 | 101.6528 | 0 | 101.6448 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.0823 | 89.0823 | 124.076 | 0 | PROCESSED | 57604.044837963 | 2016-08-04 01:04:34 | 56281 | 2012-12-20 00:00:00 | 55907.9795486111 | 2011-12-12 23:30:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061322 | We propose a deep Suzaku observation of 30 Doradus to provide a direct X-ray measurement of the chemical enrichment in the enclosed hot gas. The soft X-ray sensitivity and spectral resolution of this observation will allow us to measure key elemental abundances and thus to test models for metal yields of massive stars. We will determine the spatial variation in the thermal and chemical properties of the hot gas and the effect on the global estimation of the chemical enrichment from an integrated spectrum, as would be obtained for a distant starburst region. We will also estimate the mass-loading from the general interstellar medium --- a key parameter for determining the evolution of the hot gas. The results will serve as an observational benchmark for understanding massive star feedback. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | Q. DANIEL WANG | USA | 6 | AO6 | X-RAY SPECTROSCOPIC MAPPING OF 30 DORADUS: CHEMICAL ENRICHMENT BY MASSIVE STARS IN A CLOSED BOX | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806052010/ | Quick Look | ![]() |
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360 | RCS131723-0201.3 | 199.3422 | -2.034 | 198.698505 | -1.770799 | 198.620431 | 5.687336 | 316.04491283 | 60.17589221 | 291.8811 | 55756.3454513889 | 2011-07-14 08:17:27 | 55756.9585532407 | 2011-07-14 23:00:19 | 806078010 | 24.921 | 25 | 24.921 | 24.921 | 0 | 24.921 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.1205 | 23.1205 | 52.9619 | 1 | PROCESSED | 57602.5803009259 | 2016-08-02 13:55:38 | 56163 | 2012-08-24 00:00:00 | 55783.6867939815 | 2011-08-10 16:28:59 | 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/ver3.0/806078010/ | Quick Look | ![]() |
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361 | UGC03957 WEST | 114.5487 | 55.2415 | 113.541037 | 55.354916 | 106.445391 | 33.192967 | 162.38027408 | 28.51701147 | 289.9984 | 56004.175150463 | 2012-03-18 04:12:13 | 56005.2466550926 | 2012-03-19 05:55:11 | 806093010 | 48.2169 | 45 | 48.2249 | 48.2169 | 0 | 48.2249 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46.846 | 46.846 | 92.5679 | 0 | PROCESSED | 57604.9538773148 | 2016-08-04 22:53:35 | 56388 | 2013-04-06 00:00:00 | 56020.0984837963 | 2012-04-03 02:21:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BRENDA MIRANDA OCEJO | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806093010/ | Quick Look | ![]() |
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362 | SERSIC 159-03 | 348.4959 | -42.7314 | 347.802109 | -43.003937 | 330.666566 | -34.355163 | 348.33340728 | -64.81387916 | 47.3295 | 53851.5323611111 | 2006-04-26 12:46:36 | 53853.2668055556 | 2006-04-28 06:24:12 | 801093010 | 67.7843 | 70 | 67.8003 | 67.8003 | 67.7843 | 67.7923 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41.5833 | 41.5833 | 149.8278 | 2 | PROCESSED | 57533.6210532407 | 2016-05-25 14:54:19 | 54400 | 2007-10-27 00:00:00 | 53907.8625231482 | 2006-06-21 20:42:02 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012045 | We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JELLE KAASTRA | EUR | 1 | AO1 | O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN? | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801093010/ | Quick Look | ![]() |
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363 | FORNAX CLUSTER N30' | 54.7324 | -34.9521 | 54.250694 | -35.113851 | 39.207877 | -52.359999 | 235.87381769 | -53.55297023 | 245 | 54479.2031134259 | 2008-01-14 04:52:29 | 54480.3542708333 | 2008-01-15 08:30:09 | 802021010 | 55.8107 | 53 | 55.8107 | 55.8107 | 0 | 55.8107 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.3441 | 58.3441 | 99.4438 | 2 | PROCESSED | 57541.3134259259 | 2016-06-02 07:31:20 | 54864 | 2009-02-02 00:00:00 | 54490.3658680556 | 2008-01-25 08:46:51 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020038 | To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 2 | AO2 | DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802021010/ | Quick Look | ![]() |
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364 | NGC 4636 NORTH | 190.6832 | 3.0555 | 190.045327 | 3.32935 | 188.609453 | 7.038209 | 297.61641621 | 65.83736523 | 111.9967 | 54441.2091087963 | 2007-12-07 05:01:07 | 54443.0530555556 | 2007-12-09 01:16:24 | 802022010 | 71.4294 | 67 | 0 | 71.4294 | 0 | 71.4294 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 61.781 | 61.781 | 159.3101 | 3 | PROCESSED | 57540.8428703704 | 2016-06-01 20:13:44 | 55000 | 2009-06-18 00:00:00 | 54633.6943402778 | 2008-06-16 16:39:51 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020038 | To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 2 | AO2 | DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802022010/ | Quick Look | ![]() |
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365 | THE MOON | 142.9239 | 10.1507 | 142.252683 | 10.371816 | 141.955643 | -4.265217 | 222.87402657 | 40.10832518 | 105.6986 | 56975.5846296296 | 2014-11-14 14:01:52 | 56975.7154166667 | 2014-11-14 17:10:12 | 809001230 | 5.1848 | 45 | 5.1848 | 5.2128 | 0 | 5.2208 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7753009259 | 2016-08-16 18:36:26 | 57358 | 2015-12-02 00:00:00 | 56992.4173148148 | 2014-12-01 10:00:56 | 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/ver3.0/809001230/ | Quick Look | ![]() |
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366 | A2052_GALACTIC_1 | 225.6293 | 8.2927 | 225.017778 | 8.488428 | 220.521255 | 24.436359 | 7.81905694 | 53.73503279 | 292.5625 | 54295.7150810185 | 2007-07-14 17:09:43 | 54296.5765509259 | 2007-07-15 13:50:14 | 802038010 | 33.7334 | 30 | 33.7334 | 33.7334 | 0 | 33.7334 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30.5272 | 30.5272 | 74.4239 | 1 | PROCESSED | 57539.2674305556 | 2016-05-31 06:25:06 | 54709 | 2008-08-31 00:00:00 | 54339.4114583333 | 2007-08-27 09:52:30 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOH TAKEI | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802038010/ | Quick Look | ![]() |
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367 | ABELL 3395 | 96.7698 | -54.5043 | 96.516816 | -54.472103 | 108.474853 | -77.510268 | 263.27498484 | -25.21804833 | 150.0003 | 54815.4865046296 | 2008-12-15 11:40:34 | 54817.3168865741 | 2008-12-17 07:36:19 | 803020010 | 104.3469 | 100 | 104.3469 | 104.3469 | 0 | 104.3469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.661 | 81.661 | 158.1299 | 3 | PROCESSED | 57545.0306828704 | 2016-06-06 00:44:11 | 55210 | 2010-01-14 00:00:00 | 54840.5412268518 | 2009-01-09 12:59:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030078 | We propose to observe a merging cluster Abell 3395 with Suzaku for 100 ks. Abell 3395 has two X-ray emission peaks in the ICM, and they can have a large velocity difference of 3000 km/s at maximum. From the line shift of iron K line, we detect the bulk motion of the ICM, and compare it with the velocity distribution of galaxies. The difference of velocity distributions between the ICM and galaxies reflects the difference of their cross sections during the cluster merging. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 3 | AO3 | COMPARISON BETWEEN VELOCITY DISTRIBUTIONS OF ICM AND GALAXIES IN A MERGING CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803020010/ | Quick Look | ![]() |
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368 | ABELL 426 SW2.5 | 49.2375 | 41.0889 | 48.414756 | 40.905656 | 57.924284 | 22.08131 | 150.35281041 | -13.90838125 | 95.0009 | 55800.8414467593 | 2011-08-27 20:11:41 | 55801.0598611111 | 2011-08-28 01:26:12 | 806101010 | 10.6344 | 10 | 10.6584 | 10.6504 | 0 | 10.6344 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.3417 | 10.3417 | 18.8559 | 0 | PROCESSED | 57602.9850925926 | 2016-08-02 23:38:32 | 55652 | 2011-04-01 00:00:00 | 55818.1410069444 | 2011-09-14 03:23:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806101010/ | Quick Look | ![]() |
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369 | PKS 0745-191 | 116.9737 | -19.0727 | 116.418821 | -18.947622 | 123.702706 | -39.408553 | 236.29361594 | 3.21678926 | 294.0001 | 54232.5006712963 | 2007-05-12 12:00:58 | 54233.2258564815 | 2007-05-13 05:25:14 | 802062030 | 30.7942 | 30 | 30.8022 | 30.7942 | 0 | 30.8022 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.6388 | 26.6388 | 62.6301 | 0 | PROCESSED | 57538.6331134259 | 2016-05-30 15:11:41 | 54695 | 2008-08-17 00:00:00 | 54245.5042592593 | 2007-05-25 12:06:08 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062030/ | Quick Look | ![]() |
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370 | RXCJ2157.4-0747 NW | 329.1863 | -7.8673 | 328.525365 | -8.105597 | 328.55802 | 4.374692 | 49.60582387 | -44.43308021 | 249.9998 | 56972.0423726852 | 2014-11-11 01:01:01 | 56972.5418171296 | 2014-11-11 13:00:13 | 809020010 | 23.1307 | 20 | 23.1307 | 23.1307 | 0 | 23.1307 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7608101852 | 2016-08-16 18:15:34 | 57352 | 2015-11-26 00:00:00 | 56986.4053819444 | 2014-11-25 09:43:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809020010/ | Quick Look | ![]() |
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371 | ABELL 426 SW5 | 48.5394 | 40.6338 | 47.721481 | 40.448025 | 57.239803 | 21.793555 | 150.14795961 | -14.57654163 | 88.4979 | 55802.0865856482 | 2011-08-29 02:04:41 | 55802.4896875 | 2011-08-29 11:45:09 | 806106010 | 16.7241 | 15 | 16.7401 | 16.7241 | 0 | 16.7481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.0406 | 13.0406 | 34.8239 | 0 | PROCESSED | 57602.9971990741 | 2016-08-02 23:55:58 | 55652 | 2011-04-01 00:00:00 | 55826.1207638889 | 2011-09-22 02:53:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806106010/ | Quick Look | ![]() |
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372 | ABELL 426 SE2.5 | 50.5437 | 41.0145 | 49.717849 | 40.836073 | 58.92258 | 21.737665 | 151.24059841 | -13.42708975 | 89.5612 | 55797.9346180556 | 2011-08-24 22:25:51 | 55798.1676041667 | 2011-08-25 04:01:21 | 806113010 | 11.0423 | 10 | 11.0503 | 11.0583 | 0 | 11.0423 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6711 | 9.6711 | 20.1199 | 0 | PROCESSED | 57602.9433217593 | 2016-08-02 22:38:23 | 55652 | 2011-04-01 00:00:00 | 55855.134849537 | 2011-10-21 03:14:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806113010/ | Quick Look | ![]() |
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373 | ABELL 426 NE3.5 | 50.9699 | 42.1175 | 50.135538 | 41.940653 | 59.578071 | 22.712479 | 150.87690614 | -12.33503289 | 89.4979 | 55809.4033333333 | 2011-09-05 09:40:48 | 55809.6251273148 | 2011-09-05 15:00:11 | 806127010 | 10.32 | 10 | 10.332 | 10.32 | 0 | 10.336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.379 | 9.379 | 19.156 | 0 | PROCESSED | 57603.0714583333 | 2016-08-03 01:42:54 | 55652 | 2011-04-01 00:00:00 | 55866.0295833333 | 2011-11-01 00:42:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806127010/ | Quick Look | ![]() |
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374 | COMA11 | 194.6305 | 28.3939 | 194.027281 | 28.663593 | 180.9862 | 31.643484 | 72.26601068 | 87.98563538 | 292.5148 | 54270.6441782407 | 2007-06-19 15:27:37 | 54272.0078009259 | 2007-06-21 00:11:14 | 802082010 | 53.0217 | 50 | 53.0217 | 53.0217 | 0 | 53.0217 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.6673 | 46.6673 | 117.806 | 2 | PROCESSED | 57539.0191203704 | 2016-05-31 00:27:32 | 54695 | 2008-08-17 00:00:00 | 54322.5438888889 | 2007-08-10 13:03:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024438 | Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JOEL BREGMAN | Yoh Takei | USJ | 2 | AO2 | THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802082010/ | Quick Look | ![]() |
375 | ABELL 426 NE4 | 51.1184 | 42.2072 | 50.283013 | 42.030909 | 59.719337 | 22.768966 | 150.91831547 | -12.19892536 | 89.4976 | 55808.4229282407 | 2011-09-04 10:09:01 | 55808.6738425926 | 2011-09-04 16:10:20 | 806128010 | 10.3385 | 10 | 10.3385 | 10.3465 | 0 | 10.3465 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.7761 | 9.7761 | 21.6719 | 0 | PROCESSED | 57603.0579282407 | 2016-08-03 01:23:25 | 55652 | 2011-04-01 00:00:00 | 55865.1235069444 | 2011-10-31 02:57:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806128010/ | Quick Look | ![]() |
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376 | ABELL 426 NNE7 | 50.5088 | 43.4191 | 49.666767 | 43.240516 | 59.612457 | 24.057079 | 149.84713218 | -11.44434377 | 60.4957 | 55807.8394560185 | 2011-09-03 20:08:49 | 55808.0773148148 | 2011-09-04 01:51:20 | 806146010 | 11.0932 | 10 | 11.0932 | 11.0932 | 0 | 11.0932 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.9534 | 8.9534 | 20.5199 | 0 | PROCESSED | 57603.0508217593 | 2016-08-03 01:13:11 | 55652 | 2011-04-01 00:00:00 | 55845.2850578704 | 2011-10-11 06:50:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806146010/ | Quick Look | ![]() |
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377 | A2199 OFFSET4 | 247.7662 | 39.3698 | 247.336958 | 39.47607 | 234.094682 | 60.066425 | 62.70620415 | 43.21916708 | 270.0003 | 55791.1922337963 | 2011-08-18 04:36:49 | 55791.5912037037 | 2011-08-18 14:11:20 | 806150010 | 18.7116 | 20 | 18.7116 | 18.7116 | 0 | 18.7116 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.643 | 13.643 | 34.4639 | 0 | PROCESSED | 57602.8546064815 | 2016-08-02 20:30:38 | 55652 | 2011-04-01 00:00:00 | 55806.2666087963 | 2011-09-02 06:23:55 | 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/ver3.0/806150010/ | Quick Look | ![]() |
378 | A2199 OFFSET5 | 248.9722 | 38.6569 | 248.539372 | 38.75774 | 236.294551 | 59.658507 | 61.80111812 | 42.24739511 | 272.0003 | 55791.5924652778 | 2011-08-18 14:13:09 | 55792.1787152778 | 2011-08-19 04:17:21 | 806151010 | 21.084 | 20 | 21.092 | 21.092 | 0 | 21.084 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.9536 | 18.9536 | 50.6459 | 0 | PROCESSED | 57602.8747916667 | 2016-08-02 20:59:42 | 55652 | 2011-04-01 00:00:00 | 55806.2354050926 | 2011-09-02 05:38:59 | 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/ver3.0/806151010/ | Quick Look | ![]() |
379 | A1631_W | 193.0037 | -15.2462 | 192.346534 | -14.974562 | 197.903914 | -8.910337 | 303.13836962 | 47.6253175 | 112.9992 | 56305.7238541667 | 2013-01-13 17:22:21 | 56306.3738194444 | 2013-01-14 08:58:18 | 807006010 | 21.0052 | 20 | 21.0212 | 21.0052 | 0 | 21.027 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.5999 | 18.5999 | 56.1539 | 0 | PROCESSED | 57608.4939351852 | 2016-08-08 11:51:16 | 56703 | 2014-02-15 00:00:00 | 56337.5213541667 | 2013-02-14 12:30:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807006010/ | Quick Look | ![]() |
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380 | PERSEUS F_2 | 49.9481 | 41.7834 | 49.118842 | 41.602757 | 58.6868 | 22.59977 | 150.42037818 | -13.03556783 | 257.3692 | 56324.1634259259 | 2013-02-01 03:55:20 | 56324.4342939815 | 2013-02-01 10:25:23 | 807019010 | 17.2086 | 15 | 17.2156 | 17.2156 | 0 | 17.2086 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.5555 | 18.5555 | 23.3999 | 0 | PROCESSED | 57610.4952314815 | 2016-08-10 11:53:08 | 56731 | 2014-03-15 00:00:00 | 56365.4862731482 | 2013-03-14 11:40:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | 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 will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807019010/ | Quick Look | ![]() |
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381 | PERSEUS S1_2 | 49.8718 | 41.2522 | 49.04624 | 41.071281 | 58.468323 | 22.105155 | 150.6720925 | -13.51034913 | 256.4607 | 56333.5592939815 | 2013-02-10 13:25:23 | 56334.2077546296 | 2013-02-11 04:59:10 | 807020010 | 24.4245 | 25 | 24.4485 | 24.4245 | 0 | 24.4485 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23.7447 | 23.7447 | 55.9999 | 0 | PROCESSED | 57610.5627083333 | 2016-08-10 13:30:18 | 56731 | 2014-03-15 00:00:00 | 56365.492662037 | 2013-03-14 11:49:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | 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 will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807020010/ | Quick Look | ![]() |
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382 | ABELL 3395 N | 96.6064 | -54.3394 | 96.351199 | -54.307997 | 107.885857 | -77.369468 | 263.07484149 | -25.27687082 | 220.9999 | 56329.4933449074 | 2013-02-06 11:50:25 | 56330.7758564815 | 2013-02-07 18:37:14 | 807031010 | 46.9751 | 45 | 46.98 | 46.9751 | 0 | 46.9861 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.0083 | 42.0083 | 110.7998 | 2 | PROCESSED | 57610.5772337963 | 2016-08-10 13:51:13 | 56715 | 2014-02-27 00:00:00 | 56349.5329398148 | 2013-02-26 12:47:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070072 | We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO TANAKA | JAP | 7 | AO7 | INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807031010/ | Quick Look | ![]() |
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383 | ABELL 3395 S | 96.923 | -54.6479 | 96.67195 | -54.614958 | 109.024535 | -77.630718 | 263.45062321 | -25.16108018 | 230.2008 | 56339.3357060185 | 2013-02-16 08:03:25 | 56340.1778703704 | 2013-02-17 04:16:08 | 807032010 | 47.1849 | 45 | 47.1849 | 47.1849 | 0 | 47.1849 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.7509 | 49.7509 | 72.7539 | 2 | PROCESSED | 57610.6116898148 | 2016-08-10 14:40:50 | 56717 | 2014-03-01 00:00:00 | 56349.6397569444 | 2013-02-26 15:21:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070072 | We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO TANAKA | JAP | 7 | AO7 | INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807032010/ | Quick Look | ![]() |
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384 | CENA LOBE BGD2 | 197.06 | -39.3239 | 196.354066 | -39.057193 | 211.892811 | -29.411895 | 306.47248435 | 23.43231323 | 291.4078 | 56123.1069212963 | 2012-07-15 02:33:58 | 56123.5835300926 | 2012-07-15 14:00:17 | 807043010 | 21.2772 | 20 | 21.2772 | 21.2772 | 0 | 21.2772 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.4729 | 19.4729 | 41.1679 | 0 | PROCESSED | 57606.6117476852 | 2016-08-06 14:40:55 | 56018 | 2012-04-01 00:00:00 | 56142.2269675926 | 2012-08-03 05:26:50 | 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/ver3.0/807043010/ | Quick Look | ![]() |
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385 | SDSS J1302+4729 | 195.5068 | 47.4831 | 194.946247 | 47.751657 | 168.926268 | 48.423966 | 117.80880843 | 69.53967787 | 316.2365 | 56076.2710648148 | 2012-05-29 06:30:20 | 56076.7058217593 | 2012-05-29 16:56:23 | 807060010 | 20.427 | 20 | 20.427 | 20.427 | 0 | 20.427 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24.66 | 24.66 | 37.5599 | 1 | PROCESSED | 57605.5578240741 | 2016-08-05 13:23:16 | 56500 | 2013-07-27 00:00:00 | 56134.0735300926 | 2012-07-26 01:45:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807060010/ | Quick Look | ![]() |
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386 | ANTLIA E5 | 159.3469 | -35.3315 | 158.776481 | -35.071439 | 177.451568 | -40.165459 | 274.29394045 | 19.97884062 | 279.4997 | 56095.3697337963 | 2012-06-17 08:52:25 | 56096.5972916667 | 2012-06-18 14:20:06 | 807070010 | 46.7814 | 45 | 46.7894 | 46.7814 | 0 | 46.7974 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0617 | 41.0617 | 106.0579 | 2 | PROCESSED | 57605.7158333333 | 2016-08-05 17:10:48 | 56590 | 2013-10-25 00:00:00 | 56219.6892361111 | 2012-10-19 16:32:30 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807070010/ | Quick Look | ![]() |
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387 | RCS0442-2815 | 70.5602 | -28.2499 | 70.060746 | -28.343732 | 62.940418 | -49.88298 | 228.44078987 | -39.40072076 | 273.8381 | 54903.705462963 | 2009-03-13 16:55:52 | 54905.2669444444 | 2009-03-15 06:24:24 | 803060010 | 52.3573 | 40 | 52.3573 | 52.3573 | 0 | 52.3573 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.4137 | 47.4137 | 134.8779 | 1 | PROCESSED | 57545.8322222222 | 2016-06-06 19:58:24 | 55329 | 2010-05-13 00:00:00 | 54917.4174652778 | 2009-03-27 10:01:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803060010/ | Quick Look | ![]() |
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388 | A496 P-CENTER | 68.4146 | -13.2791 | 67.835234 | -13.38285 | 64.149602 | -34.804694 | 209.60984883 | -36.48888222 | 55.8718 | 54680.8514814815 | 2008-08-02 20:26:08 | 54682.0543865741 | 2008-08-04 01:18:19 | 803073010 | 44.2607 | 30 | 44.2607 | 44.2607 | 0 | 44.2607 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36.9355 | 36.9355 | 103.904 | 2 | PROCESSED | 57543.1885416667 | 2016-06-04 04:31:30 | 55059 | 2009-08-16 00:00:00 | 54693.2133796296 | 2008-08-15 05:07:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 034424 | A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | RENATO DUPKE | KYOKO MATSUSHITA | USJ | 3 | AO3 | LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803073010/ | Quick Look | ![]() |
389 | A2219 | 250.0709 | 46.72 | 249.708198 | 46.815683 | 232.227971 | 67.561681 | 72.64070926 | 41.481603 | 57.4824 | 54924.5730787037 | 2009-04-03 13:45:14 | 54927.1154282407 | 2009-04-06 02:46:13 | 804011010 | 106.6481 | 100 | 106.6481 | 106.6481 | 0 | 106.659 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114.7986 | 114.7986 | 219.6398 | 2 | PROCESSED | 57546.0936921296 | 2016-06-07 02:14:55 | 55324 | 2010-05-08 00:00:00 | 54949.5242939815 | 2009-04-28 12:34:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040011 | We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAOMI OTA | JAP | 4 | AO4 | SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804011010/ | Quick Look | ![]() |
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390 | ABELL 665 | 128.154 | 65.9045 | 127.018266 | 66.074275 | 110.985423 | 45.219486 | 149.6634974 | 34.85484411 | 289.999 | 56026.3998958333 | 2012-04-09 09:35:51 | 56027.1251967593 | 2012-04-10 03:00:17 | 807072010 | 50.431 | 50 | 50.431 | 50.431 | 0 | 50.431 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.0111 | 41.0111 | 62.6599 | 1 | PROCESSED | 57605.1298958333 | 2016-08-05 03:07:03 | 56018 | 2012-04-01 00:00:00 | 56044.1528240741 | 2012-04-27 03:40:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072010/ | Quick Look | ![]() |
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391 | ABELL 665 | 127.5519 | 65.9953 | 126.410061 | 66.162736 | 110.613991 | 45.219649 | 149.61230509 | 34.59661242 | 290.0005 | 56027.1259953704 | 2012-04-10 03:01:26 | 56027.8057638889 | 2012-04-10 19:20:18 | 807072020 | 51.446 | 50 | 51.446 | 51.446 | 0 | 51.446 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.2769 | 43.2769 | 58.728 | 1 | PROCESSED | 57605.1345717593 | 2016-08-05 03:13:47 | 56018 | 2012-04-01 00:00:00 | 56044.1899537037 | 2012-04-27 04:33:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072020/ | Quick Look | ![]() |
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392 | RCS110619-0423.6 | 166.5769 | -4.3915 | 165.941193 | -4.121064 | 169.375504 | -9.341083 | 260.07293798 | 49.52807614 | 109.9541 | 56253.8521296296 | 2012-11-22 20:27:04 | 56256.0092476852 | 2012-11-25 00:13:19 | 807075010 | 77.0765 | 75 | 77.0925 | 77.0765 | 0 | 77.1005 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69.3805 | 69.3805 | 186.3458 | 4 | PROCESSED | 57608.1296875 | 2016-08-08 03:06:45 | 56641 | 2013-12-15 00:00:00 | 56275.577025463 | 2012-12-14 13:50:55 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | 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 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807075010/ | Quick Look | ![]() |
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393 | A2029_1 | 227.7409 | 5.7498 | 227.121161 | 5.938119 | 223.529064 | 22.632778 | 6.48668362 | 50.54283023 | 112.9511 | 55224.0253819444 | 2010-01-28 00:36:33 | 55224.3328703704 | 2010-01-28 07:59:20 | 804024010 | 7.6925 | 10 | 7.6925 | 7.7079 | 0 | 7.7005 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4.6083 | 4.6083 | 26.5639 | 1 | PROCESSED | 57550.3752314815 | 2016-06-11 09:00:20 | 55612 | 2011-02-20 00:00:00 | 55245.2966203704 | 2010-02-18 07:07:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required 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 breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024010/ | Quick Look | ![]() |
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394 | HYDRA A SW | 139.253 | -12.251 | 138.651756 | -12.041032 | 145.924531 | -26.640711 | 242.88145003 | 24.78864489 | 106.4205 | 56241.8334490741 | 2012-11-10 20:00:10 | 56242.8342708333 | 2012-11-11 20:01:21 | 807090010 | 39.8399 | 40 | 39.8479 | 39.8559 | 0 | 39.8399 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 33.7085 | 33.7085 | 86.4639 | 0 | PROCESSED | 57607.9882407407 | 2016-08-07 23:43:04 | 56631 | 2013-12-05 00:00:00 | 56265.6332986111 | 2012-12-04 15:11:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807090010/ | Quick Look | ![]() |
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395 | NGC741 E | 29.459 | 5.6113 | 28.805334 | 5.368113 | 29.381945 | -6.027315 | 151.51137993 | -53.53548595 | 71.776 | 55054.8091087963 | 2009-08-11 19:25:07 | 55055.0619675926 | 2009-08-12 01:29:14 | 804053010 | 11.3778 | 10 | 11.3778 | 11.3858 | 0 | 11.3938 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.0052 | 8.0052 | 21.838 | 0 | PROCESSED | 57548.1250231482 | 2016-06-09 03:00:02 | 55430 | 2010-08-22 00:00:00 | 55064.1656134259 | 2009-08-21 03:58:29 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804053010/ | Quick Look | ![]() |
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396 | NGC2841 | 140.401 | 51.0226 | 139.538295 | 51.235726 | 125.597618 | 33.622725 | 166.8971148 | 44.0746119 | 94.9994 | 55518.5609259259 | 2010-11-18 13:27:44 | 55519.8036342593 | 2010-11-19 19:17:14 | 805028010 | 85.5269 | 80 | 85.5429 | 85.5269 | 0 | 85.5429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.375 | 59.375 | 107.3518 | 1 | PROCESSED | 57554.1596180556 | 2016-06-15 03:49:51 | 55898 | 2011-12-03 00:00:00 | 55530.1645949074 | 2010-11-30 03:57:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050028 | We propose a 80 ksec observation of an edge-on nearby spiral galaxy, NGC 2841 and the halo region. The expected temperature of the halo is ∼0.5 keV, and the characteristics enable Suzku to study the gas properties out to intergalactic space in a reliable way. We aim to obtain the temperature in the halo region within ∼5%, and hopefully an evidence for the gas dynamics not only between the disk and the halo region, but also between the halo and the intergalactic medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IKUYUKI MITSUISHI | JAP | 5 | AO5 | STUDY OF X-RAY HALO OF AN EDGE-ON GALAXY NGC 2841 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805028010/ | Quick Look | ![]() |
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397 | VIRGO N5 | 187.7004 | 14.5243 | 187.069101 | 14.800365 | 181.146119 | 16.359636 | 281.02135681 | 76.51020537 | 313.9964 | 56098.5183449074 | 2012-06-20 12:26:25 | 56098.9203125 | 2012-06-20 22:05:15 | 807110010 | 15.7789 | 13 | 15.7789 | 15.7894 | 0 | 15.7829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.0728 | 16.0728 | 34.728 | 0 | PROCESSED | 57605.7329166667 | 2016-08-05 17:35:24 | 56018 | 2012-04-01 00:00:00 | 56214.963587963 | 2012-10-14 23:07:34 | 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/ver3.0/807110010/ | Quick Look | ![]() |
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398 | NGC741MOSAICS_P1 | 29.0595 | 4.7357 | 28.408059 | 4.491575 | 28.699079 | -6.708921 | 151.53660126 | -54.49712787 | 71.6617 | 55052.4780671296 | 2009-08-09 11:28:25 | 55052.6946643518 | 2009-08-09 16:40:19 | 804054010 | 9.3222 | 10 | 9.3302 | 9.3222 | 0 | 9.3302 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.003 | 8.003 | 18.6719 | 1 | PROCESSED | 57548.0801967593 | 2016-06-09 01:55:29 | 55451 | 2010-09-12 00:00:00 | 55084.9869212963 | 2009-09-10 23:41:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054010/ | Quick Look | ![]() |
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399 | NGC 6338 | 258.8129 | 57.4208 | 258.599761 | 57.475287 | 235.015954 | 79.490546 | 85.8195722 | 35.41601483 | 46.4308 | 56771.4831712963 | 2014-04-24 11:35:46 | 56771.8058333333 | 2014-04-24 19:20:24 | 809099010 | 15.4756 | 10 | 15.4756 | 15.4756 | 0 | 15.4756 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14.5259 | 14.5259 | 26.0449 | 0 | PROCESSED | 57614.9892708333 | 2016-08-14 23:44:33 | 57155 | 2015-05-13 00:00:00 | 56789.6384722222 | 2014-05-12 15:19:24 | 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 | B | 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/ver3.0/809099010/ | Quick Look | ![]() |
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400 | VIRGO S1 | 187.7666 | 12.1106 | 187.133775 | 12.386627 | 182.229484 | 14.183198 | 284.29495534 | 74.24059367 | 308.501 | 56111.2691087963 | 2012-07-03 06:27:31 | 56111.5314583333 | 2012-07-03 12:45:18 | 807115010 | 12.5216 | 10 | 12.5336 | 12.5216 | 0 | 12.5366 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.182 | 13.182 | 22.642 | 0 | PROCESSED | 57606.5476736111 | 2016-08-06 13:08:39 | 56018 | 2012-04-01 00:00:00 | 56226.6475 | 2012-10-26 15:32:24 | 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/ver3.0/807115010/ | Quick Look | ![]() |
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401 | ABELL 426 E3 | 51.0503 | 41.5202 | 50.219736 | 41.343661 | 59.4655 | 22.121233 | 151.27232524 | -12.79481746 | 89.0003 | 55041.9666666667 | 2009-07-29 23:12:00 | 55042.2904398148 | 2009-07-30 06:58:14 | 804058010 | 11.2798 | 10 | 11.2798 | 11.5518 | 0 | 11.5518 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7201 | 10.7201 | 27.9661 | 0 | PROCESSED | 57547.981412037 | 2016-06-08 23:33:14 | 55427 | 2010-08-19 00:00:00 | 55060.7814236111 | 2009-08-17 18:45:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804058010/ | Quick Look | ![]() |
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402 | AWM4 | 241.2331 | 23.9108 | 240.70062 | 24.045882 | 232.521444 | 43.67819 | 39.92527821 | 46.49145981 | 302.6954 | 56859.2473263889 | 2014-07-21 05:56:09 | 56859.4627314815 | 2014-07-21 11:06:20 | 809102010 | 9.31 | 11 | 9.31 | 9.438 | 0 | 9.438 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4155092593 | 2016-08-15 09:58:20 | 57239 | 2015-08-05 00:00:00 | 56873.5548958333 | 2014-08-04 13:19:03 | 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 | B | 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/ver3.0/809102010/ | Quick Look | ![]() |
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403 | A133_W | 15.4513 | -21.8877 | 14.840059 | -22.156478 | 5.012562 | -26.12974 | 147.70952455 | -84.25382555 | 44.9935 | 55354.0979513889 | 2010-06-07 02:21:03 | 55355.296099537 | 2010-06-08 07:06:23 | 805019010 | 50.0449 | 50 | 50.0449 | 50.0449 | 0 | 50.0449 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.2813 | 41.2813 | 103.4758 | 0 | PROCESSED | 57551.9211689815 | 2016-06-12 22:06:29 | 55765 | 2011-07-23 00:00:00 | 55393.3189467593 | 2010-07-16 07:39:17 | 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/ver3.0/805019010/ | Quick Look | ![]() |
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404 | A2199 OFFSET3 | 246.6242 | 39.5648 | 246.194654 | 39.676177 | 232.295962 | 59.97972 | 62.9383018 | 44.10633033 | 299.9982 | 55790.598287037 | 2011-08-17 14:21:32 | 55791.1863425926 | 2011-08-18 04:28:20 | 806149010 | 21.366 | 20 | 21.374 | 21.374 | 0 | 21.366 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.2743 | 20.2743 | 50.8019 | 1 | PROCESSED | 57602.8605787037 | 2016-08-02 20:39:14 | 55652 | 2011-04-01 00:00:00 | 55806.2156365741 | 2011-09-02 05:10:31 | 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/ver3.0/806149010/ | Quick Look | ![]() |
405 | ABELL 3733 | 315.4567 | -28.0341 | 314.710836 | -28.231283 | 309.79285 | -10.656463 | 17.77333082 | -39.60697798 | 260.2652 | 56981.8706481482 | 2014-11-20 20:53:44 | 56982.1530439815 | 2014-11-21 03:40:23 | 809108010 | 14.5884 | 15 | 14.5964 | 14.6044 | 0 | 14.5884 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7988541667 | 2016-08-16 19:10:21 | 57362 | 2015-12-06 00:00:00 | 56996.4060300926 | 2014-12-05 09:44:41 | 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/ver3.0/809108010/ | Quick Look | ![]() |
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406 | VIRGO S12 | 187.4953 | 8.619 | 186.859997 | 8.895202 | 183.424434 | 10.881709 | 286.60241823 | 70.80739613 | 122.0035 | 56270.1617592593 | 2012-12-09 03:52:56 | 56270.5772106482 | 2012-12-09 13:51:11 | 807126010 | 16.4275 | 16 | 16.4275 | 16.4275 | 0 | 16.4275 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.1837 | 16.1837 | 35.8639 | 0 | PROCESSED | 57608.2146527778 | 2016-08-08 05:09:06 | 56018 | 2012-04-01 00:00:00 | 56338.4929166667 | 2013-02-15 11:49:48 | 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/ver3.0/807126010/ | Quick Look | ![]() |
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407 | RCS1620+3046 | 245.0418 | 30.7908 | 244.551505 | 30.909318 | 234.634805 | 51.209306 | 50.54291734 | 44.60353773 | 131.519 | 55203.6116666667 | 2010-01-07 14:40:48 | 55204.6008564815 | 2010-01-08 14:25:14 | 804081010 | 43.4882 | 38 | 43.4882 | 43.4882 | 0 | 43.4882 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6324 | 16.6324 | 85.4538 | 0 | PROCESSED | 57550.1212615741 | 2016-06-11 02:54:37 | 55584 | 2011-01-23 00:00:00 | 55218.2018402778 | 2010-01-22 04:50:39 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041525 | Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AMALIA HICKS | USA | 4 | AO4 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804081010/ | Quick Look | ![]() |
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408 | VIRGO S17 | 187.3614 | 6.7452 | 186.724859 | 7.021486 | 184.063087 | 9.111826 | 287.56473465 | 68.95823146 | 122.4996 | 56272.071724537 | 2012-12-11 01:43:17 | 56272.5258796296 | 2012-12-11 12:37:16 | 807131010 | 18.9432 | 18 | 18.9512 | 18.9432 | 0 | 18.9512 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.6145 | 18.6145 | 39.2319 | 1 | PROCESSED | 57608.241712963 | 2016-08-08 05:48:04 | 56018 | 2012-04-01 00:00:00 | 56291.7338773148 | 2012-12-30 17:36:47 | 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/ver3.0/807131010/ | Quick Look | ![]() |
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409 | A3404 | 101.1266 | -54.2028 | 100.864696 | -54.149703 | 118.987538 | -76.520827 | 263.61200949 | -22.68018452 | 319.1401 | 54971.6181944444 | 2009-05-20 14:50:12 | 54974.625162037 | 2009-05-23 15:00:14 | 804089010 | 122.0929 | 121 | 122.1009 | 122.1009 | 0 | 122.0929 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.1261 | 106.1261 | 259.7879 | 4 | PROCESSED | 57546.7060532407 | 2016-06-07 16:56:43 | 55358 | 2010-06-11 00:00:00 | 54992.6862615741 | 2009-06-10 16:28:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042025 | Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reduction and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | THOMAS REIPRICH | EUR | 4 | AO4 | COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTERS A3404 AND A2537 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804089010/ | Quick Look | ![]() |
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410 | NGC 253 | 11.8603 | -25.2295 | 11.246067 | -25.502313 | 0.06066 | -27.714636 | 97.43086004 | -87.9001973 | 242.9983 | 55544.0947685185 | 2010-12-14 02:16:28 | 55546.9460763889 | 2010-12-16 22:42:21 | 805018010 | 101.0026 | 100 | 101.0026 | 101.0026 | 0 | 101.0026 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82.6689 | 82.6689 | 246.3359 | 1 | PROCESSED | 57554.5316203704 | 2016-06-15 12:45:32 | 55975 | 2012-02-18 00:00:00 | 55607.3286111111 | 2011-02-15 07:53:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050015 | Suzaku observations of a hot halo of nearby, edge-on starburst galaxy, NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by a previous offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and dynamics of the galaxy outflow to the intergalactic space. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORIKO YAMASAKI | JAP | 5 | AO5 | SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805018010/ | Quick Look | ![]() |
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411 | A3667_SE | 303.4605 | -57.0338 | 302.458448 | -57.1853 | 291.78529 | -36.098363 | 340.61636005 | -33.57067764 | 74.2668 | 55298.167349537 | 2010-04-12 04:00:59 | 55299.2716435185 | 2010-04-13 06:31:10 | 805036010 | 66.2872 | 50 | 66.2952 | 66.2872 | 0 | 66.2872 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.249 | 51.249 | 95.3978 | 1 | PROCESSED | 57551.2001967593 | 2016-06-12 04:48:17 | 55675 | 2011-04-24 00:00:00 | 55309.2055324074 | 2010-04-23 04:55:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050039 | We propose an additional offset pointing of Abell 3667, one of the nearest, typical merging cluster. Using the 3 observations pointed along the merger axis on AO-1, we detected a possible super hot component around the cluster center (Nakazawa et al. 2009). To identify the existence and location of this component, we propose to observe the South-East Relic region, about 17 f south to the original southern-most pointing. This observation aims at verifying and locating the super hot component in this cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | JAP | 5 | AO5 | TRACING THE POSSIBLE SUPER-HOT COMPONENT IN THE MERGING CLUSTER ABELL 3667 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805036010/ | Quick Look | ![]() |
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412 | ABELL1835 OFFSET1 | 210.441 | 2.9038 | 209.807683 | 3.144591 | 207.277058 | 14.34402 | 340.72312739 | 60.50812136 | 306.2398 | 55382.6847453704 | 2010-07-05 16:26:02 | 55384.1217361111 | 2010-07-07 02:55:18 | 805037010 | 49.4391 | 50 | 49.4471 | 49.4391 | 0 | 49.4471 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.0599 | 43.0599 | 124.1398 | 1 | PROCESSED | 57552.5235532407 | 2016-06-13 12:33:55 | 55807 | 2011-09-03 00:00:00 | 55441.2415856482 | 2010-09-02 05:47:53 | 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/ver3.0/805037010/ | Quick Look | ![]() |
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413 | ABELL 85 S1 | 10.6021 | -9.9841 | 9.970303 | -10.258056 | 5.733976 | -13.366048 | 115.42621428 | -72.72412936 | 230 | 56292.2572800926 | 2012-12-31 06:10:29 | 56295.6314583333 | 2013-01-03 15:09:18 | 807135010 | 139.9982 | 50 | 139.9982 | 139.9982 | 0 | 139.9982 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.82 | 11.82 | 25.4779 | 0 | PROCESSED | 57608.4068402778 | 2016-08-08 09:45:51 | 56703 | 2014-02-15 00:00:00 | 56337.496875 | 2013-02-14 11:55:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071791 | We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | STEVEN ALLEN | USA | 7 | AO7 | TRACING A MERGER FROM START TO FINISH IN ABELL 85 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807135010/ | Quick Look | ![]() |
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414 | NGC3402 BACKGROUND | 161.6656 | -13.5535 | 161.046219 | -13.289693 | 168.522728 | -19.671776 | 262.34680831 | 39.29035073 | 110.091 | 55549.4379282407 | 2010-12-19 10:30:37 | 55549.7563425926 | 2010-12-19 18:09:08 | 805071010 | 12.5184 | 10 | 12.5344 | 12.5184 | 0 | 12.5344 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.8582 | 11.8582 | 27.4799 | 0 | PROCESSED | 57554.4605439815 | 2016-06-15 11:03:11 | 55960 | 2012-02-03 00:00:00 | 55593.0714699074 | 2011-02-01 01:42:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805071010/ | Quick Look | ![]() |
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415 | ESO3060170 | 85.0359 | -40.9515 | 84.636079 | -40.976582 | 81.358883 | -64.245092 | 246.54247084 | -30.30516606 | 320.0075 | 55327.721400463 | 2010-05-11 17:18:49 | 55328.2676388889 | 2010-05-12 06:25:24 | 805075010 | 31.3959 | 30 | 31.4039 | 31.3959 | 0 | 31.4119 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.684 | 28.684 | 47.1899 | 2 | PROCESSED | 57551.4609953704 | 2016-06-12 11:03:50 | 55707 | 2011-05-26 00:00:00 | 55341.5181365741 | 2010-05-25 12:26:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051513 | We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 5 | AO5 | HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805075010/ | Quick Look | ![]() |
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416 | CYGNUS A SUB | 299.7227 | 40.8585 | 299.290982 | 40.72139 | 317.590165 | 59.487138 | 76.23979532 | 5.91406977 | 241.0006 | 56615.3145717593 | 2013-11-19 07:32:59 | 56616.3224189815 | 2013-11-20 07:44:17 | 808016010 | 42.5204 | 40 | 42.5284 | 42.5284 | 0 | 42.5204 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.9173 | 38.9173 | 87.0719 | 1 | PROCESSED | 57613.3640625 | 2016-08-13 08:44:15 | 56995 | 2014-12-04 00:00:00 | 56629.6679050926 | 2013-12-03 16:01:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080018 | We have observed a merging cluster Cygnus A in the Suzaku GO-3 with 45ks. This observation confirmed a hot region between the main and sub components. Furthermore, we found a gas velocity shift between the main and sub by about 2500 km/s. We believe that these are colliding with each other. The current result are limited by statistics and systematic uncertainty. To improve the accurary of the measurement and complete our study, we propose two additional observations located the main and sub components at the center of the FOV. These will provide the best chance to look into a merging cluster "in motion". | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 8 | AO8 | CYGNUS A CLUSTER: THE BEST MERGING SYSTEM FOR THE SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808016010/ | Quick Look | ![]() |
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417 | PKS 0745-191 | 116.4685 | -19.4632 | 115.915912 | -19.340315 | 123.218132 | -39.89918 | 236.39245911 | 2.60836561 | 294.0003 | 55317.3681365741 | 2010-05-01 08:50:07 | 55318.1516087963 | 2010-05-02 03:38:19 | 805086010 | 31.7299 | 35 | 31.7299 | 31.7299 | 0 | 31.7299 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.646 | 27.646 | 67.682 | 0 | PROCESSED | 57551.3418981482 | 2016-06-12 08:12:20 | 55696 | 2011-05-15 00:00:00 | 55330.121087963 | 2010-05-14 02:54:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805086010/ | Quick Look | ![]() |
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418 | RCS2318-0024 | 349.6301 | -0.4169 | 348.988896 | -0.690483 | 350.299766 | 3.723056 | 79.21894267 | -55.19865221 | 248.0438 | 55526.0185648148 | 2010-11-26 00:26:44 | 55527.293912037 | 2010-11-27 07:03:14 | 805089010 | 50.305 | 73 | 50.329 | 50.305 | 0 | 50.337 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.6346 | 45.6346 | 110.1738 | 0 | PROCESSED | 57554.2552893518 | 2016-06-15 06:07:37 | 55903 | 2011-12-08 00:00:00 | 55537.0791898148 | 2010-12-07 01:54:02 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051527 | Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 5 | AO5 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805089010/ | Quick Look | ![]() |
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419 | NGC1550_BGD | 66.1553 | 2.4144 | 65.504252 | 2.300401 | 64.719628 | -18.959095 | 191.78857248 | -30.8138174 | 260.0006 | 56697.3550694444 | 2014-02-09 08:31:18 | 56698.0418634259 | 2014-02-10 01:00:17 | 808061010 | 31.1456 | 30 | 31.1536 | 31.1536 | 0 | 31.1456 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8043171296 | 2016-08-13 19:18:13 | 57102 | 2015-03-21 00:00:00 | 56736.7213425926 | 2014-03-20 17:18:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080110 | We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TORU SASAKI | JAP | 8 | AO8 | STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808061010/ | Quick Look | ![]() |
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420 | A133_FIELD_3 | 15.3292 | -22.0955 | 14.718033 | -22.364433 | 4.799478 | -26.269218 | 147.50079252 | -84.48957915 | 231.9998 | 56631.4102314815 | 2013-12-05 09:50:44 | 56632.6168981482 | 2013-12-06 14:48:20 | 808083010 | 51.8568 | 50 | 51.8568 | 51.8568 | 0 | 51.8568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.9569 | 47.9569 | 104.2418 | 0 | PROCESSED | 57613.5483217593 | 2016-08-13 13:09:35 | 57009 | 2014-12-18 00:00:00 | 56643.7003587963 | 2013-12-17 16:48:31 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808083010/ | Quick Look | ![]() |
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421 | A133_FIELD_4 | 16.0019 | -22.0663 | 15.391978 | -22.334366 | 5.44253 | -26.509377 | 153.04375578 | -84.18809016 | 231.9997 | 56632.6176967593 | 2013-12-06 14:49:29 | 56633.8716666667 | 2013-12-07 20:55:12 | 808084010 | 52.5282 | 50 | 52.5282 | 52.5282 | 0 | 52.5282 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.912 | 49.912 | 108.3281 | 0 | PROCESSED | 57613.5467013889 | 2016-08-13 13:07:15 | 57061 | 2015-02-08 00:00:00 | 56695.6415046296 | 2014-02-07 15:23:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808084010/ | Quick Look | ![]() |
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422 | ABELL 1068 | 160.2123 | 39.7867 | 159.491465 | 40.048011 | 145.700686 | 28.920989 | 179.4205229 | 60.1860041 | 130.0008 | 55863.1263310185 | 2011-10-29 03:01:55 | 55864.5459837963 | 2011-10-30 13:06:13 | 806028030 | 53.3186 | 50 | 53.3186 | 53.335 | 0 | 53.3266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.0713 | 49.0713 | 122.6438 | 0 | PROCESSED | 57603.6522800926 | 2016-08-03 15:39:17 | 55652 | 2011-04-01 00:00:00 | 55874.122662037 | 2011-11-09 02:56:38 | 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/ver3.0/806028030/ | Quick Look | ![]() |
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423 | A426VIR N | 48.9538 | 42.7811 | 48.120761 | 42.596803 | 58.224249 | 23.764199 | 149.23070312 | -12.5987294 | 270.5957 | 56710.5023726852 | 2014-02-22 12:03:25 | 56711.155775463 | 2014-02-23 03:44:19 | 808087010 | 23.3776 | 25 | 23.3856 | 23.3856 | 0 | 23.3776 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.5612 | 20.5612 | 56.4419 | 0 | PROCESSED | 57613.8896296296 | 2016-08-13 21:21:04 | 57089 | 2015-03-08 00:00:00 | 56723.6141898148 | 2014-03-07 14:44:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808087010/ | Quick Look | ![]() |
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424 | A426VIR W | 48.7321 | 42.6495 | 47.900602 | 42.4644 | 58.012629 | 23.684677 | 149.16205221 | -12.79713949 | 270.0001 | 56711.1564351852 | 2014-02-23 03:45:16 | 56711.6279976852 | 2014-02-23 15:04:19 | 808088010 | 24.7428 | 25 | 24.7587 | 24.7428 | 0 | 24.7667 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.0168 | 22.0168 | 40.7359 | 0 | PROCESSED | 57613.8909259259 | 2016-08-13 21:22:56 | 57141 | 2015-04-29 00:00:00 | 56764.7613657407 | 2014-04-17 18:16:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808088010/ | Quick Look | ![]() |
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425 | ABELL 1689 (OFFSET) | 198.1886 | -1.1923 | 197.54634 | -0.927328 | 197.227317 | 6.029723 | 314.05162405 | 61.21838483 | 111.865 | 56657.0769444444 | 2013-12-31 01:50:48 | 56660.6460069445 | 2014-01-03 15:30:15 | 808089030 | 53.2272 | 130 | 53.2272 | 53.2272 | 0 | 53.2272 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 3.3279 | 0 | PROCESSED | 57613.7319791667 | 2016-08-13 17:34:03 | 56383 | 2013-04-01 00:00:00 | 56713.6636342593 | 2014-02-25 15:55:38 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089030/ | Quick Look | ![]() |
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426 | ABELL 1689 (OFFSET) | 198.1809 | -1.2604 | 197.538539 | -0.995417 | 197.246177 | 5.963813 | 314.01167358 | 61.15261163 | 111.9001 | 56670.9898148148 | 2014-01-13 23:45:20 | 56672.9376388889 | 2014-01-15 22:30:12 | 808089040 | 37.4667 | 90 | 37.4667 | 37.4667 | 0 | 37.4667 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7681134259 | 2016-08-13 18:26:05 | 56383 | 2013-04-01 00:00:00 | 56687.7783564815 | 2014-01-30 18:40:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KA-WAH WONG | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808089040/ | Quick Look | ![]() |
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427 | COMA W SHOCK2 | 194.0639 | 28.3374 | 193.459144 | 28.607762 | 180.49458 | 31.367738 | 81.80911298 | 88.38803012 | 275.4001 | 56475.6616782407 | 2013-07-02 15:52:49 | 56476.1674884259 | 2013-07-03 04:01:11 | 808091010 | 15.6934 | 15 | 15.7094 | 15.6934 | 0 | 15.7094 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.6254 | 16.6254 | 43.694 | 0 | PROCESSED | 57611.6755902778 | 2016-08-11 16:12:51 | 56858 | 2014-07-20 00:00:00 | 56492.6168865741 | 2013-07-19 14:48:19 | 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/ver3.0/808091010/ | Quick Look | ![]() |
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428 | A2877-SOUTH | 17.378 | -46.6527 | 16.824483 | -46.918871 | 351.212416 | -48.486015 | 293.76700694 | -70.15260223 | 237.9995 | 56647.8346643518 | 2013-12-21 20:01:55 | 56649.916875 | 2013-12-23 22:00:18 | 808103010 | 83.5172 | 80 | 83.5172 | 83.5252 | 0 | 83.5332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81.2993 | 81.2993 | 179.8979 | 4 | PROCESSED | 57613.6802199074 | 2016-08-13 16:19:31 | 57033 | 2015-01-11 00:00:00 | 56665.8173263889 | 2014-01-08 19:36:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082014 | We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BHARADWAJ VIJAYSARATHY | EUR | 8 | AO8 | INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808103010/ | Quick Look | ![]() |
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429 | COMA NW6 | 194.1545 | 29.4183 | 193.551623 | 29.688554 | 179.999631 | 32.366617 | 96.76135884 | 87.44172405 | 319.9992 | 55734.4158796296 | 2011-06-22 09:58:52 | 55734.7419328704 | 2011-06-22 17:48:23 | 806044010 | 13.52 | 15 | 13.52 | 13.52 | 0 | 13.52 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.5945 | 11.5945 | 28.1679 | 1 | PROCESSED | 57602.3747453704 | 2016-08-02 08:59:38 | 55652 | 2011-04-01 00:00:00 | 55768.2886574074 | 2011-07-26 06:55:40 | 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/ver3.0/806044010/ | Quick Look | ![]() |
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430 | A3528-S OFFSET 1 | 193.8801 | -29.4768 | 193.202783 | -29.206094 | 204.617979 | -21.613954 | 303.99602967 | 33.38651365 | 289.4829 | 56500.4359953704 | 2013-07-27 10:27:50 | 56501.528587963 | 2013-07-28 12:41:10 | 808104010 | 40.3411 | 50 | 40.3491 | 40.3491 | 0 | 40.3411 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.8623 | 40.8623 | 94.384 | 2 | PROCESSED | 57612.0687037037 | 2016-08-12 01:38:56 | 56955 | 2014-10-25 00:00:00 | 56587.7834490741 | 2013-10-22 18:48:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808104010/ | Quick Look | ![]() |
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431 | BEYOND VIRGO 3 | 187.7131 | 16.6287 | 187.083239 | 16.904753 | 180.24751 | 18.281087 | 277.46526397 | 78.4695575 | 119.4716 | 55906.3990277778 | 2011-12-11 09:34:36 | 55907.0070717593 | 2011-12-12 00:10:11 | 806062010 | 24.1336 | 30 | 24.1336 | 24.1336 | 0 | 24.1336 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22.399 | 22.399 | 52.5119 | 1 | PROCESSED | 57604.102974537 | 2016-08-04 02:28:17 | 56289 | 2012-12-28 00:00:00 | 55920.9612731482 | 2011-12-25 23:04:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806062010/ | Quick Look | ![]() |
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432 | BEYOND VIRGO 5 | 187.715 | 17.1647 | 187.085509 | 17.440751 | 180.014258 | 18.769278 | 276.35604201 | 78.95966269 | 118.1329 | 55918.8504976852 | 2011-12-23 20:24:43 | 55919.8960300926 | 2011-12-24 21:30:17 | 806064010 | 41.7692 | 40 | 41.7772 | 41.7692 | 0 | 41.7772 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.3124 | 34.3124 | 90.2919 | 1 | PROCESSED | 57604.2418402778 | 2016-08-04 05:48:15 | 56340 | 2013-02-17 00:00:00 | 55972.6886458333 | 2012-02-15 16:31:39 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806064010/ | Quick Look | ![]() |
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433 | VIRGO E1 | 188.0634 | 12.5322 | 187.431175 | 12.808036 | 182.325865 | 14.686251 | 284.88156742 | 74.72763223 | 285 | 56481.2981828704 | 2013-07-08 07:09:23 | 56481.5626736111 | 2013-07-08 13:30:15 | 808116010 | 10.3353 | 10 | 10.3353 | 10.3353 | 0 | 10.3353 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8.8323 | 8.8323 | 22.8459 | 0 | PROCESSED | 57611.7060416667 | 2016-08-11 16:56:42 | 56383 | 2013-04-01 00:00:00 | 56524.6432407407 | 2013-08-20 15:26:16 | 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/ver3.0/808116010/ | Quick Look | ![]() |
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434 | VIRGO E5 | 189.1714 | 13.1819 | 188.540883 | 13.456957 | 183.073594 | 15.719707 | 288.31179147 | 75.63323247 | 284.9999 | 56482.4931365741 | 2013-07-09 11:50:07 | 56482.9348726852 | 2013-07-09 22:26:13 | 808120010 | 12.2986 | 12 | 12.2986 | 12.2986 | 0 | 12.2986 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.2671 | 12.2671 | 38.1619 | 0 | PROCESSED | 57611.7660300926 | 2016-08-11 18:23:05 | 56383 | 2013-04-01 00:00:00 | 56496.6035416667 | 2013-07-23 14:29:06 | 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/ver3.0/808120010/ | Quick Look | ![]() |
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435 | THE MOON | 137.2637 | 11.2624 | 136.584895 | 11.465744 | 136.302979 | -4.908841 | 218.49853071 | 35.60818154 | 285.3989 | 56784.0743402778 | 2014-05-07 01:47:03 | 56784.198125 | 2014-05-07 04:45:18 | 809001050 | 5.7625 | 45 | 5.7705 | 5.7625 | 0 | 5.7785 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.371 | 4.371 | 10.6879 | 1 | PROCESSED | 57615.062337963 | 2016-08-15 01:29:46 | 57218 | 2015-07-15 00:00:00 | 56852.5744328704 | 2014-07-14 13:47:11 | 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/ver3.0/809001050/ | Quick Look | ![]() |
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436 | BEYOND VIRGO 7 | 187.7158 | 17.6999 | 187.086679 | 17.97595 | 179.778986 | 19.25601 | 275.1422843 | 79.44418151 | 118.4175 | 55920.9292708333 | 2011-12-25 22:18:09 | 55922.3029166667 | 2011-12-27 07:16:12 | 806066010 | 51.5018 | 50 | 51.5258 | 51.5178 | 0 | 51.5018 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.0209 | 45.0209 | 118.6698 | 0 | PROCESSED | 57604.2629861111 | 2016-08-04 06:18:42 | 56340 | 2013-02-17 00:00:00 | 55972.6991203704 | 2012-02-15 16:46:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORBERT WERNER | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806066010/ | Quick Look | ![]() |
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437 | THE MOON | 24.3624 | 9.7895 | 23.702448 | 9.535235 | 26.139692 | -0.327211 | 141.30582848 | -51.43331262 | 73.7995 | 56857.0209259259 | 2014-07-19 00:30:08 | 56857.1515856482 | 2014-07-19 03:38:17 | 809001140 | 4.2907 | 45 | 4.2907 | 4.2907 | 0 | 4.2907 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4055439815 | 2016-08-15 09:43:59 | 57267 | 2015-09-02 00:00:00 | 56902.7022685185 | 2014-09-02 16:51:16 | 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/ver3.0/809001140/ | Quick Look | ![]() |
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438 | THE MOON | 139.925 | 10.5889 | 139.25032 | 10.800859 | 139.007269 | -4.769046 | 220.6720528 | 37.66748388 | 105.6998 | 56975.3249305556 | 2014-11-14 07:47:54 | 56975.4487615741 | 2014-11-14 10:46:13 | 809001210 | 3.5246 | 45 | 3.5246 | 3.5246 | 0 | 3.5246 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.771412037 | 2016-08-16 18:30:50 | 57358 | 2015-12-02 00:00:00 | 56992.4131018518 | 2014-12-01 09:54:52 | 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/ver3.0/809001210/ | Quick Look | ![]() |
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439 | THE MOON | 144.4436 | 10.011 | 143.773859 | 10.236526 | 143.42105 | -3.916716 | 223.94276709 | 41.37428155 | 105.6999 | 56975.7165856482 | 2014-11-14 17:11:53 | 56975.8473611111 | 2014-11-14 20:20:12 | 809001240 | 6.2192 | 45 | 6.2192 | 6.2272 | 0 | 6.2512 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7771412037 | 2016-08-16 18:39:05 | 57358 | 2015-12-02 00:00:00 | 56992.4178703704 | 2014-12-01 10:01:44 | 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/ver3.0/809001240/ | Quick Look | ![]() |
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440 | RCS211853-6334.5 | 319.7157 | -63.5732 | 318.707212 | -63.784045 | 298.683481 | -45.002818 | 330.73727963 | -40.23433007 | 78.3879 | 55689.9756018518 | 2011-05-08 23:24:52 | 55691.0148148148 | 2011-05-10 00:21:20 | 806079010 | 69.5446 | 70 | 69.5526 | 69.5446 | 0 | 69.5526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.3836 | 57.3836 | 89.7739 | 0 | PROCESSED | 57601.9954398148 | 2016-08-01 23:53:26 | 56068 | 2012-05-21 00:00:00 | 55701.1727314815 | 2011-05-20 04:08:44 | 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/ver3.0/806079010/ | Quick Look | ![]() |
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441 | THE MOON | 330.3821 | -8.1914 | 329.721062 | -8.43265 | 329.560437 | 3.662364 | 50.06648816 | -45.61675095 | 252.3 | 56989.8522685185 | 2014-11-28 20:27:16 | 56989.9654976852 | 2014-11-28 23:10:19 | 809001280 | 4.7272 | 45 | 4.7272 | 4.7272 | 0 | 4.7272 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.401712963 | 2016-08-17 09:38:28 | 57415 | 2016-01-28 00:00:00 | 57002.4419444445 | 2014-12-11 10:36:24 | 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/ver3.0/809001280/ | Quick Look | ![]() |
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442 | THE MOON | 332.0733 | -7.3936 | 331.41518 | -7.63885 | 331.413251 | 3.82441 | 52.31004503 | -46.62982693 | 251.0013 | 56989.9669444444 | 2014-11-28 23:12:24 | 56990.1008449074 | 2014-11-29 02:25:13 | 809001290 | 4.227 | 45 | 4.227 | 4.2506 | 0 | 4.235 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4062962963 | 2016-08-17 09:45:04 | 57415 | 2016-01-28 00:00:00 | 57002.4422453704 | 2014-12-11 10:36:50 | 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/ver3.0/809001290/ | Quick Look | ![]() |
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443 | CEN_A_LOBE_N2 | 201.2142 | -42.0778 | 200.484454 | -41.817568 | 216.546241 | -30.52743 | 309.53774085 | 20.36490033 | 292.2294 | 56861.2578587963 | 2014-07-23 06:11:19 | 56862.6946990741 | 2014-07-24 16:40:22 | 809003010 | 52.1427 | 50 | 52.1507 | 52.1427 | 0 | 52.1587 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.3107 | 19.3107 | 40.0719 | 0 | PROCESSED | 57615.4510648148 | 2016-08-15 10:49:32 | 57242 | 2015-08-08 00:00:00 | 56875.1594560185 | 2014-08-06 03:49:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809003010/ | Quick Look | ![]() |
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444 | A3526 | 191.2847 | -39.8559 | 190.600127 | -39.582502 | 207.545871 | -31.88181 | 301.61867579 | 22.99978629 | 109.9984 | 55943.9465393518 | 2012-01-17 22:43:01 | 55944.2683333333 | 2012-01-18 06:26:24 | 806089010 | 15.9106 | 15 | 15.9186 | 15.9106 | 0 | 15.9186 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.985 | 12.985 | 27.7919 | 0 | PROCESSED | 57604.3987268518 | 2016-08-04 09:34:10 | 56332 | 2013-02-09 00:00:00 | 55964.1580439815 | 2012-02-07 03:47:35 | 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/ver3.0/806089010/ | Quick Look | ![]() |
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445 | ABELL 426 SW3 | 49.102 | 40.9982 | 48.280214 | 40.814462 | 57.790981 | 22.022932 | 150.31514223 | -14.0400409 | 94.9993 | 55801.0601967593 | 2011-08-28 01:26:41 | 55801.3084722222 | 2011-08-28 07:24:12 | 806102010 | 11.955 | 10 | 11.955 | 11.955 | 0 | 11.955 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.864 | 7.864 | 21.4239 | 1 | PROCESSED | 57602.9856134259 | 2016-08-02 23:39:17 | 55652 | 2011-04-01 00:00:00 | 55818.1485185185 | 2011-09-14 03:33:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806102010/ | Quick Look | ![]() |
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446 | N23_DEML71 | 76.4544 | -67.9572 | 76.483575 | -68.02238 | 338.831134 | -84.597327 | 278.75688601 | -34.83345845 | 297.0986 | 56021.0207986111 | 2012-04-04 00:29:57 | 56023.6043402778 | 2012-04-06 14:30:15 | 807008010 | 101.9614 | 100 | 101.9614 | 101.9614 | 0 | 101.9614 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.0031 | 99.0031 | 223.204 | 1 | PROCESSED | 57605.1620023148 | 2016-08-05 03:53:17 | 56401 | 2013-04-19 00:00:00 | 56034.2910069444 | 2012-04-17 06:59:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070036 | Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYUKI UCHIDA | JAP | 7 | AO7 | FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807008010/ | Quick Look | ![]() |
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447 | ABELL 426 SW6 | 48.2625 | 40.4485 | 47.446504 | 40.261728 | 56.965884 | 21.67573 | 150.06660907 | -14.84565948 | 88.4982 | 55802.8164814815 | 2011-08-29 19:35:44 | 55803.0348958333 | 2011-08-30 00:50:15 | 806108010 | 11.5336 | 10 | 11.5656 | 11.5576 | 0 | 11.5336 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.7551 | 10.7551 | 18.8561 | 0 | PROCESSED | 57603.0017476852 | 2016-08-03 00:02:31 | 55652 | 2011-04-01 00:00:00 | 55826.1269444444 | 2011-09-22 03:02:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806108010/ | Quick Look | ![]() |
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448 | CEN_A_LOBE_N4 | 200.0149 | -42.0781 | 199.290063 | -41.815855 | 215.61315 | -30.91319 | 308.59567712 | 20.47867303 | 294.4884 | 56864.2718634259 | 2014-07-26 06:31:29 | 56865.6863194444 | 2014-07-27 16:28:18 | 809005010 | 49.4215 | 50 | 49.4215 | 50.3093 | 0 | 50.3093 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.7711 | 14.7711 | 31.0519 | 0 | PROCESSED | 57615.4593055556 | 2016-08-15 11:01:24 | 57242 | 2015-08-08 00:00:00 | 56875.2119675926 | 2014-08-06 05:05:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809005010/ | Quick Look | ![]() |
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449 | A3112W | 49.1257 | -44.1666 | 48.689569 | -44.349648 | 25.156648 | -58.765875 | 252.9579492 | -56.34974536 | 40.0005 | 56834.0356481482 | 2014-06-26 00:51:20 | 56835.5486458333 | 2014-06-27 13:10:03 | 809025010 | 48.949 | 45 | 48.949 | 48.949 | 0 | 48.949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.966 | 11.966 | 40.6069 | 2 | PROCESSED | 57615.3397685185 | 2016-08-15 08:09:16 | 57249 | 2015-08-15 00:00:00 | 56881.2363078704 | 2014-08-12 05:40:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809025010/ | Quick Look | ![]() |
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450 | FJ0846+5326 | 131.5564 | 53.4343 | 130.632054 | 53.617254 | 118.481008 | 34.023671 | 164.73615985 | 38.37651034 | 277.0006 | 56764.8665393518 | 2014-04-17 20:47:49 | 56766.1148032407 | 2014-04-19 02:45:19 | 809037010 | 44.7166 | 45 | 44.7166 | 44.7166 | 0 | 44.7166 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9585416667 | 2016-08-14 23:00:18 | 57145 | 2015-05-03 00:00:00 | 56782.5079976852 | 2014-05-05 12:11:31 | 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/ver3.0/809037010/ | Quick Look | ![]() |
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451 | OFF-FIELD1 | 154.5616 | 22.312 | 153.870987 | 22.562652 | 148.318203 | 10.965902 | 212.25034337 | 55.01303699 | 298.5999 | 56782.6031712963 | 2014-05-05 14:28:34 | 56783.5417939815 | 2014-05-06 13:00:11 | 809052010 | 41.103 | 40 | 41.103 | 41.103 | 0 | 41.103 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.0283 | 39.0283 | 81.0719 | 1 | PROCESSED | 57615.0526388889 | 2016-08-15 01:15:48 | 57162 | 2015-05-20 00:00:00 | 56793.5659490741 | 2014-05-16 13:34:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANJALI GUPTA | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809052010/ | Quick Look | ![]() |
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452 | ABELL 98-SOUTH | 11.6766 | 20.275 | 11.015845 | 20.00206 | 18.757977 | 14.029978 | 121.42486866 | -42.58290308 | 251.4904 | 57011.5401736111 | 2014-12-20 12:57:51 | 57012.9168171296 | 2014-12-21 22:00:13 | 809080010 | 48.2579 | 100 | 48.2579 | 49.0544 | 0 | 49.1104 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5485532407 | 2016-08-17 13:09:55 | 56748 | 2014-04-01 00:00:00 | 57107.4443171296 | 2015-03-26 10:39:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809080010/ | Quick Look | ![]() |
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453 | ABELL 3411 OFFSET | 130.7649 | -17.3143 | 130.18997 | -17.133567 | 138.838529 | -34.101685 | 241.9812862 | 15.18552207 | 105.3327 | 56967.309849537 | 2014-11-06 07:26:11 | 56968.1939467593 | 2014-11-07 04:39:17 | 809083010 | 38.952 | 39 | 38.952 | 39.272 | 0 | 39.288 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7398263889 | 2016-08-16 17:45:21 | 57358 | 2015-12-02 00:00:00 | 56982.4550231482 | 2014-11-21 10:55:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091528 | Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | REINOUT VAN WEEREN | USA | 9 | AO9 | ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809083010/ | Quick Look | ![]() |
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454 | ABELL 426 NE6 | 51.7255 | 42.539 | 50.886134 | 42.364994 | 60.28512 | 22.967764 | 151.10360581 | -11.67130403 | 89.4994 | 55810.8220717593 | 2011-09-06 19:43:47 | 55811.0314583333 | 2011-09-07 00:45:18 | 806132010 | 11.4246 | 10 | 11.4406 | 11.4246 | 0 | 11.4486 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.0645 | 10.0645 | 18.0879 | 0 | PROCESSED | 57603.0828703704 | 2016-08-03 01:59:20 | 55652 | 2011-04-01 00:00:00 | 55866.2046759259 | 2011-11-01 04:54:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806132010/ | Quick Look | ![]() |
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455 | ABELL 426 NNE6 | 50.4234 | 43.1429 | 49.58355 | 42.964001 | 59.463368 | 23.808902 | 149.95061465 | -11.70868128 | 60.4955 | 55807.3026967593 | 2011-09-03 07:15:53 | 55807.5834375 | 2011-09-03 14:00:09 | 806144010 | 10.4306 | 10 | 10.4306 | 10.4306 | 0 | 10.4306 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.723 | 10.723 | 24.2539 | 0 | PROCESSED | 57603.0471990741 | 2016-08-03 01:07:58 | 55652 | 2011-04-01 00:00:00 | 55845.2864467593 | 2011-10-11 06:52:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806144010/ | Quick Look | ![]() |
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456 | SWCL1330+4206 | 202.7007 | 42.1031 | 202.156429 | 42.360378 | 179.6615 | 46.801465 | 97.22165079 | 73.00355707 | 325.866 | 57166.2929166667 | 2015-05-24 07:01:48 | 57167.0793171296 | 2015-05-25 01:54:13 | 809088020 | 34.7796 | 34 | 34.7796 | 34.7876 | 0 | 34.7796 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21.0686 | 21.0686 | 53.048 | 1 | PROCESSED | 57618.72625 | 2016-08-18 17:25:48 | 57548 | 2016-06-09 00:00:00 | 57178.157025463 | 2015-06-05 03:46:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809088020/ | Quick Look | ![]() |
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457 | CENA LOBE 1 | 201.4716 | -38.9356 | 200.750271 | -38.675827 | 215.22462 | -27.598918 | 310.226071 | 23.44775478 | 285.9999 | 56117.7018287037 | 2012-07-09 16:50:38 | 56119.8959953704 | 2012-07-11 21:30:14 | 807040010 | 84.161 | 80 | 84.161 | 84.161 | 0 | 84.161 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72.2838 | 72.2838 | 188.7955 | 3 | PROCESSED | 57606.6375347222 | 2016-08-06 15:18:03 | 56018 | 2012-04-01 00:00:00 | 56159.3425925926 | 2012-08-20 08:13:20 | 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/ver3.0/807040010/ | Quick Look | ![]() |
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458 | CENA LOBE 2 | 201.7887 | -39.7611 | 201.063779 | -39.501882 | 215.867616 | -28.245975 | 310.35734609 | 22.59512331 | 290.5003 | 56122.1648958333 | 2012-07-14 03:57:27 | 56122.4584490741 | 2012-07-14 11:00:10 | 807041020 | 12.9463 | 80 | 12.9463 | 12.9463 | 0 | 12.9463 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.6518 | 12.6518 | 25.3519 | 0 | PROCESSED | 57606.6009027778 | 2016-08-06 14:25:18 | 56018 | 2012-04-01 00:00:00 | 56142.1626736111 | 2012-08-03 03:54:15 | 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/ver3.0/807041020/ | Quick Look | ![]() |
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459 | FG09 | 160.7604 | 0.8965 | 160.118108 | 1.158829 | 161.901438 | -6.701816 | 247.95154277 | 49.5505044 | 288.8833 | 56077.2212731482 | 2012-05-30 05:18:38 | 56077.5397337963 | 2012-05-30 12:57:13 | 807050010 | 12.49 | 10 | 12.4944 | 12.49 | 0 | 12.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.8506 | 10.8506 | 27.5119 | 0 | PROCESSED | 57605.5584722222 | 2016-08-05 13:24:12 | 56462 | 2013-06-19 00:00:00 | 56096.107662037 | 2012-06-18 02:35:02 | 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/ver3.0/807050010/ | Quick Look | ![]() |
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460 | ABELL2345EAST | 321.8675 | -12.1557 | 321.189104 | -12.37369 | 320.327375 | 2.690486 | 39.92441578 | -40.06382879 | 77.2002 | 56777.6418402778 | 2014-04-30 15:24:15 | 56780.1466550926 | 2014-05-03 03:31:11 | 809119010 | 101.3009 | 100 | 101.3169 | 101.3009 | 0 | 101.3169 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.0885 | 88.0885 | 216.38 | 1 | PROCESSED | 57615.0703935185 | 2016-08-15 01:41:22 | 56748 | 2014-04-01 00:00:00 | 56790.7271759259 | 2014-05-13 17:27:08 | 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/ver3.0/809119010/ | Quick Look | ![]() |
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461 | FG03 | 118.182 | 45.9572 | 117.286088 | 46.086737 | 111.16384 | 24.564923 | 173.26592635 | 29.42392711 | 92.9981 | 56228.7772453704 | 2012-10-28 18:39:14 | 56229.1078819444 | 2012-10-29 02:35:21 | 807052010 | 14.3185 | 10 | 14.3265 | 14.3185 | 0 | 14.3345 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.365 | 15.365 | 28.544 | 0 | PROCESSED | 57607.868125 | 2016-08-07 20:50:06 | 56696 | 2014-02-08 00:00:00 | 56330.5013541667 | 2013-02-07 12:01:57 | 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/ver3.0/807052010/ | Quick Look | ![]() |
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462 | ANTLIA NW4 | 156.477 | -34.4731 | 155.913183 | -34.218342 | 174.203454 | -40.552676 | 271.69853818 | 19.42589093 | 299.2985 | 57168.4177546296 | 2015-05-26 10:01:34 | 57169.4605902778 | 2015-05-27 11:03:15 | 810066010 | 6.3596 | 40 | 6.3596 | 6.8635 | 0 | 6.8635 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 6.7341 | 6.7341 | 78.0621 | 0 | PROCESSED | 57618.7963657407 | 2016-08-18 19:06:46 | 57626 | 2016-08-26 00:00:00 | 57178.2408101852 | 2015-06-05 05:46:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101522 | We have measured hot gas properties of the nearest non-cool core cluster, Antlia, in the eastern direction out to R200. Our initial results suggest that its density profile is more consistent with some massive clusters, but significantly steeper than its cool core counterpart with a similar temperature (mass), Virgo. We propose to extend our program to observe two other directions to test azimuthal variation, which is likely to be significant. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KA-WAH WONG | USA | 10 | AO10 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/810066010/ | Quick Look | ![]() |
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463 | A2256N | 256.1941 | 78.9961 | 256.949832 | 79.060716 | 101.697267 | 76.992175 | 111.38046428 | 31.59001765 | 219.8042 | 56234.8690625 | 2012-11-03 20:51:27 | 56236.1877083333 | 2012-11-05 04:30:18 | 807024010 | 62.2855 | 60 | 62.2855 | 62.2855 | 0 | 62.2855 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 76.5361 | 76.5361 | 113.9039 | 0 | PROCESSED | 57607.9455555556 | 2016-08-07 22:41:36 | 56630 | 2013-12-04 00:00:00 | 56260.5238657407 | 2012-11-29 12:34:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070058 | We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 7 | AO7 | THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807024010/ | Quick Look | ![]() |
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464 | FG26 | 237.2323 | 8.8441 | 236.628181 | 8.995997 | 232.656986 | 28.135005 | 17.92603672 | 44.32356312 | 282.0742 | 56137.0874305556 | 2012-07-29 02:05:54 | 56137.3307986111 | 2012-07-29 07:56:21 | 807054010 | 11.8912 | 10 | 11.8912 | 11.8912 | 0 | 11.8912 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.5983 | 8.5983 | 20.9999 | 0 | PROCESSED | 57606.6870023148 | 2016-08-06 16:29:17 | 56626 | 2013-11-30 00:00:00 | 56260.480474537 | 2012-11-29 11:31:53 | 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/ver3.0/807054010/ | Quick Look | ![]() |
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465 | ANTLIA E2 | 158.2496 | -35.3292 | 157.682674 | -35.071089 | 176.423673 | -40.599314 | 273.48585529 | 19.50669913 | 277.9997 | 56092.2642361111 | 2012-06-14 06:20:30 | 56093.0181944444 | 2012-06-15 00:26:12 | 807067010 | 24.1741 | 23 | 24.1821 | 24.1741 | 0 | 24.1901 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.8534 | 22.8534 | 65.1359 | 3 | PROCESSED | 57605.6727546296 | 2016-08-05 16:08:46 | 56476 | 2013-07-03 00:00:00 | 56110.5259027778 | 2012-07-02 12:37:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807067010/ | Quick Look | ![]() |
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466 | ABELL 2597 | 351.2512 | -12.298 | 350.600815 | -12.572949 | 347.099073 | -7.834502 | 64.91051751 | -64.90126459 | 250.0013 | 56264.7750115741 | 2012-12-03 18:36:01 | 56266.2606134259 | 2012-12-05 06:15:17 | 807073040 | 54.7187 | 50 | 54.7187 | 54.7427 | 0 | 54.7267 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.919 | 47.919 | 128.3278 | 1 | PROCESSED | 57608.2146759259 | 2016-08-08 05:09:08 | 56018 | 2012-04-01 00:00:00 | 56279.7033912037 | 2012-12-18 16:52:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073040/ | Quick Look | ![]() |
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467 | COMA NW7 | 194.0035 | 29.6909 | 193.400635 | 29.961328 | 179.713479 | 32.548963 | 101.76403044 | 87.24693436 | 319.9995 | 55735.2525925926 | 2011-06-23 06:03:44 | 55735.5383680556 | 2011-06-23 12:55:15 | 806046010 | 16.1218 | 15 | 16.1514 | 16.1458 | 0 | 16.1218 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14.8517 | 14.8517 | 24.6879 | 0 | PROCESSED | 57602.3868518518 | 2016-08-02 09:17:04 | 55652 | 2011-04-01 00:00:00 | 55768.6489930556 | 2011-07-26 15:34:33 | 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/ver3.0/806046010/ | Quick Look | ![]() |
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468 | AWM7 27' SOUTH | 43.6454 | 41.2726 | 42.837995 | 41.069836 | 53.624746 | 23.507895 | 146.50839268 | -15.89370788 | 257.401 | 55975.6646296296 | 2012-02-18 15:57:04 | 55976.5071180556 | 2012-02-19 12:10:15 | 806009010 | 34.9735 | 30 | 34.9815 | 34.9735 | 0 | 34.9735 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.6452 | 33.6452 | 72.7819 | 1 | PROCESSED | 57604.6468055556 | 2016-08-04 15:31:24 | 56361 | 2013-03-10 00:00:00 | 55994.9781828704 | 2012-03-08 23:28:35 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806009010/ | Quick Look | ![]() |
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469 | J2218.6-0346 | 334.6629 | -3.7693 | 334.013965 | -4.02026 | 335.129241 | 6.290164 | 58.79146355 | -46.71055995 | 71.7798 | 56063.8991550926 | 2012-05-16 21:34:47 | 56064.7196875 | 2012-05-17 17:16:21 | 807085010 | 28.629 | 25 | 28.629 | 28.629 | 0 | 28.629 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.8327 | 26.8327 | 70.8839 | 1 | PROCESSED | 57605.4341550926 | 2016-08-05 10:25:11 | 56442 | 2013-05-30 00:00:00 | 56076.0273726852 | 2012-05-29 00:39:25 | 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/ver3.0/807085010/ | Quick Look | ![]() |
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470 | MS 1512.4+3647 | 228.6059 | 36.6198 | 228.120322 | 36.804723 | 210.693369 | 51.882401 | 59.43888584 | 58.40149096 | 128.9265 | 54463.6508449074 | 2007-12-29 15:37:13 | 54469.6946527778 | 2008-01-04 16:40:18 | 802034010 | 268.8898 | 200 | 268.9458 | 268.8898 | 0 | 268.9458 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.4803 | 47.4803 | 102.8019 | 2 | PROCESSED | 57541.0217476852 | 2016-06-02 00:31:19 | 54909 | 2009-03-19 00:00:00 | 54542.2596296296 | 2008-03-17 06:13:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020086 | Evolution of the amount of metals depends on history of super novae activities and metal tranport from inter-stellar space into the ICM. We observe a distant cluster, MS 1512+3647 (z=0.372), and determine the abundance ratio of alpha particles which are created by type II supernovae to iron by type Ia. This reveals the evolution of branch ratio of metals in a galaxy between stars and the ICM which has been unresolved observationally. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 2 | AO2 | EVOLUTION STUDY ON AMOUNT OF METALS IN THE ICM USING A DISTANT CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802034010/ | Quick Look | ![]() |
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471 | A2061 | 230.3095 | 30.6453 | 229.795666 | 30.824015 | 216.361499 | 46.967712 | 48.13899774 | 57.1713197 | 293.2901 | 53943.6955092593 | 2006-07-27 16:41:32 | 53943.9946643518 | 2006-07-27 23:52:19 | 801081010 | 13.8887 | 14 | 13.9047 | 13.9047 | 13.8887 | 13.8967 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 11.8443 | 11.8443 | 25.8399 | 0 | PROCESSED | 57535.0552083333 | 2016-05-27 01:19:30 | 54401 | 2007-10-28 00:00:00 | 53955.6442939815 | 2006-08-08 15:27:47 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801081010/ | Quick Look | ![]() |
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472 | VIRGO W4 | 186.6838 | 11.7876 | 186.04966 | 12.064261 | 181.367978 | 13.457626 | 281.0321598 | 73.60000956 | 100.001 | 56273.6409143518 | 2012-12-12 15:22:55 | 56273.9264699074 | 2012-12-12 22:14:07 | 807097010 | 14.512 | 11 | 14.512 | 14.536 | 0 | 14.52 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.7379 | 13.7379 | 24.6659 | 0 | PROCESSED | 57608.2576388889 | 2016-08-08 06:11:00 | 56018 | 2012-04-01 00:00:00 | 56342.5158680556 | 2013-02-19 12:22:51 | 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/ver3.0/807097010/ | Quick Look | ![]() |
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473 | A2249 | 257.46 | 34.4851 | 257.00595 | 34.546595 | 250.753931 | 57.089244 | 57.64541352 | 34.94797305 | 129.9858 | 54114.5939467593 | 2007-01-14 14:15:17 | 54115.1252777778 | 2007-01-15 03:00:24 | 801082010 | 22.8156 | 15 | 22.8156 | 22.8236 | 0 | 22.8236 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.7637 | 19.7637 | 45.9039 | 1 | PROCESSED | 57536.8308333333 | 2016-05-28 19:56:24 | 54695 | 2008-08-17 00:00:00 | 54133.0295833333 | 2007-02-02 00:42:36 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801082010/ | Quick Look | ![]() |
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474 | THE MOON | 344.0153 | -3.4 | 343.369759 | -3.667219 | 343.958901 | 3.149835 | 68.62224539 | -53.63365394 | 247.8502 | 56990.8695717593 | 2014-11-29 20:52:11 | 56991.0002546296 | 2014-11-30 00:00:22 | 809001360 | 4.8998 | 45 | 4.8998 | 4.8998 | 0 | 4.8998 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4137615741 | 2016-08-17 09:55:49 | 57415 | 2016-01-28 00:00:00 | 57007.4035648148 | 2014-12-16 09:41:08 | 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/ver3.0/809001360/ | Quick Look | ![]() |
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475 | VIRGO W9 | 185.2783 | 10.9356 | 184.642354 | 11.212937 | 180.431009 | 12.119991 | 277.70610968 | 72.30561596 | 99.9989 | 56275.8085763889 | 2012-12-14 19:24:21 | 56276.4093055556 | 2012-12-15 09:49:24 | 807102010 | 27.1057 | 23 | 27.1057 | 27.1057 | 0 | 27.1057 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.4791 | 28.4791 | 51.896 | 0 | PROCESSED | 57608.2880092593 | 2016-08-08 06:54:44 | 56018 | 2012-04-01 00:00:00 | 56315.5260300926 | 2013-01-23 12:37:29 | 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/ver3.0/807102010/ | Quick Look | ![]() |
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476 | CIZA J2242 OFFSET | 339.3149 | 52.6806 | 338.804058 | 52.420641 | 11.931322 | 54.574747 | 103.28112871 | -4.99517915 | 17.9944 | 55772.8222337963 | 2011-07-30 19:44:01 | 55774.1446180556 | 2011-08-01 03:28:15 | 806002010 | 55.9134 | 60 | 55.9356 | 55.9134 | 0 | 55.9134 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73.1891 | 73.1891 | 114.2 | 2 | PROCESSED | 57602.7241666667 | 2016-08-02 17:22:48 | 56162 | 2012-08-23 00:00:00 | 55792.2422222222 | 2011-08-19 05:48:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060014 | Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAJIME KAWAHARA | SHO NISHINO | JAP | 6 | AO6 | SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806002010/ | Quick Look | ![]() |
477 | FILAMENT JUNCTION 2 | 149.2538 | 26.1497 | 148.542222 | 26.388047 | 142.296251 | 12.813389 | 204.13118538 | 51.20952403 | 290.4949 | 55699.3618402778 | 2011-05-18 08:41:03 | 55701.114849537 | 2011-05-20 02:45:23 | 806004010 | 70.1591 | 70 | 70.1591 | 70.1671 | 0 | 70.1671 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63.3295 | 63.3295 | 151.4357 | 1 | PROCESSED | 57602.1051851852 | 2016-08-02 02:31:28 | 56092 | 2012-06-14 00:00:00 | 55722.7303356482 | 2011-06-10 17:31:41 | 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/ver3.0/806004010/ | Quick Look | ![]() |
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478 | VIRGO N4 | 187.7041 | 14.2061 | 187.072593 | 14.482163 | 181.285557 | 16.070988 | 281.49354158 | 76.21209693 | 310.9981 | 56104.178900463 | 2012-06-26 04:17:37 | 56104.463275463 | 2012-06-26 11:07:07 | 807109010 | 12.7577 | 12 | 12.7577 | 12.7577 | 0 | 12.7577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.291 | 13.291 | 24.5619 | 0 | PROCESSED | 57606.4838541667 | 2016-08-06 11:36:45 | 56018 | 2012-04-01 00:00:00 | 56219.6559953704 | 2012-10-19 15:44:38 | 3.0.22.44 | 3 | 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/ver3.0/807109010/ | Quick Look | ![]() |
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479 | VIRGO S4 | 187.668 | 11.1668 | 187.034459 | 11.442891 | 182.532865 | 13.281501 | 284.92853674 | 73.30851588 | 308.5011 | 56112.2229861111 | 2012-07-04 05:21:06 | 56112.5056828704 | 2012-07-04 12:08:11 | 807118010 | 12.852 | 10 | 12.852 | 12.852 | 0 | 12.852 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.8622 | 13.8622 | 24.4179 | 0 | PROCESSED | 57606.5554282407 | 2016-08-06 13:19:49 | 56018 | 2012-04-01 00:00:00 | 56141.1138194445 | 2012-08-02 02:43:54 | 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/ver3.0/807118010/ | Quick Look | ![]() |
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480 | VIRGO S13 | 187.4758 | 8.312 | 186.840292 | 8.588214 | 183.531882 | 10.592818 | 286.77930619 | 70.50542211 | 122.0007 | 56270.5777314815 | 2012-12-09 13:51:56 | 56270.8459606482 | 2012-12-09 20:18:11 | 807127010 | 13.0666 | 12 | 13.0984 | 13.0906 | 0 | 13.0666 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.5411 | 11.5411 | 23.1679 | 0 | PROCESSED | 57608.2217824074 | 2016-08-08 05:19:22 | 56018 | 2012-04-01 00:00:00 | 56291.6901273148 | 2012-12-30 16:33:47 | 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/ver3.0/807127010/ | Quick Look | ![]() |
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481 | ABELL 426 S5 | 49.6049 | 40.1572 | 48.78706 | 39.975311 | 57.933438 | 21.108752 | 151.11933243 | -14.5358666 | 87.9995 | 55426.4039930556 | 2010-08-18 09:41:45 | 55426.6474537037 | 2010-08-18 15:32:20 | 805100010 | 10.6209 | 10 | 10.6289 | 10.6209 | 0 | 10.6289 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.3257 | 10.3257 | 21.0319 | 0 | PROCESSED | 57553.1198148148 | 2016-06-14 02:52:32 | 55287 | 2010-04-01 00:00:00 | 55439.1414699074 | 2010-08-31 03:23:43 | 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/ver3.0/805100010/ | Quick Look | ![]() |
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482 | VIRGO S19 | 187.324 | 6.1182 | 186.687061 | 6.394509 | 184.281915 | 8.522189 | 287.8702994 | 68.34005974 | 122.7988 | 56272.9313310185 | 2012-12-11 22:21:07 | 56273.403587963 | 2012-12-12 09:41:10 | 807133010 | 19.3484 | 19 | 19.3601 | 19.3564 | 0 | 19.3484 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.7099 | 20.7099 | 40.798 | 0 | PROCESSED | 57608.2512384259 | 2016-08-08 06:01:47 | 56018 | 2012-04-01 00:00:00 | 56338.5094907407 | 2013-02-15 12:13:40 | 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/ver3.0/807133010/ | Quick Look | ![]() |
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483 | NGC 720 OFFSET | 28.2673 | -13.4983 | 27.658292 | -13.744232 | 21.049561 | -23.414412 | 172.55217141 | -70.17529179 | 242.404 | 55560.2543634259 | 2010-12-30 06:06:17 | 55565.2502083333 | 2011-01-04 06:00:18 | 805069010 | 223.9663 | 150 | 223.9722 | 223.9663 | 0 | 223.9722 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.3571 | 13.3571 | 28.3639 | 0 | PROCESSED | 57600.5655671296 | 2016-07-31 13:34:25 | 55994 | 2012-03-08 00:00:00 | 55627.1378009259 | 2011-03-07 03:18:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051503 | Models of galaxy formation suggest that as many as half the baryons may reside in an extended, hot halo. Detecting such a halo around a disk galaxy is, however, extremely challenging for current instrumentation. We propose instead to measure the baryon content of an isolated, X-ray bright elliptical galaxy (Mvir~6E12Msun), which provides the best opportunity to take a census of the baryons in a normal, galaxy-scale system. Currently little is known about the total baryon content of such objects, which are the likely end points of spiral galaxy merging. Combined with archival data, our offset pointing will enable the gas to be traced to ~0.75R500, comparable to what has been achieved for galaxy groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | PHILIP HUMPHREY | USA | 5 | AO5 | THE BARYON FRACTION OF AN ISOLATED ELLIPTICAL GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805069010/ | Quick Look | ![]() |
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484 | ABELL 426 S5.5 | 49.5719 | 40.0219 | 48.754994 | 39.839891 | 57.867374 | 20.985689 | 151.17444164 | -14.66274998 | 88.0005 | 55426.6477430556 | 2010-08-18 15:32:45 | 55426.8585648148 | 2010-08-18 20:36:20 | 805111010 | 11.1329 | 10 | 11.1569 | 11.1409 | 0 | 11.1329 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.1518 | 7.1518 | 18.2079 | 0 | PROCESSED | 57553.1273032407 | 2016-06-14 03:03:19 | 55287 | 2010-04-01 00:00:00 | 55439.1544212963 | 2010-08-31 03:42:22 | 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/ver3.0/805111010/ | Quick Look | ![]() |
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485 | AWM7 SE1 | 44.3556 | 41.1876 | 43.546511 | 40.987213 | 54.148816 | 23.260587 | 147.03812428 | -15.71286613 | 256.9997 | 56706.6681828704 | 2014-02-18 16:02:11 | 56707.1284953704 | 2014-02-19 03:05:02 | 808025010 | 16.8194 | 15 | 16.8194 | 16.8434 | 0 | 16.8274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.321 | 15.321 | 39.7619 | 0 | PROCESSED | 57613.8533912037 | 2016-08-13 20:28:53 | 57085 | 2015-03-04 00:00:00 | 56719.747662037 | 2014-03-03 17:56:38 | 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/ver3.0/808025010/ | Quick Look | ![]() |
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486 | MKW4 | 181.137 | 1.9141 | 180.496491 | 2.192466 | 180.278577 | 2.208157 | 276.9409609 | 62.39583381 | 136.3986 | 56655.392662037 | 2013-12-29 09:25:26 | 56656.271099537 | 2013-12-30 06:30:23 | 808066010 | 34.57 | 30 | 34.57 | 34.57 | 0 | 34.57 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.1435 | 30.1435 | 75.8879 | 0 | PROCESSED | 57613.7104861111 | 2016-08-13 17:03:06 | 57033 | 2015-01-11 00:00:00 | 56667.6362268518 | 2014-01-10 15:16:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808066010/ | Quick Look | ![]() |
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487 | A3528-S OFFSET 3 | 194.0873 | -29.8404 | 193.408879 | -29.569931 | 204.956936 | -21.869821 | 304.20210274 | 33.01923597 | 288.9994 | 56502.3985300926 | 2013-07-29 09:33:53 | 56503.6522453704 | 2013-07-30 15:39:14 | 808106010 | 61.2339 | 60 | 61.2579 | 61.2499 | 0 | 61.2339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.6474 | 61.6474 | 108.3097 | 2 | PROCESSED | 57612.1235763889 | 2016-08-12 02:57:57 | 56955 | 2014-10-25 00:00:00 | 56587.4691782407 | 2013-10-22 11:15:37 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808106010/ | Quick Look | ![]() |
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488 | AWM7 BGD | 41.6937 | 42.4876 | 40.885444 | 42.278459 | 52.542503 | 25.125109 | 144.58796377 | -15.48250354 | 257.001 | 56707.9150810185 | 2014-02-19 21:57:43 | 56708.3828587963 | 2014-02-20 09:11:19 | 808027010 | 20.4971 | 20 | 20.5011 | 20.5051 | 0 | 20.4971 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.116 | 22.116 | 40.41 | 0 | PROCESSED | 57613.8622106482 | 2016-08-13 20:41:35 | 57086 | 2015-03-05 00:00:00 | 56720.6154976852 | 2014-03-04 14:46:19 | 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/ver3.0/808027010/ | Quick Look | ![]() |
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489 | VIRGO E8 | 190.0457 | 13.6937 | 189.416619 | 13.968069 | 183.664073 | 16.534019 | 291.30515449 | 76.31072684 | 284.9998 | 56483.6999768518 | 2013-07-10 16:47:58 | 56484.1918634259 | 2013-07-11 04:36:17 | 808123010 | 18.4482 | 18 | 18.4482 | 18.4482 | 0 | 18.4482 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.2122 | 16.2122 | 42.492 | 0 | PROCESSED | 57611.7962268518 | 2016-08-11 19:06:34 | 56383 | 2013-04-01 00:00:00 | 56498.6264351852 | 2013-07-25 15:02:04 | 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/ver3.0/808123010/ | Quick Look | ![]() |
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490 | NGC 5044 | 198.8504 | -16.3899 | 198.183934 | -16.125889 | 203.593771 | -7.791309 | 311.2339251 | 46.09520433 | 290.0016 | 53918.7631712963 | 2006-07-02 18:18:58 | 53919.3600115741 | 2006-07-03 08:38:25 | 801046010 | 19.7466 | 20 | 19.7466 | 19.7466 | 19.7466 | 19.7466 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17.9716 | 17.9716 | 51.562 | 1 | PROCESSED | 57534.8255208333 | 2016-05-26 19:48:45 | 54394 | 2007-10-21 00:00:00 | 53930.6133217593 | 2006-07-14 14:43:11 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801046010/ | Quick Look | ![]() |
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491 | THE MOON | 17.8678 | 7.6685 | 17.216041 | 7.403045 | 19.391263 | 0.083978 | 131.57870726 | -54.86656285 | 73.8004 | 56856.4839814815 | 2014-07-18 11:36:56 | 56856.6565162037 | 2014-07-18 15:45:23 | 809001100 | 8.2482 | 45 | 8.2642 | 8.2482 | 0 | 8.2642 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3962962963 | 2016-08-15 09:30:40 | 57233 | 2015-07-30 00:00:00 | 56867.7358912037 | 2014-07-29 17:39:41 | 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/ver3.0/809001100/ | Quick Look | ![]() |
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492 | THE MOON | 27.6562 | 10.6142 | 26.991894 | 10.366866 | 29.46244 | -0.715898 | 145.72862444 | -49.61972993 | 73.8014 | 56857.2778935185 | 2014-07-19 06:40:10 | 56857.4015856482 | 2014-07-19 09:38:17 | 809001160 | 6.3331 | 45 | 6.3411 | 6.3411 | 0 | 6.3331 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4093287037 | 2016-08-15 09:49:26 | 57267 | 2015-09-02 00:00:00 | 56902.690775463 | 2014-09-02 16:34:43 | 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/ver3.0/809001160/ | Quick Look | ![]() |
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493 | CEN_A_LOBE_N1 | 201.8136 | -42.0782 | 201.081414 | -41.819016 | 217.012441 | -30.336854 | 310.00727378 | 20.30096505 | 292.0832 | 56859.7082060185 | 2014-07-21 16:59:49 | 56861.2571990741 | 2014-07-23 06:10:22 | 809002010 | 50.3801 | 50 | 50.3881 | 50.3881 | 0 | 50.3801 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.4775 | 11.4775 | 24.4719 | 0 | PROCESSED | 57615.4533333333 | 2016-08-15 10:52:48 | 57242 | 2015-08-08 00:00:00 | 56875.1360185185 | 2014-08-06 03:15:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809002010/ | Quick Look | ![]() |
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494 | A3112BG | 50.3312 | -44.7001 | 49.902687 | -44.878678 | 26.087437 | -59.659599 | 253.38993788 | -55.36648392 | 25.002 | 56828.7830208333 | 2014-06-20 18:47:33 | 56829.3648611111 | 2014-06-21 08:45:24 | 809028010 | 13.041 | 30 | 13.041 | 13.041 | 0 | 24.268 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.199 | 20.199 | 50.2559 | 0 | PROCESSED | 57615.2871064815 | 2016-08-15 06:53:26 | 57394 | 2016-01-07 00:00:00 | 56873.1992824074 | 2014-08-04 04:46:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809028010/ | Quick Look | ![]() |
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495 | FJ0854+4908_OFFSET | 133.7467 | 48.8373 | 132.873661 | 49.028229 | 121.743576 | 30.102388 | 170.52256786 | 40.09070343 | 275.4911 | 56776.9674074074 | 2014-04-29 23:13:04 | 56777.6286805556 | 2014-04-30 15:05:18 | 809039010 | 31.9155 | 30 | 31.9155 | 31.9155 | 0 | 31.9155 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.928 | 28.928 | 57.1259 | 0 | PROCESSED | 57615.0205555556 | 2016-08-15 00:29:36 | 57218 | 2015-07-15 00:00:00 | 56852.6002546296 | 2014-07-14 14:24:22 | 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/ver3.0/809039010/ | Quick Look | ![]() |
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496 | FJ1336+3553 | 203.9051 | 36.0067 | 203.345869 | 36.26171 | 185.165039 | 42.045012 | 79.05269341 | 77.07938329 | 299.9994 | 56835.5627546296 | 2014-06-27 13:30:22 | 56836.6564814815 | 2014-06-28 15:45:20 | 809040010 | 49.8464 | 50 | 49.8464 | 49.8464 | 0 | 49.8464 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3306828704 | 2016-08-15 07:56:11 | 57212 | 2015-07-09 00:00:00 | 56846.5971180556 | 2014-07-08 14:19:51 | 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/ver3.0/809040010/ | Quick Look | ![]() |
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497 | NGC3221 | 155.5344 | 21.5594 | 154.847338 | 21.812076 | 149.453825 | 10.59718 | 213.96748211 | 55.66659318 | 113.4999 | 56977.5304513889 | 2014-11-16 12:43:51 | 56980.5453125 | 2014-11-19 13:05:15 | 809051010 | 121.2459 | 120 | 121.2459 | 121.2459 | 0 | 121.2459 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8106018518 | 2016-08-16 19:27:16 | 57362 | 2015-12-06 00:00:00 | 56995.6190162037 | 2014-12-04 14:51:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANJALI GUPTA | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809051010/ | Quick Look | ![]() |
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498 | OFF-FIELD2 | 156.3941 | 20.5095 | 155.710931 | 20.763905 | 150.605485 | 9.917753 | 216.1857144 | 56.11255364 | 112.0717 | 56982.1681018518 | 2014-11-21 04:02:04 | 56983.2640046296 | 2014-11-22 06:20:10 | 809053010 | 39.8287 | 40 | 39.8287 | 39.8287 | 0 | 39.8287 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8087847222 | 2016-08-16 19:24:39 | 57377 | 2015-12-21 00:00:00 | 57009.4169444444 | 2014-12-18 10:00:24 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANJALI GUPTA | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809053010/ | Quick Look | ![]() |
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499 | MKW4-WN | 181.4571 | 2.3391 | 180.816687 | 2.617439 | 180.402943 | 2.725316 | 277.2234025 | 62.91169747 | 110.2998 | 56994.5218865741 | 2014-12-03 12:31:31 | 56996.9723842593 | 2014-12-05 23:20:14 | 809062010 | 90.3652 | 100 | 90.3652 | 91.5172 | 0 | 91.5172 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.7385 | 88.7385 | 211.7057 | 1 | PROCESSED | 57617.4717361111 | 2016-08-17 11:19:18 | 56748 | 2014-04-01 00:00:00 | 57007.0908912037 | 2014-12-16 02:10:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091513 | We propose to observe the nearby group MKW4 by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Four additional pointings, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variation. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 9 | AO9 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809062010/ | Quick Look | ![]() |
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500 | FORNAX OFFSET1 | 54.5865 | -35.7706 | 54.109381 | -35.93292 | 38.512958 | -53.072025 | 237.25707491 | -53.65522298 | 45.0001 | 54662.3087962963 | 2008-07-15 07:24:40 | 54663.2106365741 | 2008-07-16 05:03:19 | 803006010 | 35.2402 | 30 | 35.2482 | 35.2402 | 0 | 35.2513 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.441 | 30.441 | 77.9179 | 0 | PROCESSED | 57543.0490393518 | 2016-06-04 01:10:37 | 55055 | 2009-08-12 00:00:00 | 54686.1787384259 | 2008-08-08 04:17:23 | 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/ver3.0/803006010/ | Quick Look | ![]() |
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501 | PERSEUS OFFSET-E | 49.943 | 41.2145 | 49.117489 | 41.033844 | 58.512606 | 22.054116 | 150.73941272 | -13.51227041 | 269.9995 | 55615.1921180556 | 2011-02-23 04:36:39 | 55615.8335416667 | 2011-02-23 20:00:18 | 805045010 | 27.4595 | 25 | 27.4755 | 27.4595 | 0 | 27.4755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.5296 | 25.5296 | 55.3919 | 0 | PROCESSED | 57601.0240856482 | 2016-08-01 00:34:41 | 55996 | 2012-03-10 00:00:00 | 55628.1301157407 | 2011-03-08 03:07:22 | 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/ver3.0/805045010/ | Quick Look | ![]() |
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502 | FORNAX A W-LOBE S | 50.358 | -37.3109 | 49.88075 | -37.489463 | 32.300433 | -53.110983 | 240.40250552 | -56.92779805 | 62.5011 | 55012.4989930556 | 2009-06-30 11:58:33 | 55013.9619675926 | 2009-07-01 23:05:14 | 804038010 | 52.4253 | 50 | 52.4333 | 52.4333 | 0 | 52.4253 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.7121 | 11.7121 | 36.36 | 1 | PROCESSED | 57547.7267013889 | 2016-06-08 17:26:27 | 55393 | 2010-07-16 00:00:00 | 55026.4458564815 | 2009-07-14 10:42:02 | 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/ver3.0/804038010/ | Quick Look | ![]() |
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503 | HCG62 | 193.274 | -9.2022 | 192.623373 | -8.930867 | 195.778851 | -3.241931 | 303.62256693 | 53.66732525 | 113.6407 | 53755.3883333333 | 2006-01-20 09:19:12 | 53758.5002199074 | 2006-01-23 12:00:19 | 800013020 | 114.8488 | 100 | 114.8568 | 114.8488 | 114.8488 | 114.8568 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98.7836 | 98.7836 | 268.8498 | 4 | PROCESSED | 57532.7777199074 | 2016-05-24 18:39:55 | 54247 | 2007-05-27 00:00:00 | 54040.4546064815 | 2006-11-01 10:54:38 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001057 | We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAOMI OTA | JAP | 0 | SWG | MEASURING HARD TAILS AND METAL DISTRIBUTIONS IN THE GALAXY GROUP HCG62 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800013020/ | Quick Look | ![]() |
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504 | RXCJ0605 | 91.2587 | -35.3175 | 90.815345 | -35.312478 | 91.987157 | -58.750453 | 241.74700639 | -24.18215725 | 309.9853 | 55322.2226041667 | 2010-05-06 05:20:33 | 55323.0307060185 | 2010-05-07 00:44:13 | 805065020 | 40.0231 | 40 | 40.0231 | 40.0231 | 0 | 40.0231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.1762 | 33.1762 | 69.7899 | 0 | PROCESSED | 57551.4119097222 | 2016-06-12 09:53:09 | 55287 | 2010-04-01 00:00:00 | 55341.5093981482 | 2010-05-25 12:13:32 | 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/ver3.0/805065020/ | Quick Look | ![]() |
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505 | ABELL 2199 CENTER | 247.1922 | 39.484 | 246.76294 | 39.592842 | 233.179095 | 60.039777 | 62.84241749 | 43.66620611 | 252.3681 | 54009.2972222222 | 2006-10-01 07:08:00 | 54009.8967361111 | 2006-10-01 21:31:18 | 801056010 | 24.9282 | 25 | 25.4799 | 24.9282 | 25.4799 | 25.4799 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.519 | 20.519 | 51.7939 | 1 | PROCESSED | 57535.7247453704 | 2016-05-27 17:23:38 | 54735 | 2008-09-26 00:00:00 | 54021.2246990741 | 2006-10-13 05:23:34 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801056010/ | Quick Look | ![]() |
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506 | A3667_NW_17OFF | 302.8177 | -56.56 | 301.819585 | -56.708877 | 291.523842 | -35.547493 | 341.18808838 | -33.22347241 | 74.1682 | 53861.293912037 | 2006-05-06 07:03:14 | 53861.7356944444 | 2006-05-06 17:39:24 | 801095010 | 17.2586 | 20 | 17.2826 | 17.2746 | 17.2666 | 17.2586 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14.2555 | 14.2555 | 38.1519 | 1 | PROCESSED | 57533.636099537 | 2016-05-25 15:15:59 | 54735 | 2008-09-26 00:00:00 | 53913.7593518518 | 2006-06-27 18:13:28 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095010/ | Quick Look | ![]() |
507 | A2142 OFFSET1 | 239.3897 | 27.3899 | 238.873146 | 27.532705 | 228.881511 | 46.554196 | 44.41448178 | 48.88746657 | 283.7323 | 54316.0523726852 | 2007-08-04 01:15:25 | 54317.0211226852 | 2007-08-05 00:30:25 | 802030010 | 37.6227 | 30 | 37.6307 | 37.6227 | 0 | 37.6307 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.6677 | 29.6677 | 83.6879 | 1 | PROCESSED | 57539.4231134259 | 2016-05-31 10:09:17 | 54723 | 2008-09-14 00:00:00 | 54347.3816087963 | 2007-09-04 09:09:31 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020076 | We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802030010/ | Quick Look | ![]() |
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508 | ANTLIA CLUSTER | 157.5092 | -35.3277 | 156.944615 | -35.070958 | 175.726148 | -40.891834 | 272.94647188 | 19.18131972 | 90.0004 | 54423.2458796296 | 2007-11-19 05:54:04 | 54425.0211111111 | 2007-11-21 00:30:24 | 802035010 | 65.9528 | 60 | 65.9608 | 65.9608 | 0 | 65.9528 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58.1064 | 58.1064 | 153.3638 | 2 | PROCESSED | 57540.5835185185 | 2016-06-01 14:00:16 | 54801 | 2008-12-01 00:00:00 | 54433.3905092593 | 2007-11-29 09:22:20 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020101 | Suzaku observation of the non-cD cluster Abell 1060 shows that temperature of intra-cluster medium (ICM) increases toward the center. This phenomenon is exact opposite of that of giant cD clusters, in which temperature of the ICM decreases toward the center. To explain this observation, we have proposed that galaxies moving through the ICM interact magnetohydrodynamically with the ICM. This scenario implies that the galaxies have lost some part of their kinetic energies, while the ICM received the released energies. As a result, the ICM have been efficiently heated near the center in which galaxy number density is high. To strengthen our scenario, we propose to observation and study temperature map of the Antlia cluster which is another non-cD, relaxed, and nearby (z=0.0087) cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAO KITAGUCHI | JAP | 2 | AO2 | SUZAKU OBSERVATION OF NON-CD ANTLIA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802035010/ | Quick Look | ![]() |
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509 | AWM7 EAST OFFSET | 44.9753 | 41.5792 | 44.161968 | 41.380907 | 54.762228 | 23.48981 | 147.26183994 | -15.14450792 | 259.3934 | 54492.7386458333 | 2008-01-27 17:43:39 | 54494.7016087963 | 2008-01-29 16:50:19 | 802044010 | 85.6177 | 80 | 85.6177 | 85.6177 | 0 | 85.6177 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.6003 | 80.6003 | 169.5838 | 1 | PROCESSED | 57541.4783333333 | 2016-06-02 11:28:48 | 54888 | 2009-02-26 00:00:00 | 54515.5758796296 | 2008-02-19 13:49:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020139 | The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOSHITAKA ISHISAKI | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802044010/ | Quick Look | ![]() |
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510 | NGC 2403 | 114.2007 | 65.5918 | 112.996594 | 65.703234 | 103.458828 | 43.277316 | 150.58117971 | 29.1798975 | 310.3004 | 53810.5896875 | 2006-03-16 14:09:09 | 53811.5884143518 | 2006-03-17 14:07:19 | 800021010 | 72.3687 | 70 | 72.3767 | 72.3687 | 72.3767 | 72.3767 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 59.3591 | 59.3591 | 86.2779 | 0 | PROCESSED | 57533.2480439815 | 2016-05-25 05:57:11 | 54247 | 2007-05-27 00:00:00 | 54042.0667708333 | 2006-11-03 01:36:09 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001101 | We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUO MAKISHIMA | JAP | 0 | SWG | A PROPOSAL FOR A 70 KSEC SUZAKU OBSERVATION OF THE NORMAL SPIRAL GALAXY NGC 2403 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800021010/ | Quick Look | ![]() |
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511 | AWM7 SOUTH OFFSET | 43.219 | 40.631 | 42.416618 | 40.42683 | 53.072384 | 23.000071 | 146.52769464 | -16.61135361 | 257.3934 | 54494.7028703704 | 2008-01-29 16:52:08 | 54496.618275463 | 2008-01-31 14:50:19 | 802045010 | 31.2959 | 0 | 31.3039 | 31.3039 | 0 | 31.2959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.2298 | 78.2298 | 165.4718 | 1 | PROCESSED | 57541.4808796296 | 2016-06-02 11:32:28 | 54888 | 2009-02-26 00:00:00 | 54515.1834837963 | 2008-02-19 04:24:13 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020139 | The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOSHITAKA ISHISAKI | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802045010/ | Quick Look | ![]() |
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512 | AWM7 45' SOUTH | 43.6476 | 40.9695 | 42.841958 | 40.766746 | 53.522914 | 23.219545 | 146.6593781 | -16.15981584 | 257.4009 | 55974.8888078704 | 2012-02-17 21:19:53 | 55975.6641087963 | 2012-02-18 15:56:19 | 806010010 | 34.3602 | 35 | 34.3602 | 34.3602 | 0 | 34.3602 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.0155 | 32.0155 | 66.978 | 1 | PROCESSED | 57604.6274768518 | 2016-08-04 15:03:34 | 56361 | 2013-03-10 00:00:00 | 55994.9866319444 | 2012-03-08 23:40:45 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806010010/ | Quick Look | ![]() |
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513 | A426VIR S | 48.9041 | 42.4908 | 48.073152 | 42.306326 | 58.095587 | 23.496379 | 149.35896709 | -12.86322568 | 271.5007 | 56708.3862962963 | 2014-02-20 09:16:16 | 56709.0453009259 | 2014-02-21 01:05:14 | 808085010 | 26.26 | 25 | 26.284 | 26.276 | 0 | 26.26 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.0267 | 21.0267 | 56.9339 | 1 | PROCESSED | 57613.8719560185 | 2016-08-13 20:55:37 | 57086 | 2015-03-05 00:00:00 | 56720.6405902778 | 2014-03-04 15:22:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808085010/ | Quick Look | ![]() |
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514 | A2199_FE | 248.2855 | 39.6383 | 247.85907 | 39.742227 | 234.702574 | 60.442801 | 63.09452591 | 42.82923772 | 143.2418 | 56662.5581597222 | 2014-01-05 13:23:45 | 56663.4606944444 | 2014-01-06 11:03:24 | 808051010 | 40.3548 | 40 | 40.3708 | 40.3548 | 0 | 40.3712 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39.8119 | 39.8119 | 77.9679 | 1 | PROCESSED | 57613.7559490741 | 2016-08-13 18:08:34 | 57085 | 2015-03-04 00:00:00 | 56719.7506597222 | 2014-03-03 18:00:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080067 | We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 8 | AO8 | COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808051010/ | Quick Look | ![]() |
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515 | 3EGJ1234 1318_1 | 188.0173 | -13.3363 | 187.367898 | -13.060386 | 192.646727 | -9.069223 | 295.70141073 | 49.26333697 | 109.7313 | 54081.3723032407 | 2006-12-12 08:56:07 | 54081.9273032407 | 2006-12-12 22:15:19 | 801031010 | 19.4098 | 20 | 19.4178 | 19.4178 | 0 | 19.4098 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.7228 | 18.7228 | 47.9499 | 1 | PROCESSED | 57536.3099768518 | 2016-05-28 07:26:22 | 54735 | 2008-09-26 00:00:00 | 54094.2359722222 | 2006-12-25 05:39:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010068 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOMONORI TOTANI | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801031010/ | Quick Look | ![]() |
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516 | 3EGJ1234 1318_2 | 188.017 | -13.0869 | 187.367769 | -12.810986 | 192.545784 | -8.84065 | 295.65674578 | 49.51103665 | 109.9322 | 54081.9277777778 | 2006-12-12 22:16:00 | 54082.7766087963 | 2006-12-13 18:38:19 | 801032010 | 30.9427 | 30 | 30.9667 | 30.9587 | 0 | 30.9427 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.083 | 26.083 | 73.3339 | 1 | PROCESSED | 57536.3393055556 | 2016-05-28 08:08:36 | 54735 | 2008-09-26 00:00:00 | 54094.2665740741 | 2006-12-25 06:23:52 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010068 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOMONORI TOTANI | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801032010/ | Quick Look | ![]() |
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517 | A3667_NW_17OFF | 302.869 | -56.6666 | 301.869632 | -56.815685 | 291.522519 | -35.657764 | 341.06051648 | -33.2513141 | 258.9342 | 54038.8325578704 | 2006-10-30 19:58:53 | 54039.0106944444 | 2006-10-31 00:15:24 | 801095020 | 11.9634 | 10 | 11.9794 | 11.9794 | 11.9634 | 11.9714 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.724 | 8.724 | 15.3839 | 0 | PROCESSED | 57535.9848032407 | 2016-05-27 23:38:07 | 54735 | 2008-09-26 00:00:00 | 54056.1858796296 | 2006-11-17 04:27:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801095020/ | Quick Look | ![]() |
518 | NGC 3079 | 150.4972 | 55.6116 | 149.652795 | 55.852826 | 130.116379 | 40.274577 | 157.90048948 | 48.39234685 | 268.6689 | 54612.8709722222 | 2008-05-26 20:54:12 | 54615.4362731482 | 2008-05-29 10:28:14 | 803039020 | 102.34 | 100 | 102.348 | 102.34 | 0 | 102.348 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102.0031 | 102.0031 | 221.6019 | 2 | PROCESSED | 57542.6909027778 | 2016-06-03 16:34:54 | 54999 | 2009-06-17 00:00:00 | 54633.7055439815 | 2008-06-16 16:55:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031303 | We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID STRICKLAND | USA | 3 | AO3 | NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN? | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803039020/ | Quick Look | ![]() |
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519 | A3667_NW_RELIC | 302.5617 | -56.3599 | 301.565299 | -56.507728 | 291.421165 | -35.317169 | 341.42703548 | -33.08195751 | 74.7123 | 53858.7409837963 | 2006-05-03 17:47:01 | 53861.2933449074 | 2006-05-06 07:02:25 | 801094010 | 94.3946 | 95 | 94.4026 | 94.3946 | 94.3946 | 94.4026 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 56.2506 | 56.2506 | 220.489 | 4 | PROCESSED | 57533.7274074074 | 2016-05-25 17:27:28 | 54394 | 2007-10-21 00:00:00 | 53913.7574189815 | 2006-06-27 18:10:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAZUHIRO NAKAZAWA | CRAIG SARAZIN | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801094010/ | Quick Look | ![]() |
520 | M87N BRIGHT | 187.7 | 12.7001 | 187.067492 | 12.976168 | 181.920384 | 14.695127 | 283.404729 | 74.78396174 | 297.7704 | 54625.0923263889 | 2008-06-08 02:12:57 | 54625.6259722222 | 2008-06-08 15:01:24 | 803070010 | 24.2485 | 20 | 24.2565 | 24.2485 | 0 | 24.2565 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.2709 | 20.2709 | 46.1039 | 1 | PROCESSED | 57542.7423263889 | 2016-06-03 17:48:57 | 55009 | 2009-06-27 00:00:00 | 54642.2018865741 | 2008-06-25 04:50:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032011 | We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | EUR | 3 | AO3 | THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803070010/ | Quick Look | ![]() |
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521 | A1689-OFFSET1 | 198.0484 | -1.2633 | 197.406048 | -0.99812 | 197.124113 | 5.910782 | 313.73996571 | 61.17214089 | 289.9985 | 54670.1962962963 | 2008-07-23 04:42:40 | 54671.3488773148 | 2008-07-24 08:22:23 | 803024010 | 47.0703 | 40 | 47.0703 | 47.0813 | 0 | 47.0783 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36.3283 | 36.3283 | 99.5439 | 1 | PROCESSED | 57543.121412037 | 2016-06-04 02:54:50 | 55076 | 2009-09-02 00:00:00 | 54707.0796180556 | 2008-08-29 01:54:39 | 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/ver3.0/803024010/ | Quick Look | ![]() |
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522 | A2029_5 | 227.4808 | 5.8608 | 226.861375 | 6.050047 | 223.225848 | 22.663782 | 6.38223601 | 50.81650996 | 112.9567 | 55226.2508912037 | 2010-01-30 06:01:17 | 55226.875162037 | 2010-01-30 21:00:14 | 804024050 | 21.891 | 22 | 21.891 | 21.891 | 0 | 21.891 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.3419 | 14.3419 | 53.936 | 0 | PROCESSED | 57550.432337963 | 2016-06-11 10:22:34 | 55638 | 2011-03-18 00:00:00 | 55272.0370717593 | 2010-03-17 00:53:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required 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 breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024050/ | Quick Look | ![]() |
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523 | NGC741S2_P2 | 29.0179 | 5.3952 | 28.364923 | 5.150978 | 28.892288 | -6.076565 | 150.99426375 | -53.91742537 | 71.6631 | 55053.608287037 | 2009-08-10 14:35:56 | 55053.8425347222 | 2009-08-10 20:13:15 | 804055020 | 10.5481 | 10 | 10.5481 | 10.5481 | 0 | 10.5481 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.548 | 9.548 | 20.2299 | 0 | PROCESSED | 57548.1047800926 | 2016-06-09 02:30:53 | 55465 | 2010-09-26 00:00:00 | 55098.1704166667 | 2009-09-24 04:05:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804055020/ | Quick Look | ![]() |
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524 | AWM7 EAST OFFSET | 44.0318 | 41.5949 | 43.221288 | 41.393422 | 54.035202 | 23.723269 | 146.61375919 | -15.47239178 | 90.4995 | 53952.2676967593 | 2006-08-05 06:25:29 | 53953.2398611111 | 2006-08-06 05:45:24 | 801036010 | 38.5361 | 40 | 38.5361 | 38.5361 | 38.5361 | 38.5361 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37.541 | 37.541 | 83.9599 | 0 | PROCESSED | 57535.0870138889 | 2016-05-27 02:05:18 | 54394 | 2007-10-21 00:00:00 | 54020.7498726852 | 2006-10-12 17:59:49 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801036010/ | Quick Look | ![]() |
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525 | FJ0854+4908 | 133.7471 | 49.1347 | 132.871607 | 49.325626 | 121.634271 | 30.384389 | 170.1345398 | 40.07327965 | 275.4931 | 56775.9268865741 | 2014-04-28 22:14:43 | 56776.9669328704 | 2014-04-29 23:12:23 | 809038010 | 43.4713 | 45 | 43.4713 | 43.4713 | 0 | 43.4713 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.2119 | 40.2119 | 89.8479 | 1 | PROCESSED | 57615.0216666667 | 2016-08-15 00:31:12 | 57214 | 2015-07-11 00:00:00 | 56848.6454166667 | 2014-07-10 15:29:24 | 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/ver3.0/809038010/ | Quick Look | ![]() |
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526 | A1914_OFFSET2 | 216.77 | 37.7885 | 216.258243 | 38.012199 | 196.723878 | 48.617689 | 66.91478771 | 67.27662817 | 134.0016 | 55565.7291203704 | 2011-01-04 17:29:56 | 55566.0216550926 | 2011-01-05 00:31:11 | 805092020 | 17.0912 | 12 | 17.0992 | 17.0912 | 0 | 17.1072 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.2058 | 13.2058 | 25.2719 | 0 | PROCESSED | 57600.5511689815 | 2016-07-31 13:13:41 | 56037 | 2012-04-20 00:00:00 | 55670.1137384259 | 2011-04-19 02:43:47 | 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 | 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/ver3.0/805092020/ | Quick Look | ![]() |
527 | AWM7 NW1 | 42.8658 | 41.9211 | 42.057041 | 41.715759 | 53.244699 | 24.307791 | 145.6578115 | -15.59334332 | 257 | 56705.5358680556 | 2014-02-17 12:51:39 | 56705.8668287037 | 2014-02-17 20:48:14 | 808023010 | 14.8576 | 15 | 14.8896 | 14.8576 | 0 | 14.8736 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.0088 | 11.0088 | 28.5839 | 1 | PROCESSED | 57613.8366550926 | 2016-08-13 20:04:47 | 57085 | 2015-03-04 00:00:00 | 56719.7185532407 | 2014-03-03 17:14:43 | 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/ver3.0/808023010/ | Quick Look | ![]() |
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528 | A2199 OFFSET14 | 246.2604 | 39.5212 | 245.829944 | 39.634196 | 231.792856 | 59.849359 | 62.86911341 | 44.38588157 | 254.9999 | 55825.6665625 | 2011-09-21 15:59:51 | 55826.3946527778 | 2011-09-22 09:28:18 | 806160010 | 27.4413 | 30 | 27.4414 | 27.4413 | 0 | 27.4413 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 26.9491 | 26.9491 | 62.9019 | 0 | PROCESSED | 57603.222962963 | 2016-08-03 05:21:04 | 55652 | 2011-04-01 00:00:00 | 55851.4517361111 | 2011-10-17 10:50:30 | 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/ver3.0/806160010/ | Quick Look | ![]() |
529 | COMA E5.5 | 196.6115 | 27.8944 | 196.012448 | 28.161547 | 183.085886 | 31.985086 | 46.75951976 | 86.58537166 | 280.0017 | 55730.7852546296 | 2011-06-18 18:50:46 | 55731.2738657407 | 2011-06-19 06:34:22 | 806035010 | 10.8791 | 15 | 10.8871 | 10.8871 | 0 | 10.8791 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.5597 | 12.5597 | 42.1979 | 0 | PROCESSED | 57602.3474537037 | 2016-08-02 08:20:20 | 55652 | 2011-04-01 00:00:00 | 55770.1742939815 | 2011-07-28 04:10:59 | 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/ver3.0/806035010/ | Quick Look | ![]() |
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530 | A2104E | 235.1486 | -3.297 | 234.495076 | -3.136609 | 233.617797 | 15.850396 | 2.9252225 | 39.1285511 | 117.6908 | 54118.1261226852 | 2007-01-18 03:01:37 | 54118.6850231482 | 2007-01-18 16:26:26 | 801003010 | 22.7847 | 20 | 22.7847 | 22.7847 | 0 | 22.7847 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.7352 | 17.7352 | 48.2879 | 1 | PROCESSED | 57536.8549189815 | 2016-05-28 20:31:05 | 54735 | 2008-09-26 00:00:00 | 54132.8631365741 | 2007-02-01 20:42:55 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801003010/ | Quick Look | ![]() |
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531 | A399/401 FILAMENT | 44.7475 | 13.2485 | 44.061375 | 13.049612 | 46.15841 | -3.573964 | 164.45015039 | -39.12843885 | 74.1756 | 53966.1736921296 | 2006-08-19 04:10:07 | 53969.4641666667 | 2006-08-22 11:08:24 | 801020010 | 151.0601 | 150 | 151.0601 | 151.0681 | 151.0681 | 151.0681 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 142.2036 | 142.2036 | 284.2738 | 5 | PROCESSED | 57535.3984837963 | 2016-05-27 09:33:49 | 54526 | 2008-03-01 00:00:00 | 54021.1056944444 | 2006-10-13 02:32:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010063 | Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YUTAKA FUJITA | JAP | 1 | AO1 | THE DETECTION OF WHIM IN THE A399/401 FILAMENT | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801020010/ | Quick Look | ![]() |
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532 | ABELL 2204 | 248.0963 | 5.6404 | 247.481247 | 5.74563 | 245.314616 | 27.222606 | 21.10023438 | 33.35451369 | 261.3606 | 53995.3098958333 | 2006-09-17 07:26:15 | 53996.5098958333 | 2006-09-18 12:14:15 | 801091010 | 49.1113 | 55 | 49.1113 | 49.1113 | 49.1113 | 49.1113 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 51.9372 | 51.9372 | 103.6439 | 1 | PROCESSED | 57535.6038194444 | 2016-05-27 14:29:30 | 54526 | 2008-03-01 00:00:00 | 54020.8840277778 | 2006-10-12 21:13:00 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012018 | Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | THOMAS REIPRICH | EUR | 1 | AO1 | A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS | SPE | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801091010/ | Quick Look | ![]() |
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533 | A1060_OFFSET | 159.8425 | -27.5312 | 159.252316 | -27.270314 | 173.386883 | -33.06567 | 270.15539037 | 26.80693828 | 96.4852 | 54425.0245486111 | 2007-11-21 00:35:21 | 54427.7988888889 | 2007-11-23 19:10:24 | 802028010 | 103.7993 | 100 | 103.7993 | 103.7993 | 0 | 103.7993 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.1119 | 89.1119 | 239.6797 | 2 | PROCESSED | 57540.6102662037 | 2016-06-01 14:38:47 | 54804 | 2008-12-04 00:00:00 | 54434.2515509259 | 2007-11-30 06:02:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020060 | We propose to observe a 30' offset region of the cluster of galaxies Abell 1060 for 100 ksec to study the temperature and abundance profiles. The central region within ~0.3 times the virial radius, or 380 kpc, has been already observed as one of the SWG targets, and the temperature decrease and differnt profiles of metal abundances are clealy observed (Sato et al. 2006). This observation will reveal the temperature and abundance profiles to half the virial radius. Comparison of the abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the outer cluster region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 2 | AO2 | TEMPERATURE AND ABUNDANCE PROFILES IN THE OUTER REGION OF THE NON-CD CLUSTER A1060 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802028010/ | Quick Look | ![]() |
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534 | A2142 OFFSET2 | 239.2185 | 27.5666 | 238.702662 | 27.710117 | 228.594218 | 46.67807 | 44.63617571 | 49.06945571 | 260.7114 | 54358.4806597222 | 2007-09-15 11:32:09 | 54360.0627893518 | 2007-09-17 01:30:25 | 802031010 | 57.7187 | 50 | 57.7187 | 57.7187 | 0 | 57.7187 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 52.5976 | 52.5976 | 136.6318 | 1 | PROCESSED | 57539.9791666667 | 2016-05-31 23:30:00 | 54751 | 2008-10-12 00:00:00 | 54371.4005208333 | 2007-09-28 09:36:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020076 | We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802031010/ | Quick Look | ![]() |
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535 | AWM7 SOUTH OFFSET | 43.2198 | 40.6314 | 42.417413 | 40.427233 | 53.073147 | 23.000259 | 146.52805812 | -16.61071542 | 257.3937 | 54519.4104861111 | 2008-02-23 09:51:06 | 54521.6112847222 | 2008-02-25 14:40:15 | 802045020 | 91.2272 | 80 | 91.2272 | 91.2272 | 0 | 91.2272 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.0285 | 80.0285 | 190.1139 | 2 | PROCESSED | 57541.7536111111 | 2016-06-02 18:05:12 | 54904 | 2009-03-14 00:00:00 | 54535.283599537 | 2008-03-10 06:48:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020139 | The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOSHITAKA ISHISAKI | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802045020/ | Quick Look | ![]() |
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536 | COMABKG | 198.7472 | 31.648 | 198.161117 | 31.912033 | 183.000201 | 36.170261 | 75.72732699 | 83.16527783 | 295.0754 | 54272.0100347222 | 2007-06-21 00:14:27 | 54272.7015046296 | 2007-06-21 16:50:10 | 802083010 | 30.7831 | 30 | 30.7831 | 30.7831 | 0 | 30.7831 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.5058 | 26.5058 | 59.7399 | 0 | PROCESSED | 57539.0181597222 | 2016-05-31 00:26:09 | 54702 | 2008-08-24 00:00:00 | 54333.4315393518 | 2007-08-21 10:21:25 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024438 | Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JOEL BREGMAN | Yoh Takei | USJ | 2 | AO2 | THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802083010/ | Quick Look | ![]() |
537 | N44 SB | 80.6234 | -67.9392 | 80.661581 | -67.984502 | 334.827675 | -86.129494 | 278.35092966 | -33.30497245 | 311.8533 | 54565.7359143518 | 2008-04-09 17:39:43 | 54566.5084953704 | 2008-04-10 12:12:14 | 803036010 | 30.5568 | 30 | 30.5568 | 30.5568 | 0 | 30.5568 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.9118 | 26.9118 | 66.748 | 1 | PROCESSED | 57542.2791898148 | 2016-06-03 06:42:02 | 54946 | 2009-04-25 00:00:00 | 54580.4450810185 | 2008-04-24 10:40:55 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LARRY MADDOX | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803036010/ | Quick Look | ![]() |
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538 | NGC 4406 | 186.5483 | 12.9401 | 185.91466 | 13.216832 | 180.759915 | 14.456271 | 279.08850556 | 74.63107328 | 294.6659 | 55001.7603125 | 2009-06-19 18:14:51 | 55004.4793287037 | 2009-06-22 11:30:14 | 803043010 | 101.7736 | 90 | 101.7736 | 101.7736 | 0 | 101.7736 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86.5545 | 86.5545 | 234.8981 | 2 | PROCESSED | 57547.6610300926 | 2016-06-08 15:51:53 | 55384 | 2010-07-07 00:00:00 | 55015.2472569445 | 2009-07-03 05:56:03 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031404 | We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MICHAEL LOEWENSTEIN | USA | 3 | AO3 | UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803043010/ | Quick Look | ![]() |
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539 | DEM L 192 | 81.4194 | -67.497 | 81.444182 | -67.538512 | 340.379487 | -86.530508 | 277.77177426 | -33.0775429 | 334.6993 | 54968.6808680556 | 2009-05-17 16:20:27 | 54971.0113310185 | 2009-05-20 00:16:19 | 804009010 | 87.3165 | 80 | 87.3245 | 87.3165 | 0 | 87.3245 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80.0589 | 80.0589 | 201.3277 | 2 | PROCESSED | 57546.6405439815 | 2016-06-07 15:22:23 | 55356 | 2010-06-09 00:00:00 | 54987.4577314815 | 2009-06-05 10:59:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040009 | The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYA YAMAGUCHI | JAP | 4 | AO4 | DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804009010/ | Quick Look | ![]() |
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540 | FERMI_0281 | 197.9603 | -34.4918 | 197.262031 | -34.226396 | 210.309678 | -24.734564 | 307.70107754 | 28.19093927 | 309.4896 | 55047.2059606482 | 2009-08-04 04:56:35 | 55048.3043287037 | 2009-08-05 07:18:14 | 804018010 | 39.9038 | 40 | 39.9038 | 39.9038 | 0 | 39.9038 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.5708 | 35.5708 | 94.8819 | 1 | PROCESSED | 57548.0705902778 | 2016-06-09 01:41:39 | 55423 | 2010-08-15 00:00:00 | 55060.7435763889 | 2009-08-17 17:50:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804018010/ | Quick Look | ![]() |
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541 | NGC 5174 | 202.3569 | 11.0203 | 201.73681 | 11.278322 | 196.356635 | 18.897363 | 333.76702191 | 71.58014685 | 102.4436 | 55219.0472685185 | 2010-01-23 01:08:04 | 55220.5835532407 | 2010-01-24 14:00:19 | 804048010 | 54.5151 | 50 | 54.5231 | 54.5151 | 0 | 54.5231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.0362 | 44.0362 | 132.6979 | 0 | PROCESSED | 57550.3479050926 | 2016-06-11 08:20:59 | 55595 | 2011-02-03 00:00:00 | 55229.1361226852 | 2010-02-02 03:16:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041504 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | JOEL BREGMAN | USA | 4 | AO4 | THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804048010/ | Quick Look | ![]() |
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542 | FORNAX A W-LOBE N | 50.5227 | -36.9675 | 50.043813 | -37.145451 | 32.738272 | -52.85468 | 239.75066849 | -56.83654313 | 27.8129 | 54991.7546875 | 2009-06-09 18:06:45 | 54992.8119675926 | 2009-06-10 19:29:14 | 804037010 | 60.7627 | 50 | 60.7707 | 60.7627 | 0 | 60.7707 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.817 | 54.817 | 91.3258 | 1 | PROCESSED | 57547.5602777778 | 2016-06-08 13:26:48 | 55367 | 2010-06-20 00:00:00 | 55001.1883912037 | 2009-06-19 04:31:17 | 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/ver3.0/804037010/ | Quick Look | ![]() |
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543 | A1795_FAR_SOUTHWEST | 206.9673 | 26.3143 | 206.388758 | 26.56302 | 193.820617 | 34.636362 | 32.43951308 | 77.37921169 | 300.5685 | 55011.5565162037 | 2009-06-29 13:21:23 | 55012.4849537037 | 2009-06-30 11:38:20 | 804083010 | 38.3573 | 35 | 38.3573 | 38.6253 | 0 | 38.6333 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57598.4742013889 | 2016-07-29 11:22:51 | 55395 | 2010-07-18 00:00:00 | 55027.5898726852 | 2009-07-15 14:09:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804083010/ | Quick Look | ![]() |
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544 | A2204_FIELD_1 | 248.3552 | 5.4547 | 247.739346 | 5.558766 | 245.63481 | 27.082232 | 21.05505633 | 33.03914402 | 261.0004 | 55440.0008217593 | 2010-09-01 00:01:11 | 55441.1467013889 | 2010-09-02 03:31:15 | 805056010 | 40.6674 | 40 | 40.6674 | 40.6674 | 0 | 40.6674 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.488 | 37.488 | 98.9941 | 1 | PROCESSED | 57553.2764699074 | 2016-06-14 06:38:07 | 55287 | 2010-04-01 00:00:00 | 55456.099849537 | 2010-09-17 02:23:47 | 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/ver3.0/805056010/ | Quick Look | ![]() |
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545 | NGC3402 OFF-CENTER | 162.4923 | -13.1954 | 161.871445 | -12.930338 | 169.151232 | -19.021161 | 262.91388856 | 40.05493452 | 124.5885 | 55557.4779513889 | 2010-12-27 11:28:15 | 55558.1231134259 | 2010-12-28 02:57:17 | 805070010 | 27.8664 | 30 | 27.8744 | 27.8744 | 0 | 27.8664 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0294 | 25.0294 | 55.74 | 1 | PROCESSED | 57554.5274421296 | 2016-06-15 12:39:31 | 55961 | 2012-02-04 00:00:00 | 55595.0278703704 | 2011-02-03 00:40:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805070010/ | Quick Look | ![]() |
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546 | ABELL 115 | 13.9939 | 26.3802 | 13.320825 | 26.109701 | 23.360956 | 18.75409 | 124.19588168 | -36.48041221 | 44.0022 | 55401.606087963 | 2010-07-24 14:32:46 | 55403.0529398148 | 2010-07-26 01:16:14 | 805077010 | 66.1556 | 65 | 66.1629 | 66.1556 | 0 | 66.1829 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.8298 | 61.8298 | 124.968 | 2 | PROCESSED | 57552.6853472222 | 2016-06-13 16:26:54 | 55780 | 2011-08-07 00:00:00 | 55414.1298148148 | 2010-08-06 03:06:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051521 | We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCOTT RANDALL | USA | 5 | AO5 | THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805077010/ | Quick Look | ![]() |
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547 | ABELL 2537 | 347.0895 | -2.1864 | 346.446208 | -2.457426 | 347.265087 | 3.085071 | 73.83613509 | -54.91382092 | 56.4647 | 55368.5295486111 | 2010-06-21 12:42:33 | 55371.9946875 | 2010-06-24 23:52:21 | 805090010 | 124.8232 | 129 | 124.8472 | 124.8232 | 0 | 124.8472 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 108.3908 | 108.3908 | 281.2176 | 1 | PROCESSED | 57552.4996412037 | 2016-06-13 11:59:29 | 55772 | 2011-07-30 00:00:00 | 55403.4592361111 | 2010-07-26 11:01:18 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052007 | Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reductions and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | THOMAS REIPRICH | EUR | 5 | AO5 | COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTER A2537 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805090010/ | Quick Look | ![]() |
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548 | ABELL 426 W1 | 49.5928 | 41.5523 | 48.766062 | 41.370352 | 58.34119 | 22.451611 | 150.3228425 | -13.37443973 | 94.0008 | 55428.5346759259 | 2010-08-20 12:49:56 | 55428.7397569445 | 2010-08-20 17:45:15 | 805103010 | 10.068 | 10 | 10.068 | 10.068 | 0 | 10.068 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.3213 | 7.3213 | 17.7119 | 0 | PROCESSED | 57553.1427777778 | 2016-06-14 03:25:36 | 55287 | 2010-04-01 00:00:00 | 55439.2175 | 2010-08-31 05:13:12 | 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/ver3.0/805103010/ | Quick Look | ![]() |
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549 | A1795_NEAR_WEST | 206.9975 | 26.5902 | 206.419777 | 26.838853 | 193.705375 | 34.896895 | 33.70837645 | 77.38236805 | 300.5681 | 55009.4637962963 | 2009-06-27 11:07:52 | 55010.100162037 | 2009-06-28 02:24:14 | 804085010 | 24.2664 | 20 | 24.2664 | 24.5363 | 0 | 24.5203 | 5 | 2 | 0 | 2 | 1 | 0 | 0 | 9.9711 | 9.9711 | 22.7619 | 0 | PROCESSED | 57598.4788425926 | 2016-07-29 11:29:32 | 55386 | 2010-07-09 00:00:00 | 55020.3655555556 | 2009-07-08 08:46:24 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ERIC MILLER | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804085010/ | Quick Look | ![]() |
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550 | FORNAX CLUSTER NORTH | 54.7043 | -35.2293 | 54.224181 | -35.391159 | 39.001198 | -52.608062 | 236.34100564 | -53.57224957 | 244.9996 | 53741.5137847222 | 2006-01-06 12:19:51 | 53742.3336111111 | 2006-01-07 08:00:24 | 800002020 | 37.1921 | 80 | 37.1921 | 37.2161 | 37.2081 | 37.2001 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.2874 | 39.2874 | 70.8159 | 1 | PROCESSED | 57532.6432291667 | 2016-05-24 15:26:15 | 54247 | 2007-05-27 00:00:00 | 54039.8151041667 | 2006-10-31 19:33:45 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002020/ | Quick Look | ![]() |
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551 | NGC3628 | 170.0699 | 13.5986 | 169.41715 | 13.872528 | 165.514956 | 8.570385 | 240.83294046 | 64.7853987 | 100 | 55890.624212963 | 2011-11-25 14:58:52 | 55892.4070601852 | 2011-11-27 09:46:10 | 806018010 | 81.5115 | 80 | 81.5275 | 81.5115 | 0 | 81.5218 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.5925 | 70.5925 | 153.9938 | 1 | PROCESSED | 57603.996087963 | 2016-08-03 23:54:22 | 56269 | 2012-12-08 00:00:00 | 55901.2586689815 | 2011-12-06 06:12:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060082 | We propose 80 ksec observations of edge-on nearby spiral starburst galaxies, NGC3628 and NGC891. We aim to obtain the temperature and the abundance pattern in both the disk and halo regions of two starburst galaxies and hopefully constrain the model of the interactions between not only disk and halo but also halo and intergalactic medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IKUYUKI MITSUISHI | JAP | 6 | AO6 | OBSERVATIONS OF AN EDGE-ON STARBURST GALAXIES NGC3628 & NGC891 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806018010/ | Quick Look | ![]() |
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552 | AWM7 SE2 | 44.7376 | 40.9954 | 43.928492 | 40.796305 | 54.382202 | 22.988972 | 147.39655193 | -15.74105021 | 257.0003 | 56707.1291319444 | 2014-02-19 03:05:57 | 56707.9132407407 | 2014-02-19 21:55:04 | 808026010 | 35.304 | 35 | 35.304 | 35.316 | 0 | 35.308 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.1778 | 31.1778 | 67.742 | 4 | PROCESSED | 57613.8746064815 | 2016-08-13 20:59:26 | 57085 | 2015-03-04 00:00:00 | 56719.7754398148 | 2014-03-03 18:36:38 | 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/ver3.0/808026010/ | Quick Look | ![]() |
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553 | COMA NW3.5 | 194.5289 | 28.7386 | 193.925957 | 29.008414 | 180.709004 | 31.910374 | 80.83345269 | 87.81635354 | 116.0021 | 55917.9522685185 | 2011-12-22 22:51:16 | 55918.5091898148 | 2011-12-23 12:13:14 | 806040020 | 16.7407 | 15 | 16.7407 | 16.7631 | 0 | 16.7487 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.8051 | 15.8051 | 48.1159 | 0 | PROCESSED | 57604.2115509259 | 2016-08-04 05:04:38 | 55652 | 2011-04-01 00:00:00 | 55972.6802662037 | 2012-02-15 16:19:35 | 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/ver3.0/806040020/ | Quick Look | ![]() |
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554 | A262 NE2 | 28.537 | 36.7219 | 27.798764 | 36.476514 | 39.918494 | 23.346467 | 136.69850182 | -24.46778258 | 249.9995 | 56703.1881712963 | 2014-02-15 04:30:58 | 56703.8821643518 | 2014-02-15 21:10:19 | 808109010 | 32.9447 | 32 | 32.9527 | 32.9607 | 0 | 32.9447 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8208564815 | 2016-08-13 19:42:02 | 57080 | 2015-02-27 00:00:00 | 56714.743275463 | 2014-02-26 17:50:19 | 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 | A | 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/ver3.0/808109010/ | Quick Look | ![]() |
555 | RXCJ0605 | 91.4642 | -35.1179 | 91.019375 | -35.111883 | 92.302761 | -58.547808 | 241.59260677 | -23.96271915 | 309.9856 | 55323.8555555556 | 2010-05-07 20:32:00 | 55324.6821412037 | 2010-05-08 16:22:17 | 805065040 | 43.6946 | 40 | 43.6946 | 43.6946 | 0 | 43.7106 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.3321 | 39.3321 | 71.4139 | 0 | PROCESSED | 57551.4409837963 | 2016-06-12 10:35:01 | 55287 | 2010-04-01 00:00:00 | 55341.5146990741 | 2010-05-25 12:21:10 | 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/ver3.0/805065040/ | Quick Look | ![]() |
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556 | COMA E3 | 195.8278 | 27.896 | 195.226801 | 28.164193 | 182.356899 | 31.675143 | 49.87218267 | 87.25778961 | 279.9974 | 55729.4896064815 | 2011-06-17 11:45:02 | 55729.6863078704 | 2011-06-17 16:28:17 | 806032010 | 7.9801 | 10 | 7.9801 | 7.9801 | 0 | 7.9801 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.764 | 5.764 | 16.9839 | 0 | PROCESSED | 57602.3229976852 | 2016-08-02 07:45:07 | 55652 | 2011-04-01 00:00:00 | 55770.1022453704 | 2011-07-28 02:27:14 | 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/ver3.0/806032010/ | Quick Look | ![]() |
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557 | FORNAX A LOBE BKG | 50.9375 | -37.5569 | 50.463091 | -37.733287 | 32.824918 | -53.528276 | 240.74738045 | -56.44161041 | 91.6954 | 56510.6236458333 | 2013-08-06 14:58:03 | 56511.9333912037 | 2013-08-07 22:24:05 | 808044010 | 54.4545 | 50 | 54.4625 | 54.4545 | 0 | 54.4705 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.8925 | 46.8925 | 113.1478 | 1 | PROCESSED | 57612.1934837963 | 2016-08-12 04:38:37 | 56955 | 2014-10-25 00:00:00 | 56587.7940046296 | 2013-10-22 19:03:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080056 | We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 8 | AO8 | COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808044010/ | Quick Look | ![]() |
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558 | N103B | 77.15 | -68.7359 | 77.208253 | -68.79772 | 330.089921 | -84.667648 | 279.60217418 | -34.399508 | 199.4598 | 55194.4728356482 | 2009-12-29 11:20:53 | 55200.6044560185 | 2010-01-04 14:30:25 | 804039010 | 223.8999 | 150 | 224.0108 | 223.8999 | 0 | 224.0028 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.096 | 46.096 | 129.9558 | 0 | PROCESSED | 57550.0511805556 | 2016-06-11 01:13:42 | 55584 | 2011-01-23 00:00:00 | 55218.4707060185 | 2010-01-22 11:17:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040080 | We aim to detect very low abundance lines, Cr and Mn, from SNR N103B in the Large Magellanic Cloud which is a low metaricity galaxy. It is known that a mass ratio of Mn to Cr synthesized in Type Ia supernovae is strongly correrated with the metaricity of the progenitor white dwarf. In the early Suzaku observation, we already detected the Cr line with about 3-sigma confidence level. In this follow-up observation, we detect the Cr and Mn lines with significant confidence, and determine the metaricity of the progenitor of SNR N103B. This will be the first measurement of the white dwarf's metaricity in the extra-galactic object. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TORU TAMAGAWA | JAP | 4 | AO4 | A MANGANESE LINE DETECTION FROM SNR N103B IN A LOW METARICITY GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804039010/ | Quick Look | ![]() |
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559 | A478 OFFSET B | 63.3675 | 10.7352 | 62.68015 | 10.608912 | 63.410539 | -10.281556 | 182.20374123 | -28.1098658 | 260.0004 | 55601.549849537 | 2011-02-09 13:11:47 | 55602.6897685185 | 2011-02-10 16:33:16 | 805002010 | 45.3211 | 45 | 45.3211 | 45.3211 | 0 | 45.3211 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.2117 | 34.2117 | 98.4779 | 1 | PROCESSED | 57600.9178935185 | 2016-07-31 22:01:46 | 55983 | 2012-02-26 00:00:00 | 55617.4110763889 | 2011-02-25 09:51:57 | 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/ver3.0/805002010/ | Quick Look | ![]() |
560 | N49 | 81.5075 | -66.0821 | 81.488489 | -66.123294 | 4.042744 | -86.564563 | 276.09278992 | -33.24378088 | 327.2258 | 56056.8032986111 | 2012-05-09 19:16:45 | 56060.6898148148 | 2012-05-13 16:33:20 | 807007010 | 184.543 | 190 | 184.559 | 184.543 | 0 | 184.559 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 206.5829 | 206.5829 | 335.7558 | 3 | PROCESSED | 57605.4699189815 | 2016-08-05 11:16:41 | 56527 | 2013-08-23 00:00:00 | 56161.1703935185 | 2012-08-22 04:05:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070036 | Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROYUKI UCHIDA | JAP | 7 | AO7 | FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807007010/ | Quick Look | ![]() |
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561 | ABELL 3364 | 87.0888 | -31.8215 | 86.620794 | -31.836795 | 85.667368 | -55.219752 | 236.92588426 | -26.48475311 | 295.0036 | 55670.3589699074 | 2011-04-19 08:36:55 | 55670.9259027778 | 2011-04-19 22:13:18 | 806067020 | 29.9913 | 29.5 | 29.9993 | 29.9913 | 0 | 30.0073 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26.718 | 26.718 | 48.9759 | 0 | PROCESSED | 57601.5361689815 | 2016-08-01 12:52:05 | 56067 | 2012-05-20 00:00:00 | 55691.2162037037 | 2011-05-10 05:11:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | 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 none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. 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 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067020/ | Quick Look | ![]() |
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562 | CENTAURUS CLUSTER NW | 191.8913 | -40.8227 | 191.202719 | -40.549873 | 208.557036 | -32.526985 | 302.14149361 | 22.04310508 | 292.0001 | 56850.5075462963 | 2014-07-12 12:10:52 | 56854.4064236111 | 2014-07-16 09:45:15 | 809007010 | 147.8889 | 150 | 147.8889 | 148.5689 | 0 | 148.5689 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6625 | 14.6625 | 46.016 | 1 | PROCESSED | 57615.4267476852 | 2016-08-15 10:14:31 | 57283 | 2015-09-18 00:00:00 | 56917.6316666667 | 2014-09-17 15:09:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090031 | We propose to observe the north-west offset (20'--40' or 0.4--0.8 r500) of the Centaurus cluster with a 150 ks exposure. A previous Suzaku observation with a 10 ks exposure yielded a very low Fe abundance (0.0-0.1 solar) in the ICM. With a 150 ks exposure, we will detect the Fe-K line of He-like Fe and derive Fe abundance with an accuracy of 0.05 solar. Then, we will be able to study the validity of the Fe abundance derived from the Fe L lines from cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 9 | AO9 | COMPARISON OF THE FE ABUNDANCES FROM THE L AND K LINES FROM THE CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809007010/ | Quick Look | ![]() |
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563 | ABELL 3364 | 86.7248 | -31.9341 | 86.257494 | -31.951159 | 85.117761 | -55.320671 | 236.9466602 | -26.81319905 | 295.0042 | 55670.9264699074 | 2011-04-19 22:14:07 | 55671.5940162037 | 2011-04-20 14:15:23 | 806067030 | 30.7802 | 29.5 | 30.7802 | 30.7802 | 0 | 30.7802 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.2762 | 30.2762 | 57.6639 | 1 | PROCESSED | 57601.5516782407 | 2016-08-01 13:14:25 | 56059 | 2012-05-12 00:00:00 | 55692.1831018518 | 2011-05-11 04:23:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | 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 none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. 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 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067030/ | Quick Look | ![]() |
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564 | A3526 | 191.5735 | -40.3305 | 190.887021 | -40.05737 | 208.034799 | -32.201568 | 301.8706053 | 22.53064841 | 109.9984 | 55943.2367592593 | 2012-01-17 05:40:56 | 55943.6161574074 | 2012-01-17 14:47:16 | 806087010 | 14.4943 | 13 | 14.4943 | 14.4943 | 0 | 14.4943 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.3865 | 10.3865 | 32.7799 | 1 | PROCESSED | 57604.3860416667 | 2016-08-04 09:15:54 | 56332 | 2013-02-09 00:00:00 | 55964.1523148148 | 2012-02-07 03:39:20 | 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/ver3.0/806087010/ | Quick Look | ![]() |
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565 | A3526 | 191.429 | -40.092 | 190.743483 | -39.818735 | 207.789532 | -32.040636 | 301.74515791 | 22.76656347 | 109.9976 | 55943.6166319444 | 2012-01-17 14:47:57 | 55943.9461111111 | 2012-01-17 22:42:24 | 806088010 | 15.0662 | 14 | 15.0702 | 15.0662 | 0 | 15.0662 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.8434 | 14.8434 | 28.458 | 1 | PROCESSED | 57604.3884490741 | 2016-08-04 09:19:22 | 56332 | 2013-02-09 00:00:00 | 55964.2169675926 | 2012-02-07 05:12:26 | 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/ver3.0/806088010/ | Quick Look | ![]() |
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566 | ABELL 426 SW3.5 | 48.9544 | 40.9043 | 48.133622 | 40.720026 | 57.647111 | 21.964183 | 150.27094965 | -14.17935173 | 88.4992 | 55801.3110763889 | 2011-08-28 07:27:57 | 55801.6063888889 | 2011-08-28 14:33:12 | 806103010 | 10.2636 | 10 | 10.2636 | 10.2636 | 0 | 10.2636 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.5689 | 9.5689 | 25.4719 | 1 | PROCESSED | 57602.9865046296 | 2016-08-02 23:40:34 | 55652 | 2011-04-01 00:00:00 | 55825.0922337963 | 2011-09-21 02:12:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806103010/ | Quick Look | ![]() |
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567 | Z348 | 16.7077 | 1.0407 | 16.065796 | 0.773597 | 15.79467 | -5.606239 | 131.03941429 | -61.58850223 | 247.9196 | 54110.9286689815 | 2007-01-10 22:17:17 | 54111.5259722222 | 2007-01-11 12:37:24 | 801050010 | 22.6477 | 23 | 22.6477 | 22.6477 | 0 | 22.6477 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.3403 | 21.3403 | 51.589 | 1 | PROCESSED | 57536.8362384259 | 2016-05-28 20:04:11 | 54735 | 2008-09-26 00:00:00 | 54133.0321643518 | 2007-02-02 00:46:19 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010098 | We propose to carry out the Suzaku/XIS observations of 4 massive clusters at low redshifts (z <0.3). Combining the X-ray data with the existing Subaru datasets that allow us to directly reconstruct the mass distribution from the gravitational lensing measurements, we will investigate the physical relations between the mass and gas distributions to understand the nature of cluster in a quantitative way. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOSHIFUMI FUTAMASE | JAP | 1 | AO1 | THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801050010/ | Quick Look | ![]() |
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568 | ABELL 426 SW4.5 | 48.6726 | 40.7228 | 47.853753 | 40.537505 | 57.371332 | 21.850286 | 150.18660509 | -14.44721412 | 88.498 | 55801.850474537 | 2011-08-28 20:24:41 | 55802.08625 | 2011-08-29 02:04:12 | 806105010 | 10.7494 | 10 | 10.7574 | 10.7574 | 0 | 10.7494 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.915 | 8.915 | 20.3679 | 0 | PROCESSED | 57602.9947337963 | 2016-08-02 23:52:25 | 55652 | 2011-04-01 00:00:00 | 55826.0978935185 | 2011-09-22 02:20:58 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806105010/ | Quick Look | ![]() |
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569 | ABELL 426 SW6.5 | 48.1163 | 40.3561 | 47.301281 | 40.168804 | 56.822706 | 21.618937 | 150.02002462 | -14.98316021 | 88.4979 | 55803.0352314815 | 2011-08-30 00:50:44 | 55803.3008680556 | 2011-08-30 07:13:15 | 806109010 | 11.5806 | 10 | 11.5886 | 11.5806 | 0 | 11.5966 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.0679 | 7.0679 | 22.9359 | 0 | PROCESSED | 57603.0076041667 | 2016-08-03 00:10:57 | 55652 | 2011-04-01 00:00:00 | 55826.1781481482 | 2011-09-22 04:16:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806109010/ | Quick Look | ![]() |
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570 | ABELL 426 SE5.5 | 51.277 | 40.3868 | 50.453278 | 40.211126 | 59.315931 | 20.983376 | 152.07695425 | -13.63166747 | 96.5598 | 55799.6056828704 | 2011-08-26 14:32:11 | 55799.9189351852 | 2011-08-26 22:03:16 | 806119010 | 16.2703 | 15 | 16.2783 | 16.2703 | 0 | 16.2783 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.209 | 16.209 | 27.058 | 0 | PROCESSED | 57602.9656597222 | 2016-08-02 23:10:33 | 55652 | 2011-04-01 00:00:00 | 55865.074224537 | 2011-10-31 01:46:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806119010/ | Quick Look | ![]() |
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571 | ABELL 426 NE1 | 50.2177 | 41.6975 | 49.388255 | 41.517855 | 58.870415 | 22.461609 | 150.64118254 | -12.9960031 | 89.2472 | 55809.6259259259 | 2011-09-05 15:01:20 | 55809.8452662037 | 2011-09-05 20:17:11 | 806123010 | 10.9325 | 10 | 10.9325 | 10.9533 | 0 | 10.9405 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.2451 | 12.2451 | 18.9361 | 0 | PROCESSED | 57603.0729398148 | 2016-08-03 01:45:02 | 55652 | 2011-04-01 00:00:00 | 55866.0873842593 | 2011-11-01 02:05:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806123010/ | Quick Look | ![]() |
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572 | ABELL 426 NNE6.5 | 50.4676 | 43.2769 | 49.626686 | 43.098164 | 59.537818 | 23.928739 | 149.90216136 | -11.57929144 | 60.499 | 55807.5838194445 | 2011-09-03 14:00:42 | 55807.8391203704 | 2011-09-03 20:08:20 | 806145010 | 13.3332 | 10 | 13.3332 | 13.3332 | 0 | 13.3332 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.1621 | 14.1621 | 22.052 | 0 | PROCESSED | 57603.0507060185 | 2016-08-03 01:13:01 | 55652 | 2011-04-01 00:00:00 | 55845.2486226852 | 2011-10-11 05:58:01 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806145010/ | Quick Look | ![]() |
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573 | A2256BKG | 259.0594 | 79.1323 | 259.847378 | 79.183226 | 99.226233 | 77.073038 | 111.31764948 | 31.03227987 | 219.8044 | 56236.1893865741 | 2012-11-05 04:32:43 | 56237.0696875 | 2012-11-06 01:40:21 | 807025010 | 39.6865 | 40 | 39.6865 | 39.6865 | 0 | 39.6865 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.9304 | 48.9304 | 76.0479 | 0 | PROCESSED | 57607.9668634259 | 2016-08-07 23:12:17 | 56630 | 2013-12-04 00:00:00 | 56264.5702199074 | 2012-12-03 13:41:07 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070058 | We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MADOKA KAWAHARADA | JAP | 7 | AO7 | THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807025010/ | Quick Look | ![]() |
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574 | A1631_E | 193.4806 | -15.4427 | 192.82259 | -15.171579 | 198.410093 | -8.910855 | 303.81684947 | 47.4247798 | 113.0006 | 56305.0111226852 | 2013-01-13 00:16:01 | 56305.7231944445 | 2013-01-13 17:21:24 | 807005010 | 20.5236 | 20 | 20.5236 | 20.5236 | 0 | 20.5476 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.1111 | 20.1111 | 61.5119 | 1 | PROCESSED | 57608.4784143518 | 2016-08-08 11:28:55 | 56703 | 2014-02-15 00:00:00 | 56337.4913425926 | 2013-02-14 11:47:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807005010/ | Quick Look | ![]() |
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575 | NGC6946 | 308.6989 | 60.1968 | 308.436769 | 60.023263 | 358.020745 | 71.889708 | 95.74917907 | 11.70533663 | 79.9968 | 56060.7040393518 | 2012-05-13 16:53:49 | 56063.8903935185 | 2012-05-16 21:22:10 | 807035010 | 198.879 | 200 | 198.879 | 198.8958 | 0 | 198.8948 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 182.1955 | 182.1955 | 275.2756 | 3 | PROCESSED | 57605.4921296296 | 2016-08-05 11:48:40 | 56442 | 2013-05-30 00:00:00 | 56075.3809027778 | 2012-05-28 09:08:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070098 | Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. However, the origin of hot ISM is still unclear. We investigate the property of hot ISM according to luminosity of infrared emission, which is good tracer of star formation rate. If the hot ISM depend on the present activity of star formation, there are correlation between hot ISM and infrared emission. We propose the observation of the spiral galaxy NGC 6946. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SAORI KONAMI | JAP | 7 | AO7 | CLARIFICATION OF THE ORIGIN OF HOT ISM IN SPIRAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807035010/ | Quick Look | ![]() |
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576 | FILAMENT JUNCTION A | 165.6591 | 29.2454 | 164.978754 | 29.514668 | 155.086724 | 21.237285 | 201.46002358 | 65.98539565 | 289.5 | 56086.3001041667 | 2012-06-08 07:12:09 | 56088.1238425926 | 2012-06-10 02:58:20 | 807038010 | 69.1428 | 70 | 69.1588 | 69.1428 | 0 | 69.1588 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62.2992 | 62.2992 | 157.5558 | 1 | PROCESSED | 57605.6780787037 | 2016-08-05 16:16:26 | 56543 | 2013-09-08 00:00:00 | 56176.2765046296 | 2012-09-06 06:38:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070105 | We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NORIO SEKIYA | JAP | 7 | AO7 | EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807038010/ | Quick Look | ![]() |
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577 | FILAMENT JUNCTION B | 173.7402 | 21.0892 | 173.087159 | 21.365728 | 165.694635 | 16.835806 | 227.90630551 | 71.55824615 | 299.4979 | 56088.1275115741 | 2012-06-10 03:03:37 | 56089.3439814815 | 2012-06-11 08:15:20 | 807039010 | 50.1063 | 50 | 50.1189 | 50.1063 | 0 | 50.1269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.9818 | 40.9818 | 105.0959 | 0 | PROCESSED | 57605.6509375 | 2016-08-05 15:37:21 | 56543 | 2013-09-08 00:00:00 | 56176.2814236111 | 2012-09-06 06:45:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070105 | We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NORIO SEKIYA | JAP | 7 | AO7 | EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807039010/ | Quick Look | ![]() |
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578 | A262 NE1 | 28.4051 | 36.5019 | 27.66806 | 36.256213 | 39.720751 | 23.183318 | 136.64990456 | -24.70790073 | 250 | 56702.5986342593 | 2014-02-14 14:22:02 | 56703.187662037 | 2014-02-15 04:30:14 | 808108010 | 25.6102 | 24 | 25.6102 | 25.6102 | 0 | 25.6102 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8178472222 | 2016-08-13 19:37:42 | 57080 | 2015-02-27 00:00:00 | 56714.742037037 | 2014-02-26 17:48:32 | 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 | A | 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/ver3.0/808108010/ | Quick Look | ![]() |
579 | IC 5157 | 330.8663 | -34.934 | 330.129358 | -35.176355 | 320.316602 | -21.507496 | 10.02196464 | -53.45455848 | 251.1985 | 56250.3323611111 | 2012-11-19 07:58:36 | 56251.6043287037 | 2012-11-20 14:30:14 | 807048010 | 65.5411 | 150 | 65.5411 | 65.5411 | 0 | 65.5411 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 67.764 | 67.764 | 109.8861 | 1 | PROCESSED | 57608.0722222222 | 2016-08-08 01:44:00 | 56018 | 2012-04-01 00:00:00 | 56275.5333333333 | 2012-12-14 12:48:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAVID BUOTE | USA | 7 | AO7 | THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807048010/ | Quick Look | ![]() |
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580 | FG30 | 259.5133 | 56.677 | 259.289115 | 56.728173 | 238.479728 | 78.961901 | 84.88085465 | 35.08331599 | 38.7622 | 56049.4885532407 | 2012-05-02 11:43:31 | 56049.7980671296 | 2012-05-02 19:09:13 | 807051010 | 13.9787 | 10 | 13.9867 | 13.9947 | 0 | 13.9787 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.579 | 15.579 | 26.7259 | 0 | PROCESSED | 57605.3190856482 | 2016-08-05 07:39:29 | 56465 | 2013-06-22 00:00:00 | 56099.2218171296 | 2012-06-21 05:19:25 | 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/ver3.0/807051010/ | Quick Look | ![]() |
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581 | FG15 | 177.008 | 56.8964 | 176.342479 | 57.174256 | 146.620123 | 49.215769 | 139.35969999 | 58.16359998 | 300.5727 | 56073.7490856482 | 2012-05-26 17:58:41 | 56074.0586226852 | 2012-05-27 01:24:25 | 807057010 | 14.0757 | 15 | 14.0757 | 14.0757 | 0 | 14.0757 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.603 | 15.603 | 26.7399 | 1 | PROCESSED | 57605.5125578704 | 2016-08-05 12:18:05 | 56470 | 2013-06-27 00:00:00 | 56103.1467013889 | 2012-06-25 03:31:15 | 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/ver3.0/807057010/ | Quick Look | ![]() |
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582 | FG24 | 233.4334 | 3.6096 | 232.807042 | 3.776669 | 230.06319 | 22.123365 | 8.88650115 | 44.69822064 | 290.4245 | 56136.3403935185 | 2012-07-28 08:10:10 | 56136.7487152778 | 2012-07-28 17:58:09 | 807058010 | 15.8231 | 15 | 15.8231 | 15.8231 | 0 | 15.8231 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.191 | 13.191 | 35.2759 | 0 | PROCESSED | 57606.6653819444 | 2016-08-06 15:58:09 | 56527 | 2013-08-23 00:00:00 | 56161.2328240741 | 2012-08-22 05:35:16 | 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/ver3.0/807058010/ | Quick Look | ![]() |
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583 | RXJ1159+5531 | 179.9812 | 55.4402 | 179.338152 | 55.71852 | 149.981877 | 49.065325 | 137.66567163 | 60.1900448 | 115.1582 | 56268.8799768518 | 2012-12-07 21:07:10 | 56269.4140162037 | 2012-12-08 09:56:11 | 807064020 | 21.1432 | 20 | 21.1432 | 21.1512 | 0 | 21.1512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.6001 | 22.6001 | 46.14 | 0 | PROCESSED | 57608.2013310185 | 2016-08-08 04:49:55 | 56646 | 2013-12-20 00:00:00 | 56279.6625925926 | 2012-12-18 15:54:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071513 | With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | PHILIP HUMPHREY | USA | 7 | AO7 | RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807064020/ | Quick Look | ![]() |
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584 | RXJ1416.4+2315 | 214.0491 | 23.1704 | 213.474982 | 23.401811 | 202.508805 | 34.45187 | 25.95253376 | 70.44078356 | 293.1179 | 56125.9101736111 | 2012-07-17 21:50:39 | 56128.5008796296 | 2012-07-20 12:01:16 | 807065020 | 101.6938 | 100 | 101.7018 | 101.6938 | 0 | 101.7018 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.6763 | 99.6763 | 223.8209 | 2 | PROCESSED | 57606.7012037037 | 2016-08-06 16:49:44 | 56598 | 2013-11-02 00:00:00 | 56232.6190740741 | 2012-11-01 14:51:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071514 | Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID BUOTE | USA | 7 | AO7 | RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807065020/ | Quick Look | ![]() |
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585 | ANTLIA E3 | 158.6143 | -35.3303 | 158.046217 | -35.07153 | 176.766294 | -40.455458 | 273.75347644 | 19.66467309 | 278.5008 | 56093.5404166667 | 2012-06-15 12:58:12 | 56094.1877546296 | 2012-06-16 04:30:22 | 807068010 | 23.4861 | 23 | 23.5021 | 23.4861 | 0 | 23.5021 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.6862 | 20.6862 | 55.926 | 1 | PROCESSED | 57605.6943287037 | 2016-08-05 16:39:50 | 56476 | 2013-07-03 00:00:00 | 56110.5216550926 | 2012-07-02 12:31:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807068010/ | Quick Look | ![]() |
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586 | ABELL 665 | 127.933 | 65.6581 | 126.801514 | 65.827031 | 110.986153 | 44.956941 | 149.97935617 | 34.81341699 | 289.9968 | 56028.5599537037 | 2012-04-11 13:26:20 | 56029.4036226852 | 2012-04-12 09:41:13 | 807072040 | 52.791 | 50 | 52.791 | 52.799 | 0 | 52.799 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.6671 | 51.6671 | 72.8859 | 0 | PROCESSED | 57605.1597569444 | 2016-08-05 03:50:03 | 56018 | 2012-04-01 00:00:00 | 56044.1843518518 | 2012-04-27 04:25:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807072040/ | Quick Look | ![]() |
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587 | RCS110104-0351.3 | 165.266 | -3.8543 | 164.630074 | -3.585449 | 167.943149 | -9.357953 | 257.98650762 | 49.14106345 | 115.7008 | 56286.1353587963 | 2012-12-25 03:14:55 | 56287.8716898148 | 2012-12-26 20:55:14 | 807076010 | 76.1379 | 75 | 76.1539 | 76.1379 | 0 | 76.1539 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.4411 | 67.4411 | 150.0018 | 0 | PROCESSED | 57608.3704050926 | 2016-08-08 08:53:23 | 56690 | 2014-02-02 00:00:00 | 56324.5102314815 | 2013-02-01 12:14:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | 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 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807076010/ | Quick Look | ![]() |
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588 | SWCL J1403+3212 | 210.8847 | 32.2142 | 210.333728 | 32.453758 | 194.392634 | 41.437605 | 55.27159844 | 73.55798506 | 128.2493 | 56289.1009837963 | 2012-12-28 02:25:25 | 56290.2578587963 | 2012-12-29 06:11:19 | 807081010 | 52.1374 | 45 | 52.1374 | 52.143 | 0 | 52.1454 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.9868 | 42.9868 | 99.9358 | 0 | PROCESSED | 57608.4054050926 | 2016-08-08 09:43:47 | 56690 | 2014-02-02 00:00:00 | 56324.4837152778 | 2013-02-01 11:36:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071526 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the formation and evolution of the hot gaseous halos. The scaling relations and their deviations from self-similar model predictions due to non-gravitational processes are also important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z~0.6 galaxy clusters, selected from the Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such the X-ray luminosity and temperature. With this sample, we are able to model the selection functions relatively easily and place cleaner and tighter constraints on the evolution of X-ray properties of galaxy clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 7 | AO7 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807081010/ | Quick Look | ![]() |
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589 | HYDRA A FAR SE | 139.7 | -12.375 | 139.09881 | -12.163612 | 146.431142 | -26.609663 | 243.28582967 | 25.05625041 | 300 | 56082.6736342593 | 2012-06-04 16:10:02 | 56083.9368981482 | 2012-06-05 22:29:08 | 807088010 | 40.939 | 40 | 40.947 | 40.939 | 0 | 40.947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.9143 | 37.9143 | 109.1358 | 0 | PROCESSED | 57605.5894444444 | 2016-08-05 14:08:48 | 56464 | 2013-06-21 00:00:00 | 56096.2405208333 | 2012-06-18 05:46:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807088010/ | Quick Look | ![]() |
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590 | A2163BGD2 | 243.9063 | -6.5323 | 243.237281 | -6.40839 | 243.158854 | 14.509957 | 6.38161233 | 30.26602519 | 93.9997 | 57078.975787037 | 2015-02-25 23:25:08 | 57079.8335763889 | 2015-02-26 20:00:21 | 809011010 | 28.8166 | 30 | 28.8326 | 28.8166 | 0 | 28.8406 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6710763889 | 2016-08-17 16:06:21 | 57458 | 2016-03-11 00:00:00 | 57091.463587963 | 2015-03-10 11:07:34 | 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/ver3.0/809011010/ | Quick Look | ![]() |
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591 | G115.7+17.5 | 336.6801 | 78.3035 | 336.566813 | 78.048018 | 59.497327 | 68.492125 | 115.72297849 | 17.51053762 | 214.3075 | 56311.7506712963 | 2013-01-19 18:00:58 | 56313.7419328704 | 2013-01-21 17:48:23 | 807093010 | 97.8732 | 100 | 97.8892 | 97.8732 | 0 | 97.8892 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.3977 | 94.3977 | 172.0079 | 1 | PROCESSED | 57608.5818634259 | 2016-08-08 13:57:53 | 56708 | 2014-02-20 00:00:00 | 56342.5694097222 | 2013-02-19 13:39:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072021 | We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANNA SCAIFE | EUR | 7 | AO7 | CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807093010/ | Quick Look | ![]() |
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592 | VIRGO W6 | 186.0979 | 11.4464 | 185.462989 | 11.723363 | 180.971644 | 12.912849 | 279.57270772 | 73.07967034 | 99.9988 | 56274.3472685185 | 2012-12-13 08:20:04 | 56274.8098726852 | 2012-12-13 19:26:13 | 807099010 | 22.4217 | 19 | 22.4217 | 22.4217 | 0 | 22.4217 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.182 | 19.182 | 39.9499 | 1 | PROCESSED | 57608.269224537 | 2016-08-08 06:27:41 | 56018 | 2012-04-01 00:00:00 | 56342.6277893518 | 2013-02-19 15:04:01 | 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/ver3.0/807099010/ | Quick Look | ![]() |
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593 | VIRGO W11 | 184.734 | 10.623 | 184.097417 | 10.900554 | 180.060818 | 11.617697 | 276.51178499 | 71.80735655 | 99.9988 | 56276.9834143518 | 2012-12-15 23:36:07 | 56277.5397337963 | 2012-12-16 12:57:13 | 807104010 | 24.3087 | 24 | 24.3087 | 24.311 | 0 | 24.3127 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23.5095 | 23.5095 | 48.0381 | 0 | PROCESSED | 57608.2867361111 | 2016-08-08 06:52:54 | 56018 | 2012-04-01 00:00:00 | 56338.5029050926 | 2013-02-15 12:04:11 | 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/ver3.0/807104010/ | Quick Look | ![]() |
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594 | VIRGO N6 | 187.706 | 14.8589 | 187.074932 | 15.134961 | 181.007785 | 16.666841 | 280.53999282 | 76.82590701 | 310.9995 | 56104.4640740741 | 2012-06-26 11:08:16 | 56104.8946296296 | 2012-06-26 21:28:16 | 807111010 | 20.488 | 15 | 20.488 | 20.496 | 0 | 20.496 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.9025 | 19.9025 | 37.198 | 1 | PROCESSED | 57606.4880555556 | 2016-08-06 11:42:48 | 56018 | 2012-04-01 00:00:00 | 56117.9917361111 | 2012-07-09 23:48:06 | 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/ver3.0/807111010/ | Quick Look | ![]() |
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595 | VIRGO S2 | 187.7262 | 11.7827 | 187.093118 | 12.058753 | 182.329563 | 13.867553 | 284.50264567 | 73.91527115 | 308.5008 | 56111.5319791667 | 2012-07-03 12:46:03 | 56111.8286805556 | 2012-07-03 19:53:18 | 807116010 | 14.0408 | 10 | 14.0488 | 14.0408 | 0 | 14.0568 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.1631 | 13.1631 | 25.6319 | 0 | PROCESSED | 57606.5448611111 | 2016-08-06 13:04:36 | 56018 | 2012-04-01 00:00:00 | 56139.1771180556 | 2012-07-31 04:15:03 | 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/ver3.0/807116010/ | Quick Look | ![]() |
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596 | VIRGO S3 | 187.7051 | 11.4733 | 187.071794 | 11.749367 | 182.439346 | 13.576413 | 284.74763768 | 73.61284119 | 308.498 | 56111.8292013889 | 2012-07-03 19:54:03 | 56112.2224189815 | 2012-07-04 05:20:17 | 807117010 | 15.063 | 10 | 15.063 | 15.063 | 0 | 15.063 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.396 | 13.396 | 33.9619 | 0 | PROCESSED | 57606.5537384259 | 2016-08-06 13:17:23 | 56018 | 2012-04-01 00:00:00 | 56139.230787037 | 2012-07-31 05:32:20 | 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/ver3.0/807117010/ | Quick Look | ![]() |
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597 | VIRGO S9 | 187.5697 | 9.5888 | 186.935063 | 9.864954 | 183.095212 | 11.799058 | 286.04491696 | 71.76339412 | 306.8996 | 56115.2917361111 | 2012-07-07 07:00:06 | 56115.6641319444 | 2012-07-07 15:56:21 | 807123010 | 18.9179 | 14 | 18.9339 | 18.9179 | 0 | 18.9339 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.6185 | 18.6185 | 32.168 | 0 | PROCESSED | 57606.5741087963 | 2016-08-06 13:46:43 | 56018 | 2012-04-01 00:00:00 | 56142.0874884259 | 2012-08-03 02:05:59 | 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/ver3.0/807123010/ | Quick Look | ![]() |
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598 | VIRGO S14 | 187.4376 | 7.6823 | 186.801678 | 7.958538 | 183.753215 | 10.000828 | 287.13089499 | 69.88593318 | 122 | 56270.8466666667 | 2012-12-09 20:19:12 | 56271.2320717593 | 2012-12-10 05:34:11 | 807128010 | 15.4204 | 12 | 15.4364 | 15.4204 | 0 | 15.4444 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.7417 | 16.7417 | 33.2879 | 0 | PROCESSED | 57608.2246643518 | 2016-08-08 05:23:31 | 56018 | 2012-04-01 00:00:00 | 56291.692349537 | 2012-12-30 16:36:59 | 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/ver3.0/807128010/ | Quick Look | ![]() |
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599 | VIRGO S15 | 187.3986 | 7.3548 | 186.762452 | 7.631062 | 183.850325 | 9.685273 | 287.25281516 | 69.55887671 | 122.0016 | 56271.2325925926 | 2012-12-10 05:34:56 | 56271.6272106482 | 2012-12-10 15:03:11 | 807129010 | 18.2136 | 16 | 18.2296 | 18.2136 | 0 | 18.2296 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17.3218 | 17.3218 | 34.056 | 0 | PROCESSED | 57608.2302430556 | 2016-08-08 05:31:33 | 56018 | 2012-04-01 00:00:00 | 56291.7069328704 | 2012-12-30 16:57:59 | 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/ver3.0/807129010/ | Quick Look | ![]() |
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600 | A399EAST | 44.8284 | 12.9677 | 44.143216 | 12.769088 | 46.15453 | -3.865608 | 164.75111172 | -39.30361408 | 72.1818 | 56529.3727777778 | 2013-08-25 08:56:48 | 56530.5036921296 | 2013-08-26 12:05:19 | 808007010 | 50.2768 | 50 | 50.2928 | 50.2768 | 0 | 50.3008 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3039 | 46.3039 | 97.684 | 0 | PROCESSED | 57612.4010069444 | 2016-08-12 09:37:27 | 56956 | 2014-10-26 00:00:00 | 56587.522349537 | 2013-10-22 12:32:11 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHITAKA ISHISAKI | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808007010/ | Quick Look | ![]() |
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601 | COMA CLUSTER | 194.3893 | 26.9261 | 193.783242 | 27.196084 | 181.532075 | 30.236179 | 24.84225016 | 88.62234831 | 316.4746 | 55348.2119907407 | 2010-06-01 05:05:16 | 55350.6877199074 | 2010-06-03 16:30:19 | 805079010 | 101.7805 | 100 | 101.7805 | 101.7805 | 0 | 101.7805 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77.4308 | 77.4308 | 213.8639 | 1 | PROCESSED | 57553.0722685185 | 2016-06-14 01:44:04 | 55731 | 2011-06-19 00:00:00 | 55365.54125 | 2010-06-18 12:59:24 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051523 | The metal-enrichment mechanism of the hot gas in clusters of galaxies is still not completely understood, particularly at large (~virial) radii where current metallicity measurements are virtually non-existent. Yet a determinaton of elemental abundances of the gas at this radius will allow us to determine which enrichment mechanism (ram pressure stripping or galactic winds) is prevalant in the outskirts of clusters. We propose a 100 kec Suzaku observation of Coma at the virial radius to determine the Fe and S abundances at this location. The ratio of these two elements will allow us to discriminate among competing models for chemical enrichment. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JIMMY IRWIN | USA | 5 | AO5 | THE DETERMINATION OF THE METALLICITY OF COMA AT THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805079010/ | Quick Look | ![]() |
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602 | A1914_OFFSET3 | 216.2544 | 37.895 | 215.741562 | 38.120181 | 196.10746 | 48.514193 | 67.56094175 | 67.61680074 | 134.0009 | 55566.0223148148 | 2011-01-05 00:32:08 | 55566.4306365741 | 2011-01-05 10:20:07 | 805093020 | 12.8294 | 12 | 12.8294 | 12.8294 | 0 | 12.8294 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.721 | 13.721 | 35.2699 | 0 | PROCESSED | 57600.553599537 | 2016-07-31 13:17:11 | 55995 | 2012-03-09 00:00:00 | 55627.1328009259 | 2011-03-07 03:11:14 | 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 | 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/ver3.0/805093020/ | Quick Look | ![]() |
603 | A2744_NE | 3.7189 | -30.3078 | 3.087931 | -30.585769 | 350.157324 | -29.032997 | 9.14048559 | -81.37985976 | 233.5002 | 56616.3325694445 | 2013-11-20 07:58:54 | 56618.5994791667 | 2013-11-22 14:23:15 | 808008010 | 82.773 | 80 | 82.781 | 82.781 | 0 | 82.773 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71.7365 | 71.7365 | 195.8377 | 2 | PROCESSED | 57613.443900463 | 2016-08-13 10:39:13 | 56995 | 2014-12-04 00:00:00 | 56629.7456481482 | 2013-12-03 17:53:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080005 | We propose an additional 80ks pointing to complete our mapping of A2744 out to large radii and constrain the thermodynamical history of the cluster growth. A2744 is a multiple merger, nicknamed Pandora's cluster. Our analysis of existing Suzaku data suggest that this cluster has an anisotropic temperature structure near the virial radius and there is not a simple correlation between temperature and surface mass density of member galaxies. With proposed observations, we can determine, for the first time, the temperature and entropy profiles near the radio relic in the northeast and further test a scenario of gas heating and shock propagation in the cluster outskirts. Suzaku is most suited for this study because of the lowest background and excellent sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 8 | AO8 | REVEALING THE THERMODYNAMICAL EVOLUTION IN THE PANDORA'S CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808008010/ | Quick Look | ![]() |
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604 | COMA SUBHALO1 | 195.4003 | 29.028 | 194.800096 | 29.29674 | 181.356993 | 32.514724 | 73.80298118 | 87.06170231 | 296.7987 | 56451.3782638889 | 2013-06-08 09:04:42 | 56452.0681712963 | 2013-06-09 01:38:10 | 808018010 | 31.1826 | 30 | 31.1906 | 31.1826 | 0 | 31.1906 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.8197 | 28.8197 | 59.604 | 1 | PROCESSED | 57611.5003935185 | 2016-08-11 12:00:34 | 56869 | 2014-07-31 00:00:00 | 56503.6225462963 | 2013-07-30 14:56:28 | 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/ver3.0/808018010/ | Quick Look | ![]() |
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605 | ABELL 426 W7.5 | 47.1647 | 41.6449 | 46.344371 | 41.454202 | 56.483409 | 23.060639 | 148.68932505 | -14.26285782 | 94.0006 | 55431.5082175926 | 2010-08-23 12:11:50 | 55431.8251967593 | 2010-08-23 19:48:17 | 805117010 | 15.0656 | 15 | 15.0896 | 15.0656 | 0 | 15.0896 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.992 | 10.992 | 27.3839 | 0 | PROCESSED | 57553.174525463 | 2016-06-14 04:11:19 | 55287 | 2010-04-01 00:00:00 | 55446.2098263889 | 2010-09-07 05:02:09 | 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/ver3.0/805117010/ | Quick Look | ![]() |
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606 | A3627_NORTH | 243.656 | -60.6115 | 242.575411 | -60.485559 | 253.80029 | -38.641261 | 325.45745985 | -6.96421785 | 306.0001 | 56545.808912037 | 2013-09-10 19:24:50 | 56546.5556828704 | 2013-09-11 13:20:11 | 808058010 | 51.8996 | 50 | 51.9316 | 51.9236 | 0 | 51.8996 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43.0284 | 43.0284 | 64.5119 | 1 | PROCESSED | 57612.6119097222 | 2016-08-12 14:41:09 | 56956 | 2014-10-26 00:00:00 | 56588.8328935185 | 2013-10-23 19:59:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080097 | We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATSUHIRO HAYASHI | JAP | 8 | AO8 | OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808058010/ | Quick Look | ![]() |
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607 | MKW4-W2 | 181.7129 | 1.8545 | 181.072483 | 2.132812 | 180.830723 | 2.382546 | 278.14148217 | 62.56052834 | 136.8029 | 56652.6158217593 | 2013-12-26 14:46:47 | 56655.3919097222 | 2013-12-29 09:24:21 | 808065010 | 102.6011 | 100 | 102.6011 | 102.6011 | 0 | 102.6011 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.6977 | 88.6977 | 239.8258 | 1 | PROCESSED | 57613.7424421296 | 2016-08-13 17:49:07 | 57079 | 2015-02-26 00:00:00 | 56700.7408449074 | 2014-02-12 17:46:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUANYUAN SU | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808065010/ | Quick Look | ![]() |
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608 | A133_FIELD_1 | 15.9453 | -21.6335 | 15.33461 | -21.90164 | 5.595502 | -26.095488 | 150.67449532 | -83.82895318 | 231.9994 | 56645.5063078704 | 2013-12-19 12:09:05 | 56646.6683449074 | 2013-12-20 16:02:25 | 808081010 | 53.6483 | 50 | 53.6643 | 53.6483 | 0 | 53.6643 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.6512 | 52.6512 | 100.3879 | 1 | PROCESSED | 57613.6155439815 | 2016-08-13 14:46:23 | 57061 | 2015-02-08 00:00:00 | 56695.6487152778 | 2014-02-07 15:34:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808081010/ | Quick Look | ![]() |
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609 | COMA E2 | 195.5294 | 27.8966 | 194.927658 | 28.165178 | 182.080007 | 31.557077 | 51.52244118 | 87.51055859 | 279.9995 | 55729.2687268518 | 2011-06-17 06:26:58 | 55729.4890856482 | 2011-06-17 11:44:17 | 806031010 | 9.1256 | 10 | 9.1336 | 9.1256 | 0 | 9.1416 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.9108 | 8.9108 | 19.0319 | 0 | PROCESSED | 57602.3188194444 | 2016-08-02 07:39:06 | 55652 | 2011-04-01 00:00:00 | 55770.1098958333 | 2011-07-28 02:38:15 | 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/ver3.0/806031010/ | Quick Look | ![]() |
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610 | FORNAX CLUSTER NORTH | 54.7043 | -35.2294 | 54.224181 | -35.391259 | 39.001136 | -52.608154 | 236.34117402 | -53.57224789 | 244.9993 | 53749.1506134259 | 2006-01-14 03:36:53 | 53750.3265509259 | 2006-01-15 07:50:14 | 800002030 | 45.575 | 80 | 45.583 | 45.579 | 45.575 | 45.587 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42.5713 | 42.5713 | 101.6 | 1 | PROCESSED | 57532.6714236111 | 2016-05-24 16:06:51 | 54247 | 2007-05-27 00:00:00 | 54039.9702777778 | 2006-10-31 23:17:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002030/ | Quick Look | ![]() |
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611 | CIZASOUTHPE | 340.7756 | 52.9173 | 340.257126 | 52.654896 | 13.355059 | 54.189252 | 104.17197619 | -5.21572392 | 71.9989 | 56461.8747800926 | 2013-06-18 20:59:41 | 56464.2467361111 | 2013-06-21 05:55:18 | 808092010 | 92.9595 | 99 | 92.9675 | 92.9675 | 0 | 92.9595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96.3125 | 96.3125 | 204.9216 | 2 | PROCESSED | 57611.5762268518 | 2016-08-11 13:49:46 | 56848 | 2014-07-10 00:00:00 | 56481.818287037 | 2013-07-08 19:38:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081530 | The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REINOUT VAN WEEREN | USA | 8 | AO8 | SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808092010/ | Quick Look | ![]() |
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612 | PLCK G214.6-37.0 | 137.1752 | 14.6923 | 136.484307 | 14.895327 | 135.215425 | -1.654352 | 214.5759479 | 36.9399481 | 287 | 56413.2455439815 | 2013-05-01 05:53:35 | 56416.322349537 | 2013-05-04 07:44:11 | 808101010 | 119.2637 | 120 | 119.2637 | 119.2637 | 0 | 119.2637 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106.3127 | 106.3127 | 265.8039 | 5 | PROCESSED | 57611.2793981482 | 2016-08-11 06:42:20 | 56795 | 2014-05-18 00:00:00 | 56429.7933217593 | 2013-05-17 19:02:23 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082007 | We propose a detailed investigation of the nature of PLCK G214.6-37.0, discovered in the Planck survey. We aim at constraining the presence and properties of filamentary structures connecting and surrounding the clusters. We will unveil the overall dynamics of this complex structure and establish its detailed pressure distribution that can be used for a better estimation of YX to be compared with YSZ. Thus, we will perform a direct search for structures in between identified supercluster components from a careful comparison with the Planck results. Furthermore, the distribution of the PLCK G214.6-37.0 components suggest that it is evolving accreting sub-clusters along the filaments. That makes this supercluster one of the to search for the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LORENZO LOVISARI | EUR | 8 | AO8 | TRACKING DOWN THE PLANCK SUPERCLUSTER PLCK G214.6-37.0 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808101010/ | Quick Look | ![]() |
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613 | ABELL 3364 | 86.9739 | -32.0342 | 86.50731 | -32.050049 | 85.482586 | -55.428799 | 237.12200328 | -26.63960547 | 295.0051 | 55671.5944444444 | 2011-04-20 14:16:00 | 55672.2917939815 | 2011-04-21 07:00:11 | 806067040 | 31.8869 | 29.5 | 31.8949 | 31.8949 | 0 | 31.8869 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.6154 | 29.6154 | 60.2459 | 0 | PROCESSED | 57601.5617939815 | 2016-08-01 13:28:59 | 56067 | 2012-05-20 00:00:00 | 55692.2490277778 | 2011-05-11 05:58:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | 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 none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. 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 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067040/ | Quick Look | ![]() |
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614 | UGC03957 EAST | 115.9739 | 55.4967 | 114.966906 | 55.616404 | 107.333122 | 33.607468 | 162.19834712 | 29.35111138 | 294.9944 | 56008.1335648148 | 2012-03-22 03:12:20 | 56009.1717476852 | 2012-03-23 04:07:19 | 806094010 | 46.6221 | 45 | 46.6221 | 46.6221 | 0 | 46.6221 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45.2608 | 45.2608 | 89.6879 | 1 | PROCESSED | 57604.9930324074 | 2016-08-04 23:49:58 | 56434 | 2013-05-22 00:00:00 | 56068.628900463 | 2012-05-21 15:05:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BRENDA MIRANDA OCEJO | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806094010/ | Quick Look | ![]() |
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615 | A3528-S OFFSET 2 | 193.9782 | -29.6501 | 193.300361 | -29.379506 | 204.778966 | -21.736125 | 304.09397791 | 33.21155179 | 289.0026 | 56501.5292476852 | 2013-07-28 12:42:07 | 56502.3981481482 | 2013-07-29 09:33:20 | 808105010 | 42.3 | 40 | 42.3 | 42.3078 | 0 | 42.316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.5258 | 42.5258 | 75.0659 | 2 | PROCESSED | 57612.0639583333 | 2016-08-12 01:32:06 | 56955 | 2014-10-25 00:00:00 | 56587.7982523148 | 2013-10-22 19:09:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808105010/ | Quick Look | ![]() |
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616 | A2104S | 235.0317 | -3.4139 | 234.377731 | -3.253044 | 233.528717 | 15.709214 | 2.71321412 | 39.14413145 | 117.9978 | 54120.3324884259 | 2007-01-20 07:58:47 | 54120.8266087963 | 2007-01-20 19:50:19 | 801004010 | 17.3234 | 20 | 17.3234 | 17.3234 | 0 | 17.3234 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.8291 | 13.8291 | 42.6819 | 1 | PROCESSED | 57536.8854166667 | 2016-05-28 21:15:00 | 54750 | 2008-10-11 00:00:00 | 54137.3891898148 | 2007-02-06 09:20:26 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MAKOTO HATTORI | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801004010/ | Quick Look | ![]() |
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617 | IIZW108 | 318.5228 | 2.5728 | 317.890055 | 2.365228 | 321.781705 | 17.722745 | 53.56011975 | -29.86052353 | 77.7227 | 53864.5319791667 | 2006-05-09 12:46:03 | 53864.7883680556 | 2006-05-09 18:55:15 | 801075010 | 11.6052 | 11 | 11.6052 | 11.6052 | 11.6052 | 11.6052 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9.632 | 9.632 | 22.1499 | 1 | PROCESSED | 57534.2579398148 | 2016-05-26 06:11:26 | 54401 | 2007-10-28 00:00:00 | 53913.9958564815 | 2006-06-27 23:54:02 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | CALEB SCHARF | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801075010/ | Quick Look | ![]() |
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618 | ABELL 426 SE5 | 51.1493 | 40.4958 | 50.325207 | 40.319644 | 59.246759 | 21.114379 | 151.9309414 | -13.59719782 | 89.5614 | 55799.1762268518 | 2011-08-26 04:13:46 | 55799.6029861111 | 2011-08-26 14:28:18 | 806118010 | 16.4382 | 15 | 16.4462 | 16.4382 | 0 | 16.4538 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.2539 | 13.2539 | 36.8699 | 0 | PROCESSED | 57602.9664814815 | 2016-08-02 23:11:44 | 55652 | 2011-04-01 00:00:00 | 55855.1847685185 | 2011-10-21 04:26:04 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806118010/ | Quick Look | ![]() |
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619 | A3627SE | 243.9338 | -61.0124 | 242.844844 | -60.887647 | 254.085676 | -39.001294 | 325.27404641 | -7.34625911 | 86.273 | 54869.3739236111 | 2009-02-07 08:58:27 | 54870.87875 | 2009-02-08 21:05:24 | 803033010 | 52.6995 | 50 | 52.7395 | 52.6995 | 0 | 52.7235 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.1839 | 48.1839 | 129.9878 | 3 | PROCESSED | 57545.4958912037 | 2016-06-06 11:54:05 | 55330 | 2010-05-14 00:00:00 | 54881.3769212963 | 2009-02-19 09:02:46 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030117 | We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SHO NISHINO | JAP | 3 | AO3 | OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803033010/ | Quick Look | ![]() |
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620 | A1631_C | 193.2396 | -15.343 | 192.582019 | -15.071616 | 198.154189 | -8.910152 | 303.4747971 | 47.52714603 | 112.9996 | 56304.4910069444 | 2013-01-12 11:47:03 | 56305.0106944444 | 2013-01-13 00:15:24 | 807004010 | 23.8057 | 20 | 23.8137 | 23.8057 | 0 | 23.8057 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.9369 | 19.9369 | 44.8719 | 0 | PROCESSED | 57608.4757986111 | 2016-08-08 11:25:09 | 56704 | 2014-02-16 00:00:00 | 56337.5260300926 | 2013-02-14 12:37:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807004010/ | Quick Look | ![]() |
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621 | A548W | 86.2487 | -25.8437 | 85.742711 | -25.86316 | 84.832695 | -49.218426 | 230.35478522 | -25.32458233 | 240.9996 | 56337.0028819444 | 2013-02-14 00:04:09 | 56339.3300462963 | 2013-02-16 07:55:16 | 807033010 | 99.3707 | 100 | 99.3707 | 99.3707 | 0 | 99.3707 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 85.3446 | 85.3446 | 201.0437 | 2 | PROCESSED | 57610.6626041667 | 2016-08-10 15:54:09 | 56738 | 2014-03-22 00:00:00 | 56372.6069444445 | 2013-03-21 14:34:00 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070085 | Abell 548 west is a near-by (z=0.0424) poor cluster with an X-ray temperature of 3.4 keV. It has two bright radio relic emission located to the north (Feretti et al. 2006), and a candidate shock-front located near the relics (Solovyeva et al. 2008). The cluster X-ray luminosity is more than an order of magnitude dimmer when plotted in the kT-Lx relation. Combined with its too high galaxy velocity dispersion, we consider this target as a critical merger of two group-sized systems, which is a very rare case in our vicinity. Using Suzaku, we will parametrize the low surface brightness candidate shock region, to identify the temperature jump, which cannot be detected with XMM. We will also investigate the IC emission from the relics to measure the lower limit of its magnetic field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAZUHIRO NAKAZAWA | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A MERGING GROUP CANDIDATE ABELL 548 WEST | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807033010/ | Quick Look | ![]() |
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622 | VIRGO E7 | 189.7478 | 13.5221 | 189.118223 | 13.796711 | 183.461681 | 16.259141 | 290.25286309 | 76.08652265 | 285.0003 | 56483.2548842593 | 2013-07-10 06:07:02 | 56483.6994560185 | 2013-07-10 16:47:13 | 808122010 | 18.1665 | 17 | 18.1665 | 18.1905 | 0 | 18.1745 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.6917 | 15.6917 | 38.4039 | 2 | PROCESSED | 57611.7926273148 | 2016-08-11 19:01:23 | 56383 | 2013-04-01 00:00:00 | 56496.6013657407 | 2013-07-23 14:25:58 | 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/ver3.0/808122010/ | Quick Look | ![]() |
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623 | 3EGJ1234 1318_3 | 188.2697 | -13.5708 | 187.619846 | -13.295052 | 192.969415 | -9.186347 | 296.11455637 | 49.05777767 | 113.9119 | 54445.0609375 | 2007-12-11 01:27:45 | 54445.8543171296 | 2007-12-11 20:30:13 | 802004010 | 1.602 | 30 | 1.602 | 29.7794 | 0 | 29.7794 | 1 | 2 | 0 | 2 | 1 | 0 | 0 | 26.3048 | 26.3048 | 68.5198 | 0 | PROCESSED | 57637.5213888889 | 2016-09-06 12:30:48 | 54999 | 2009-06-17 00:00:00 | 54633.6933217593 | 2008-06-16 16:38:23 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020007 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOMONORI TOTANI | JAP | 2 | AO2 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802004010/ | Quick Look | ![]() |
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624 | 3EGJ1234 1318_4 | 188.5214 | -13.4715 | 187.871329 | -13.195924 | 193.15662 | -8.997759 | 296.47032219 | 49.18242085 | 113.9125 | 54445.8547453704 | 2007-12-11 20:30:50 | 54446.4655555556 | 2007-12-12 11:10:24 | 802005010 | 20.1392 | 20 | 0 | 20.1392 | 0 | 20.1552 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 20.0064 | 20.0064 | 52.7719 | 0 | PROCESSED | 57540.846875 | 2016-06-01 20:19:30 | 55000 | 2009-06-18 00:00:00 | 54633.6925347222 | 2008-06-16 16:37:15 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020007 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOMONORI TOTANI | JAP | 2 | AO2 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802005010/ | Quick Look | ![]() |
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625 | ABELL 262 OFFSET2 | 28.0598 | 36.4356 | 27.324082 | 36.18913 | 39.413922 | 23.227924 | 136.37355079 | -24.84408055 | 69.9996 | 54320.0778935185 | 2007-08-08 01:52:10 | 54321.2405555556 | 2007-08-09 05:46:24 | 802080010 | 54.7081 | 48 | 54.7241 | 54.7081 | 0 | 54.7241 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50.1788 | 50.1788 | 100.3968 | 1 | PROCESSED | 57539.4536226852 | 2016-05-31 10:53:13 | 54730 | 2008-09-21 00:00:00 | 54347.6730671296 | 2007-09-04 16:09:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023004 | 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 | Fabio Gastaldello | JUS | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802080010/ | Quick Look | ![]() |
626 | A3627CENTER | 243.5672 | -60.8499 | 242.482666 | -60.723566 | 253.815365 | -38.883288 | 325.25917104 | -7.10560665 | 129.9148 | 54905.9231597222 | 2009-03-15 22:09:21 | 54906.6072222222 | 2009-03-16 14:34:24 | 803032010 | 46.0339 | 50 | 46.0388 | 46.0419 | 0 | 46.0339 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43.3969 | 43.3969 | 59.0959 | 0 | PROCESSED | 57545.823900463 | 2016-06-06 19:46:25 | 55330 | 2010-05-14 00:00:00 | 54917.2613657407 | 2009-03-27 06:16:22 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030117 | We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SHO NISHINO | JAP | 3 | AO3 | OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803032010/ | Quick Look | ![]() |
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627 | A3112SE | 49.8254 | -44.4068 | 49.393169 | -44.587264 | 25.763903 | -59.224971 | 253.09009544 | -55.79916534 | 40.0009 | 56832.6869791667 | 2014-06-24 16:29:15 | 56834.034849537 | 2014-06-26 00:50:11 | 809026010 | 49.8443 | 45 | 49.8523 | 49.8443 | 0 | 49.8603 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.2246 | 44.2246 | 116.4418 | 0 | PROCESSED | 57615.347662037 | 2016-08-15 08:20:38 | 57212 | 2015-07-09 00:00:00 | 56846.5576273148 | 2014-07-08 13:22:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809026010/ | Quick Look | ![]() |
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628 | ZWCL 2341.1+0000 | 355.9117 | 0.3303 | 355.271077 | 0.05271 | 356.374003 | 1.928516 | 89.48591025 | -58.06988626 | 66.2761 | 54644.6873148148 | 2008-06-27 16:29:44 | 54645.9258912037 | 2008-06-28 22:13:17 | 803001010 | 50.7413 | 40 | 50.7493 | 50.7413 | 0 | 50.7573 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.4767 | 39.4767 | 107.0018 | 0 | PROCESSED | 57542.9355671296 | 2016-06-03 22:27:13 | 55021 | 2009-07-09 00:00:00 | 54655.1925578704 | 2008-07-08 04:37:17 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030002 | Recent advances in observational cosmology have revealed that the large-scale distribution of galaxies in the universe has a honeycomb-like structure. However it is still a mystery how such diverse structures emerge out of primeval density fluctuations that grew over time due to the effects of gravity. An important role in the structure-formation process is played by the large-scale shocks that form as the primordial density fluctuations become non-linear and the accretion flows on collapsing structures become supersonic. In order to understand cosmic-rays acceleration greater than 1000 TeV and the structure formation in the early universe, we propose a 40 ksec observation of the proto-cluster filament ZwCl 2341.1+0000 (z = 0.27) with Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JUN KATAOKA | JAP | 3 | AO3 | COSMIC-RAY ACCELERATION AND STRUCTURE FORMATION IN A MPC-SCALE FILAMENTARY NETWORK OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803001010/ | Quick Look | ![]() |
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629 | A3112N | 49.535 | -43.9764 | 49.09877 | -44.157944 | 25.831039 | -58.74808 | 252.47008016 | -56.12805661 | 40.0008 | 56831.1105439815 | 2014-06-23 02:39:11 | 56832.6863194444 | 2014-06-24 16:28:18 | 809027010 | 49.5323 | 45 | 49.5323 | 49.8923 | 0 | 49.8923 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.2405 | 44.2405 | 136.1356 | 2 | PROCESSED | 57615.3567476852 | 2016-08-15 08:33:43 | 57212 | 2015-07-09 00:00:00 | 56846.5678703704 | 2014-07-08 13:37:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809027010/ | Quick Look | ![]() |
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630 | PKS 0558-504 VIC 2 | 88.9376 | -50.5474 | 88.635341 | -50.553317 | 87.569877 | -73.980493 | 257.96524127 | -29.21937587 | 349.9999 | 56822.2473148148 | 2014-06-14 05:56:08 | 56824.093900463 | 2014-06-16 02:15:13 | 809035010 | 60.1523 | 60 | 60.1523 | 62.1728 | 0 | 62.1888 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.7476 | 56.7476 | 159.5318 | 2 | PROCESSED | 57615.2572800926 | 2016-08-15 06:10:29 | 57204 | 2015-07-01 00:00:00 | 56835.7714236111 | 2014-06-27 18:30:51 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090086 | We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAZUHIRO SAKAI | JAP | 9 | AO9 | IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809035010/ | Quick Look | ![]() |
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631 | VIRGO N7 | 187.7068 | 15.1871 | 187.075953 | 15.46316 | 180.867336 | 16.966208 | 280.02627988 | 77.13302603 | 311 | 56104.895150463 | 2012-06-26 21:29:01 | 56105.2924768518 | 2012-06-27 07:01:10 | 807112010 | 18.1828 | 16 | 18.1828 | 18.2059 | 0 | 18.1908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.604 | 16.604 | 34.3279 | 0 | PROCESSED | 57606.4965393518 | 2016-08-06 11:55:01 | 56018 | 2012-04-01 00:00:00 | 56117.9967013889 | 2012-07-09 23:55:15 | 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/ver3.0/807112010/ | Quick Look | ![]() |
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632 | RXCJ0234.5-5830 | 38.6494 | -58.5096 | 38.292773 | -58.727647 | 354.405777 | -65.806692 | 280.27566127 | -53.84414378 | 249.7915 | 55212.1975115741 | 2010-01-16 04:44:25 | 55212.4794328704 | 2010-01-16 11:30:23 | 804003010 | 13.5665 | 10 | 13.5745 | 13.5665 | 0 | 13.5825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7771 | 10.7771 | 24.3559 | 0 | PROCESSED | 57550.1603125 | 2016-06-11 03:50:51 | 55594 | 2011-02-02 00:00:00 | 55228.0359722222 | 2010-02-01 00:51:48 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804003010/ | Quick Look | ![]() |
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633 | NGC 6251 | 247.2266 | 82.6554 | 248.601394 | 82.760043 | 99.818913 | 73.103839 | 115.95247359 | 31.23340212 | 185.0319 | 55885.7751736111 | 2011-11-20 18:36:15 | 55887.7821875 | 2011-11-22 18:46:21 | 806015010 | 100.1571 | 100 | 100.1651 | 100.1571 | 0 | 100.1651 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98.5943 | 98.5943 | 173.3759 | 1 | PROCESSED | 57603.983599537 | 2016-08-03 23:36:23 | 56264 | 2012-12-03 00:00:00 | 55897.1810300926 | 2011-12-02 04:20:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060045 | Suzaku observations of lobes of Fanaroff-Riley Type-1 Radio Galaxies NGC 6251 and IC 4296 are proposed. Utilizing the high sensitivity for the diffuse sources of Suzaku, we propose precise measurement of the inverse-Compton X-rays form Fanaroff-Riley Type-1 Radio lobes to determine the electron energy density. Comparing the electron energy density with those of Fanaroff-Riley Type-2 Radio lobes, we examine an evolution model of the radio galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROMI SETA | JAP | 6 | AO6 | OBSERVATIONS OF LOBES OF FANAROFF-RILEY TYPE-1 RADIO GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806015010/ | Quick Look | ![]() |
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634 | A1674_NE | 196.3328 | 67.5805 | 195.880568 | 67.847887 | 143.656053 | 62.969177 | 120.89335151 | 49.49272287 | 327.6637 | 56799.3349189815 | 2014-05-22 08:02:17 | 56800.5487962963 | 2014-05-23 13:10:16 | 809042010 | 60.5303 | 40 | 0 | 60.5303 | 0 | 0 | 0 | 3 | 0 | 0 | 1 | 0 | 0 | 61.6512 | 61.6512 | 104.8597 | 2 | PROCESSED | 57615.1320023148 | 2016-08-15 03:10:05 | 57626 | 2016-08-26 00:00:00 | 56818.712650463 | 2014-06-10 17:06:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042010/ | Quick Look | ![]() |
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635 | NGC 5044 SOUTH 30' | 198.7482 | -16.8629 | 198.081082 | -16.598731 | 203.683963 | -8.265963 | 311.00467544 | 45.63931299 | 110.0008 | 55222.2581365741 | 2010-01-26 06:11:43 | 55224.0190277778 | 2010-01-28 00:27:24 | 804014010 | 65.1766 | 60 | 65.1846 | 65.1766 | 0 | 65.1846 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44.1628 | 44.1628 | 152.1218 | 1 | PROCESSED | 57550.4424768518 | 2016-06-11 10:37:10 | 55602 | 2011-02-10 00:00:00 | 55236.2169675926 | 2010-02-09 05:12:26 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040013 | Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KYOKO MATSUSHITA | JAP | 4 | AO4 | METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804014010/ | Quick Look | ![]() |
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636 | A1674_Center | 195.9709 | 67.5098 | 195.513873 | 67.777673 | 143.620899 | 62.81475 | 121.09709791 | 49.57408901 | 327.6687 | 56800.5493171296 | 2014-05-23 13:11:01 | 56801.6251736111 | 2014-05-24 15:00:15 | 809042020 | 56.0395 | 40 | 0 | 56.0395 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 56.0296 | 56.0296 | 92.9376 | 0 | PROCESSED | 57615.1546180556 | 2016-08-15 03:42:39 | 57626 | 2016-08-26 00:00:00 | 56862.7934837963 | 2014-07-24 19:02:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042020/ | Quick Look | ![]() |
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637 | CIZASOUTHPW | 340.5329 | 52.9469 | 340.016017 | 52.68489 | 13.195696 | 54.305912 | 104.05697228 | -5.12002469 | 72.9252 | 56464.2477662037 | 2013-06-21 05:56:47 | 56466.5627777778 | 2013-06-23 13:30:24 | 808093010 | 98.4207 | 99 | 98.4287 | 98.4207 | 0 | 98.4287 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99.1006 | 99.1006 | 200.0056 | 0 | PROCESSED | 57611.6015277778 | 2016-08-11 14:26:12 | 56848 | 2014-07-10 00:00:00 | 56481.8295486111 | 2013-07-08 19:54:33 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081530 | The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REINOUT VAN WEEREN | USA | 8 | AO8 | SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808093010/ | Quick Look | ![]() |
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638 | A1674_Offset | 196.9691 | 67.2995 | 196.521421 | 67.56601 | 144.467706 | 63.021341 | 120.47867852 | 49.75037622 | 328.362 | 56801.6258333333 | 2014-05-24 15:01:12 | 56802.7363541667 | 2014-05-25 17:40:21 | 809042030 | 67.4756 | 40 | 0 | 67.4756 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 63.4535 | 63.4535 | 95.9418 | 0 | PROCESSED | 57615.1567013889 | 2016-08-15 03:45:39 | 57626 | 2016-08-26 00:00:00 | 56818.7013541667 | 2014-06-10 16:49:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042030/ | Quick Look | ![]() |
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639 | A1674_SW | 195.6324 | 67.4673 | 195.171121 | 67.735617 | 143.543166 | 62.683089 | 121.29194244 | 49.62561755 | 325.0183 | 56802.7378472222 | 2014-05-25 17:42:30 | 56804.2224537037 | 2014-05-27 05:20:20 | 809042040 | 6.3772 | 40 | 6.3772 | 90.8498 | 0 | 6.3772 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 71.0768 | 71.0768 | 103.0788 | 1 | PROCESSED | 57615.185787037 | 2016-08-15 04:27:32 | 57626 | 2016-08-26 00:00:00 | 56818.7191203704 | 2014-06-10 17:15:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KIYOSHI HAYASHIDA | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809042040/ | Quick Look | ![]() |
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640 | COMA RADIO RELIC | 193.8629 | 27.2883 | 193.256096 | 27.558895 | 180.859214 | 30.350856 | 43.32885714 | 89.09337318 | 130.9989 | 54823.8794328704 | 2008-12-23 21:06:23 | 54829.0002777778 | 2008-12-29 00:00:24 | 803051010 | 205.062 | 140 | 205.07 | 205.07 | 0 | 205.062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 170.6222 | 170.6222 | 442.3917 | 3 | PROCESSED | 57545.2371412037 | 2016-06-06 05:41:29 | 55218 | 2010-01-22 00:00:00 | 54851.5095949074 | 2009-01-20 12:13:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031431 | We will observe the Coma cluster radio relic with the HXD/PIN to detect nonthermal Inverse Compton emission. This is the second brightest cluster radio relic known. The small PIN FOV will separate the Coma radio relic and halo. The PIN data will be a strong test of merger shock acceleration processes; a nondetection would be inconsistent with current theories. The data will allow the relic magnetic field, and nonthermal energy and pressure to be derived. The XIS observation of the relic will be used to detect the merger shock. The relic is associated with the merging NGC 4839 subgroup, which will also be observed. The 2 XIS observations will determine the dynamics of the merging subgroup. We will search for redshift differences between the Coma cluster, subgroup, and merger shock. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | CRAIG SARAZIN | USA | 3 | AO3 | HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO RELIC AND THE DYNAMICS OF THE MERGING SUBGROUP IN THE COMA CLUSTER | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803051010/ | Quick Look | ![]() |
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641 | FG23 | 232.4567 | 44.1429 | 232.030206 | 44.313314 | 209.251166 | 59.914107 | 71.72776372 | 54.06523853 | 150.3369 | 57007.3108101852 | 2014-12-16 07:27:34 | 57008.1494791667 | 2014-12-17 03:35:15 | 809058010 | 38.4415 | 40 | 38.4415 | 38.4415 | 0 | 38.4415 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5220601852 | 2016-08-17 12:31:46 | 57482 | 2016-04-04 00:00:00 | 57114.5765972222 | 2015-04-02 13:50:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ELENA D'ONGHIA | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809058010/ | Quick Look | ![]() |
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642 | THE MOON | 135.7323 | 11.3866 | 135.051985 | 11.584787 | 134.824104 | -5.224923 | 217.57839096 | 34.30376044 | 284.6998 | 56783.949849537 | 2014-05-06 22:47:47 | 56784.073125 | 2014-05-07 01:45:18 | 809001040 | 5.5556 | 45 | 5.5556 | 5.5714 | 0 | 5.5636 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.574 | 4.574 | 10.6479 | 0 | PROCESSED | 57615.0559606482 | 2016-08-15 01:20:35 | 57162 | 2015-05-20 00:00:00 | 56796.5928240741 | 2014-05-19 14:13:40 | 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/ver3.0/809001040/ | Quick Look | ![]() |
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643 | CENTAURUS SE4 | 192.8602 | -42.5262 | 192.164471 | -42.254349 | 210.265844 | -33.700282 | 302.93248329 | 20.34554874 | 294.0685 | 56854.4082407407 | 2014-07-16 09:47:52 | 56854.9480092593 | 2014-07-16 22:45:08 | 809068010 | 20.659 | 20 | 20.659 | 20.659 | 0 | 20.659 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.395 | 10.395 | 22.0319 | 0 | PROCESSED | 57615.3959606482 | 2016-08-15 09:30:11 | 57250 | 2015-08-16 00:00:00 | 56883.1729050926 | 2014-08-14 04:08:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091522 | We propose here to observe the outskirts of the X-ray bright, nearby Centaurus cluster with good azimuthal coverage by adding 3 new arms with total exposure 204ks. This will extend our initial analysis in one direction to the north-west which has allowed our team to obtain high spatial resolution profiles of temperature, density and entropy. The XMM temperature map of the central 30 arcmins shows a complex temperature environment and deviations from spherical symmetry, and good azimuthal coverage is important to obtain an accurate understanding of the outskirts.Observations of the Perseus cluster have shown significant azimuthal variations in the ICM temperature and entropy. Centaurus is the best target for understanding the ICM in the outskirts of a relaxed, intermediate mass cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | CHRISTOPHER REYNOLDS | USA | 9 | AO9 | OBSERVATIONS OF THE X-RAY BRIGHT, NEARBY CENTAURUS CLUSTER TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809068010/ | Quick Look | ![]() |
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644 | RCS1102-0319 | 165.6362 | -3.316 | 164.999495 | -3.046688 | 168.075129 | -8.718258 | 257.90567893 | 49.79184665 | 114.0911 | 54817.3259259259 | 2008-12-17 07:49:20 | 54817.9773611111 | 2008-12-17 23:27:24 | 803065010 | 26.3811 | 21 | 26.3811 | 26.3811 | 0 | 26.3811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.9089 | 13.9089 | 56.27 | 0 | PROCESSED | 57544.9757407407 | 2016-06-05 23:25:04 | 55206 | 2010-01-10 00:00:00 | 54840.2609143518 | 2009-01-09 06:15:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803065010/ | Quick Look | ![]() |
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645 | M87N FAINT | 187.6988 | 12.9392 | 187.066448 | 13.215269 | 181.818448 | 14.91295 | 283.11850774 | 75.01113844 | 297.6812 | 54625.626400463 | 2008-06-08 15:02:01 | 54627.068275463 | 2008-06-10 01:38:19 | 803069010 | 65.2474 | 60 | 65.2474 | 65.2714 | 0 | 65.2554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57.9068 | 57.9068 | 124.5638 | 0 | PROCESSED | 57542.7828587963 | 2016-06-03 18:47:19 | 55009 | 2009-06-27 00:00:00 | 54642.2950694444 | 2008-06-25 07:04:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032011 | We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AURORA SIMIONESCU | EUR | 3 | AO3 | THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803069010/ | Quick Look | ![]() |
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646 | THE MOON | 137.1548 | 11.8786 | 136.473781 | 12.081578 | 136.019585 | -4.350943 | 217.75615417 | 35.77416951 | 105.7184 | 56975.0809490741 | 2014-11-14 01:56:34 | 56975.1987615741 | 2014-11-14 04:46:13 | 809001190 | 6.413 | 45 | 6.413 | 6.413 | 0 | 6.413 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.77 | 2016-08-16 18:28:48 | 57358 | 2015-12-02 00:00:00 | 56992.4097916667 | 2014-12-01 09:50:06 | 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/ver3.0/809001190/ | Quick Look | ![]() |
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647 | RXCJ2157.4-0747 NE | 329.3742 | -7.8003 | 328.713545 | -8.039068 | 328.756448 | 4.373785 | 49.81973283 | -44.55901105 | 250.0004 | 56972.5422453704 | 2014-11-11 13:00:50 | 56973.0835069445 | 2014-11-12 02:00:15 | 809021010 | 18.63 | 20 | 18.646 | 18.63 | 0 | 18.646 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.764375 | 2016-08-16 18:20:42 | 57352 | 2015-11-26 00:00:00 | 56986.4078240741 | 2014-11-25 09:47:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809021010/ | Quick Look | ![]() |
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648 | ABELL 98-NORTH | 11.5751 | 20.8392 | 10.913914 | 20.566164 | 18.902329 | 14.584822 | 121.31617836 | -42.01643069 | 67.4405 | 56841.1634490741 | 2014-07-03 03:55:22 | 56841.958599537 | 2014-07-03 23:00:23 | 809078020 | 23.888 | 100 | 24.68 | 23.888 | 0 | 24.9396 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3618865741 | 2016-08-15 08:41:07 | 56748 | 2014-04-01 00:00:00 | 56875.6040393518 | 2014-08-06 14:29:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078020/ | Quick Look | ![]() |
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649 | A2029_2 | 227.8527 | 6.0108 | 227.233944 | 6.198717 | 223.562452 | 22.914786 | 6.92100367 | 50.6092725 | 112.9534 | 55224.3333912037 | 2010-01-28 08:00:05 | 55224.9794444444 | 2010-01-28 23:30:24 | 804024020 | 26.0185 | 22 | 26.0225 | 26.0185 | 0 | 26.0262 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.9033 | 15.9033 | 55.814 | 0 | PROCESSED | 57550.4048726852 | 2016-06-11 09:43:01 | 55637 | 2011-03-17 00:00:00 | 55271.0156365741 | 2010-03-16 00:22:31 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required 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 breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUZURU TAWARA | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804024020/ | Quick Look | ![]() |
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650 | A1246_CENTER | 170.9992 | 21.4865 | 170.340675 | 21.761183 | 163.096496 | 16.147963 | 224.00399917 | 69.32667171 | 120.0006 | 55151.2043981482 | 2009-11-16 04:54:20 | 55152.274525463 | 2009-11-17 06:35:19 | 804028010 | 48.4564 | 40 | 48.4724 | 48.4564 | 0 | 48.4724 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.2156 | 37.2156 | 92.4339 | 0 | PROCESSED | 57549.4081018518 | 2016-06-10 09:47:40 | 55531 | 2010-12-01 00:00:00 | 55162.1616319445 | 2009-11-27 03:52:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040053 | We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 4 | AO4 | MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804028010/ | Quick Look | ![]() |
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651 | FG34 | 359.5671 | 15.0896 | 358.927387 | 14.811234 | 5.724886 | 13.991032 | 104.34552863 | -45.85455759 | 250.6856 | 56999.6725115741 | 2014-12-08 16:08:25 | 57000.6669328704 | 2014-12-09 16:00:23 | 809060010 | 38.5062 | 40 | 38.5062 | 38.5062 | 0 | 38.5062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.0584 | 35.0584 | 85.8958 | 1 | PROCESSED | 57617.4968634259 | 2016-08-17 11:55:29 | 57377 | 2015-12-21 00:00:00 | 57010.1825925926 | 2014-12-19 04:22:56 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ELENA D'ONGHIA | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809060010/ | Quick Look | ![]() |
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652 | A1246_OFF | 171.128 | 21.4191 | 170.469781 | 21.693883 | 163.239064 | 16.135503 | 224.30142226 | 69.41574013 | 120.0005 | 55163.0212152778 | 2009-11-28 00:30:33 | 55164.9606365741 | 2009-11-29 23:03:19 | 804029010 | 80.3804 | 80 | 80.3964 | 80.3804 | 0 | 80.391 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55.158 | 55.158 | 167.5558 | 1 | PROCESSED | 57549.6578472222 | 2016-06-10 15:47:18 | 55549 | 2010-12-19 00:00:00 | 55181.239849537 | 2009-12-16 05:45:23 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040053 | We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 4 | AO4 | MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804029010/ | Quick Look | ![]() |
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653 | ABELL 2877 | 17.5065 | -45.9303 | 16.951425 | -46.196287 | 351.939456 | -47.942764 | 293.04607396 | -70.83949903 | 47.4208 | 56809.9110532407 | 2014-06-01 21:51:55 | 56810.1181712963 | 2014-06-02 02:50:10 | 809100010 | 11.908 | 10 | 11.916 | 11.908 | 0 | 11.9306 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1778240741 | 2016-08-15 04:16:04 | 57197 | 2015-06-24 00:00:00 | 56828.5915856482 | 2014-06-20 14:11:53 | 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 | B | 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/ver3.0/809100010/ | Quick Look | ![]() |
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654 | AWM7 45' EAST | 44.4244 | 41.5971 | 43.612656 | 41.396941 | 54.340636 | 23.633961 | 146.87973673 | -15.32937684 | 74.1373 | 55780.4446527778 | 2011-08-07 10:40:18 | 55781.3155208333 | 2011-08-08 07:34:21 | 806008010 | 36.8794 | 35 | 36.8794 | 36.8794 | 0 | 36.8794 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.7039 | 35.7039 | 75.2399 | 0 | PROCESSED | 57602.7523726852 | 2016-08-02 18:03:25 | 56169 | 2012-08-30 00:00:00 | 55802.4637384259 | 2011-08-29 11:07:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KYOKO MATSUSHITA | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806008010/ | Quick Look | ![]() |
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655 | ABELL 2667 | 357.8478 | -26.2362 | 357.201143 | -26.514394 | 347.004245 | -23.092849 | 33.32905605 | -76.56526922 | 64.8822 | 55724.4201273148 | 2011-06-12 10:04:59 | 55725.7009490741 | 2011-06-13 16:49:22 | 806029030 | 52.2862 | 50 | 52.3022 | 52.2862 | 0 | 52.3102 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42.9697 | 42.9697 | 110.6559 | 1 | PROCESSED | 57602.2711574074 | 2016-08-02 06:30:28 | 55652 | 2011-04-01 00:00:00 | 55757.6986458333 | 2011-07-15 16:46:03 | 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/ver3.0/806029030/ | Quick Look | ![]() |
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656 | COMA E3.5 | 195.93 | 27.9076 | 195.329276 | 28.17566 | 182.445576 | 31.726119 | 49.60850486 | 87.16763542 | 128.002 | 55917.6227314815 | 2011-12-22 14:56:44 | 55917.9487384259 | 2011-12-22 22:46:11 | 806032020 | 14.769 | 15 | 14.777 | 14.785 | 0 | 14.769 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.6169 | 9.6169 | 28.1599 | 1 | PROCESSED | 57604.2057175926 | 2016-08-04 04:56:14 | 55652 | 2011-04-01 00:00:00 | 55937.7819444444 | 2012-01-11 18:46:00 | 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/ver3.0/806032020/ | Quick Look | ![]() |
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657 | COMA E7 | 197.1143 | 27.885 | 196.516478 | 28.15145 | 183.559395 | 32.176347 | 45.24852034 | 86.15126123 | 280.0002 | 55732.0582291667 | 2011-06-20 01:23:51 | 55732.4446990741 | 2011-06-20 10:40:22 | 806038010 | 15.1175 | 15 | 15.1335 | 15.1175 | 0 | 15.1415 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.3295 | 16.3295 | 33.3039 | 0 | PROCESSED | 57602.3596643518 | 2016-08-02 08:37:55 | 55652 | 2011-04-01 00:00:00 | 55770.1779398148 | 2011-07-28 04:16:14 | 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/ver3.0/806038010/ | Quick Look | ![]() |
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658 | COMA NW1 | 194.8094 | 28.1686 | 194.206284 | 28.438076 | 181.270608 | 31.513632 | 64.44263169 | 87.98368038 | 319.9994 | 55732.4516550926 | 2011-06-20 10:50:23 | 55732.6453935185 | 2011-06-20 15:29:22 | 806039010 | 9.633 | 10 | 9.633 | 9.633 | 0 | 9.633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.038 | 8.038 | 16.7279 | 0 | PROCESSED | 57602.3588310185 | 2016-08-02 08:36:43 | 55652 | 2011-04-01 00:00:00 | 55768.2335416667 | 2011-07-26 05:36:18 | 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/ver3.0/806039010/ | Quick Look | ![]() |
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659 | COMA NW5.5 | 194.2342 | 29.281 | 193.631324 | 29.551161 | 180.146914 | 32.276161 | 93.88493667 | 87.52983745 | 319.9944 | 55734.0685763889 | 2011-06-22 01:38:45 | 55734.4155439815 | 2011-06-22 09:58:23 | 806043010 | 15.6631 | 15 | 15.6631 | 15.6631 | 0 | 15.6631 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.384 | 16.384 | 29.9559 | 1 | PROCESSED | 57602.3741203704 | 2016-08-02 08:58:44 | 55652 | 2011-04-01 00:00:00 | 55768.2836458333 | 2011-07-26 06:48:27 | 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/ver3.0/806043010/ | Quick Look | ![]() |
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660 | SPT-CL J2337-5942 | 354.3472 | -59.706 | 353.656399 | -59.982964 | 322.211454 | -50.57498 | 319.15808948 | -55.0279039 | 35.9387 | 55674.1154282407 | 2011-04-23 02:46:13 | 55674.9342592593 | 2011-04-23 22:25:20 | 806073010 | 38.8415 | 35 | 38.8415 | 38.8415 | 0 | 38.8415 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.8423 | 33.8423 | 70.74 | 0 | PROCESSED | 57601.5793402778 | 2016-08-01 13:54:15 | 56067 | 2012-05-20 00:00:00 | 55692.2710069445 | 2011-05-11 06:30:15 | 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/ver3.0/806073010/ | Quick Look | ![]() |
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661 | ABELL 3364 | 86.8402 | -31.7251 | 86.371508 | -31.741602 | 85.303796 | -55.115651 | 236.7542178 | -26.65907095 | 295.0034 | 55669.7134722222 | 2011-04-18 17:07:24 | 55670.3585416667 | 2011-04-19 08:36:18 | 806067010 | 30.0737 | 29.5 | 30.0897 | 30.0737 | 0 | 30.0897 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.5437 | 28.5437 | 55.7279 | 1 | PROCESSED | 57601.535787037 | 2016-08-01 12:51:32 | 56067 | 2012-05-20 00:00:00 | 55691.1662962963 | 2011-05-10 03:59:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | 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 none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. 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 | A | KA-WAH WONG | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806067010/ | Quick Look | ![]() |
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662 | SPT-CL J0546-5345 | 86.64 | -53.7518 | 86.378624 | -53.768776 | 81.098351 | -77.090454 | 261.46331102 | -30.97881567 | 53.9016 | 55781.3261805556 | 2011-08-08 07:49:42 | 55782.8335763889 | 2011-08-09 20:00:21 | 806071010 | 99.7366 | 110 | 99.7366 | 99.7366 | 0 | 99.7366 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78.9114 | 78.9114 | 130.2079 | 3 | PROCESSED | 57602.7921180556 | 2016-08-02 19:00:39 | 56169 | 2012-08-30 00:00:00 | 55802.4644907407 | 2011-08-29 11:08:52 | 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/ver3.0/806071010/ | Quick Look | ![]() |
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663 | A1750N | 202.8147 | -1.6537 | 202.171177 | -1.396479 | 201.71761 | 7.336429 | 322.93839507 | 59.66232121 | 293.5219 | 55744.8544444444 | 2011-07-02 20:30:24 | 55746.9911111111 | 2011-07-04 23:47:12 | 806096010 | 74.7134 | 80 | 74.7294 | 74.7134 | 0 | 74.7294 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61.6402 | 61.6402 | 184.5979 | 1 | PROCESSED | 57602.5091435185 | 2016-08-02 12:13:10 | 56144 | 2012-08-05 00:00:00 | 55775.4134027778 | 2011-08-02 09:55:18 | 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/ver3.0/806096010/ | Quick Look | ![]() |
664 | A2199 OFFSET8 | 247.7871 | 40.0108 | 247.362763 | 40.116965 | 233.730787 | 60.681855 | 63.58609445 | 43.22438175 | 270.3665 | 55796.7271180556 | 2011-08-23 17:27:03 | 55797.4578703704 | 2011-08-24 10:59:20 | 806154010 | 30.7084 | 30 | 30.7084 | 30.7084 | 0 | 30.7084 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.6487 | 25.6487 | 63.134 | 2 | PROCESSED | 57602.9315046296 | 2016-08-02 22:21:22 | 55652 | 2011-04-01 00:00:00 | 55806.3170138889 | 2011-09-02 07:36:30 | 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/ver3.0/806154010/ | Quick Look | ![]() |
665 | ABELL 426 SE6 | 51.3915 | 40.2857 | 50.568134 | 40.110458 | 59.377203 | 20.862689 | 152.21004388 | -13.66501615 | 96.5621 | 55799.9192708333 | 2011-08-26 22:03:45 | 55800.1515856482 | 2011-08-27 03:38:17 | 806120010 | 10.1455 | 10 | 10.1455 | 10.1695 | 0 | 10.1535 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.8587 | 8.8587 | 20.0639 | 0 | PROCESSED | 57602.969212963 | 2016-08-02 23:15:40 | 55652 | 2011-04-01 00:00:00 | 55865.0772569444 | 2011-10-31 01:51:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806120010/ | Quick Look | ![]() |
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666 | ABELL 426 NE2 | 50.5182 | 41.8628 | 49.686815 | 41.684269 | 59.152818 | 22.559001 | 150.73800989 | -12.73403508 | 89.4986 | 55808.6745949074 | 2011-09-04 16:11:25 | 55808.8752314815 | 2011-09-04 21:00:20 | 806124010 | 10.2106 | 10 | 10.2426 | 10.2346 | 0 | 10.2106 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.6835 | 11.6835 | 17.3279 | 0 | PROCESSED | 57603.0596412037 | 2016-08-03 01:25:53 | 55652 | 2011-04-01 00:00:00 | 55865.9664467593 | 2011-10-31 23:11:41 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806124010/ | Quick Look | ![]() |
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667 | ABELL 426 NE3 | 50.8162 | 42.0347 | 49.982827 | 41.857279 | 59.43466 | 22.663828 | 150.82784183 | -12.4676031 | 89.4977 | 55809.0721412037 | 2011-09-05 01:43:53 | 55809.4029513889 | 2011-09-05 09:40:15 | 806126010 | 10.5666 | 10 | 10.5666 | 10.5906 | 0 | 10.5746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.704 | 10.704 | 28.5759 | 0 | PROCESSED | 57603.0680902778 | 2016-08-03 01:38:03 | 55652 | 2011-04-01 00:00:00 | 55866.0158333333 | 2011-11-01 00:22:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806126010/ | Quick Look | ![]() |
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668 | ABELL 426 NE7 | 52.033 | 42.7019 | 51.191639 | 42.529059 | 60.569296 | 23.064384 | 151.19797458 | -11.40826829 | 89.5003 | 55811.3970486111 | 2011-09-07 09:31:45 | 55811.6487384259 | 2011-09-07 15:34:11 | 806134010 | 11.079 | 10 | 11.0908 | 11.087 | 0 | 11.079 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10.7886 | 10.7886 | 21.7361 | 0 | PROCESSED | 57603.0933449074 | 2016-08-03 02:14:25 | 55652 | 2011-04-01 00:00:00 | 55868.9251967593 | 2011-11-03 22:12:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806134010/ | Quick Look | ![]() |
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669 | ABELL 426 NNE2 | 50.087 | 42.0498 | 49.255577 | 41.869667 | 58.874503 | 22.827107 | 150.35811431 | -12.75634017 | 60.4956 | 55804.0547916667 | 2011-08-31 01:18:54 | 55804.3098726852 | 2011-08-31 07:26:13 | 806136010 | 10.686 | 10 | 10.686 | 10.686 | 0 | 10.686 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.899 | 6.899 | 22.0319 | 1 | PROCESSED | 57603.0180208333 | 2016-08-03 00:25:57 | 55652 | 2011-04-01 00:00:00 | 55830.1908333333 | 2011-09-26 04:34:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806136010/ | Quick Look | ![]() |
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670 | ABELL 426 NNE3 | 50.1707 | 42.3226 | 49.337205 | 42.142774 | 59.021278 | 23.072073 | 150.2566965 | -12.4946686 | 60.4975 | 55804.5824189815 | 2011-08-31 13:58:41 | 55804.7849768518 | 2011-08-31 18:50:22 | 806138010 | 9.859 | 10 | 9.859 | 9.859 | 0 | 9.859 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10.125 | 10.125 | 17.4719 | 0 | PROCESSED | 57603.0234606482 | 2016-08-03 00:33:47 | 55652 | 2011-04-01 00:00:00 | 55871.8708680556 | 2011-11-06 20:54:03 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806138010/ | Quick Look | ![]() |
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671 | NGC 7796 | 359.7407 | -55.4558 | 359.095869 | -55.734273 | 329.790591 | -49.001607 | 317.90399943 | -60.12089491 | 60.4505 | 56078.2927430556 | 2012-05-31 07:01:33 | 56080.5001851852 | 2012-06-02 12:00:16 | 807047010 | 161.6136 | 150 | 161.6216 | 161.6216 | 0 | 161.6136 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134.0432 | 134.0432 | 190.7118 | 0 | PROCESSED | 57605.6269328704 | 2016-08-05 15:02:47 | 56018 | 2012-04-01 00:00:00 | 56090.2424537037 | 2012-06-12 05:49:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAVID BUOTE | USA | 7 | AO7 | THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807047010/ | Quick Look | ![]() |
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672 | A3376 EAST | 90.8243 | -39.9606 | 90.417011 | -39.957602 | 91.41993 | -63.398251 | 246.56739968 | -25.79165375 | 80.8001 | 56549.3239699074 | 2013-09-14 07:46:31 | 56551.6953472222 | 2013-09-16 16:41:18 | 808028010 | 81.5734 | 81 | 81.5734 | 81.5734 | 0 | 81.5734 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75.1814 | 75.1814 | 204.8578 | 2 | PROCESSED | 57612.6739467593 | 2016-08-12 16:10:29 | 56956 | 2014-10-26 00:00:00 | 56588.6883449074 | 2013-10-23 16:31:13 | 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/ver3.0/808028010/ | Quick Look | ![]() |
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673 | FG27 | 243.6269 | 26.7212 | 243.111772 | 26.845958 | 234.444811 | 46.957031 | 44.57695273 | 45.05698279 | 293.3995 | 56144.3018055556 | 2012-08-05 07:14:36 | 56144.5557638889 | 2012-08-05 13:20:18 | 807056010 | 11.2194 | 15 | 11.235 | 11.2194 | 0 | 11.235 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.9114 | 10.9114 | 21.9359 | 1 | PROCESSED | 57606.7546643518 | 2016-08-06 18:06:43 | 56533 | 2013-08-29 00:00:00 | 56167.1527893518 | 2012-08-28 03:40:01 | 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/ver3.0/807056010/ | Quick Look | ![]() |
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674 | SDSS J0837+4414 | 129.4975 | 44.2566 | 128.645697 | 44.432041 | 120.139652 | 24.860483 | 176.37698799 | 37.1577345 | 110.1912 | 56213.8277083333 | 2012-10-13 19:51:54 | 56214.3515393518 | 2012-10-14 08:26:13 | 807061010 | 20.6219 | 20 | 20.6219 | 20.6219 | 0 | 20.6219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.958 | 20.958 | 45.2399 | 0 | PROCESSED | 57607.7583796296 | 2016-08-07 18:12:04 | 56598 | 2013-11-02 00:00:00 | 56232.4985185185 | 2012-11-01 11:57:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807061010/ | Quick Look | ![]() |
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675 | HYDRA A OUT | 139.8502 | -12.6235 | 139.249709 | -12.411636 | 146.680072 | -26.793484 | 243.60142222 | 25.01758475 | 300.0034 | 56085.1461574074 | 2012-06-07 03:30:28 | 56085.6667824074 | 2012-06-07 16:00:10 | 807091010 | 20.3276 | 20 | 20.3516 | 20.3436 | 0 | 20.3276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16.5403 | 16.5403 | 44.9779 | 0 | PROCESSED | 57605.607349537 | 2016-08-05 14:34:35 | 56491 | 2013-07-18 00:00:00 | 56120.2321296296 | 2012-07-12 05:34:16 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807091010/ | Quick Look | ![]() |
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676 | G171.9-40.7 | 48.2433 | 8.3685 | 47.57264 | 8.181881 | 48.126521 | -9.211403 | 171.97024112 | -40.65556769 | 252.8031 | 56320.012025463 | 2013-01-28 00:17:19 | 56322.7126967593 | 2013-01-30 17:06:17 | 807092010 | 100.9825 | 100 | 100.9905 | 100.9825 | 0 | 100.9848 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93.1617 | 93.1617 | 233.2957 | 0 | PROCESSED | 57608.6871527778 | 2016-08-08 16:29:30 | 56749 | 2014-04-02 00:00:00 | 56365.6023263889 | 2013-03-14 14:27:21 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072021 | We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ANNA SCAIFE | EUR | 7 | AO7 | CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807092010/ | Quick Look | ![]() |
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677 | VIRGO W1 | 187.5107 | 12.2426 | 186.877692 | 12.518786 | 181.938422 | 14.202058 | 283.26919479 | 74.29186005 | 291.9999 | 56110.6712847222 | 2012-07-02 16:06:39 | 56110.9370138889 | 2012-07-02 22:29:18 | 807094010 | 12.7859 | 10 | 12.7939 | 12.7939 | 0 | 12.7859 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.5429 | 10.5429 | 22.9519 | 0 | PROCESSED | 57606.5451157407 | 2016-08-06 13:04:58 | 56018 | 2012-04-01 00:00:00 | 56127.137662037 | 2012-07-19 03:18:14 | 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/ver3.0/807094010/ | Quick Look | ![]() |
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678 | VIRGO W7 | 185.8245 | 11.2655 | 185.18923 | 11.542594 | 180.795697 | 12.638786 | 278.94638045 | 72.81351487 | 99.9999 | 56274.8104398148 | 2012-12-13 19:27:02 | 56275.3217013889 | 2012-12-14 07:43:15 | 807100010 | 23.4449 | 20 | 23.4529 | 23.4529 | 0 | 23.4449 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.0353 | 25.0353 | 44.1699 | 0 | PROCESSED | 57608.2724652778 | 2016-08-08 06:32:21 | 56018 | 2012-04-01 00:00:00 | 56338.5069560185 | 2013-02-15 12:10:01 | 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/ver3.0/807100010/ | Quick Look | ![]() |
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679 | VIRGO W8 | 185.551 | 11.0911 | 184.915383 | 11.368319 | 180.616918 | 12.370601 | 278.32881118 | 72.55156974 | 99.4998 | 56275.3224074074 | 2012-12-14 07:44:16 | 56275.8078240741 | 2012-12-14 19:23:16 | 807101010 | 22.1703 | 21 | 22.1783 | 22.1703 | 0 | 22.1863 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8585 | 18.8585 | 41.918 | 0 | PROCESSED | 57608.2782291667 | 2016-08-08 06:40:39 | 56018 | 2012-04-01 00:00:00 | 56315.5145023148 | 2013-01-23 12:20:53 | 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/ver3.0/807101010/ | Quick Look | ![]() |
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680 | VIRGO N1 | 187.7027 | 13.2607 | 187.070564 | 13.536766 | 181.686135 | 15.207962 | 282.74012713 | 75.31771863 | 314.0012 | 56097.8290740741 | 2012-06-19 19:53:52 | 56098.0419328704 | 2012-06-20 01:00:23 | 807106010 | 9.9319 | 10 | 9.9319 | 9.9399 | 0 | 9.9399 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.542 | 9.542 | 18.3839 | 0 | PROCESSED | 57605.7042592593 | 2016-08-05 16:54:08 | 56018 | 2012-04-01 00:00:00 | 56225.4789699074 | 2012-10-25 11:29:43 | 3.0.22.44 | 4 | 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/ver3.0/807106010/ | Quick Look | ![]() |
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681 | VIRGO N2 | 187.703 | 13.5671 | 187.071067 | 13.843165 | 181.556537 | 15.487683 | 282.35217615 | 75.60823465 | 313.9984 | 56098.0424074074 | 2012-06-20 01:01:04 | 56098.2606828704 | 2012-06-20 06:15:23 | 807107010 | 10.7068 | 10 | 10.7068 | 10.7308 | 0 | 10.7148 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.659 | 8.659 | 18.848 | 1 | PROCESSED | 57605.7127777778 | 2016-08-05 17:06:24 | 56018 | 2012-04-01 00:00:00 | 56214.9560763889 | 2012-10-14 22:56:45 | 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/ver3.0/807107010/ | Quick Look | ![]() |
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682 | A2199_NE | 247.516 | 39.7841 | 247.089512 | 39.891486 | 233.470249 | 60.402163 | 63.26645529 | 43.42583068 | 143.5992 | 56661.6024074074 | 2014-01-04 14:27:28 | 56662.5572222222 | 2014-01-05 13:22:24 | 808050010 | 44.1631 | 40 | 44.1711 | 44.1631 | 0 | 44.1711 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.3531 | 42.3531 | 82.4919 | 1 | PROCESSED | 57613.7484953704 | 2016-08-13 17:57:50 | 57079 | 2015-02-26 00:00:00 | 56713.7287037037 | 2014-02-25 17:29:20 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080067 | We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KOSUKE SATO | JAP | 8 | AO8 | COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808050010/ | Quick Look | ![]() |
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683 | VIRGO N8 | 187.7075 | 15.4944 | 187.076861 | 15.770459 | 180.735378 | 17.246403 | 279.52276063 | 77.41962086 | 310.9997 | 56105.2930439815 | 2012-06-27 07:01:59 | 56105.7028703704 | 2012-06-27 16:52:08 | 807113010 | 18.7018 | 18 | 18.7057 | 18.7018 | 0 | 18.7097 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.7504 | 18.7504 | 35.4 | 0 | PROCESSED | 57606.4979050926 | 2016-08-06 11:56:59 | 56018 | 2012-04-01 00:00:00 | 56118.0144097222 | 2012-07-10 00:20:45 | 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/ver3.0/807113010/ | Quick Look | ![]() |
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684 | VIRGO N9 | 187.7056 | 15.8164 | 187.075176 | 16.092459 | 180.594255 | 17.538861 | 278.95935226 | 77.71791573 | 310.4995 | 56106.6618171296 | 2012-06-28 15:53:01 | 56107.1398611111 | 2012-06-29 03:21:24 | 807114010 | 22.9788 | 19 | 22.9788 | 23.0059 | 0 | 22.9788 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20.6819 | 20.6819 | 41.2959 | 1 | PROCESSED | 57606.5125578704 | 2016-08-06 12:18:05 | 56018 | 2012-04-01 00:00:00 | 56118.0912037037 | 2012-07-10 02:11:20 | 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/ver3.0/807114010/ | Quick Look | ![]() |
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685 | VIRGO S6 | 187.6479 | 10.5513 | 187.013944 | 10.827404 | 182.769907 | 12.710704 | 285.44540552 | 72.71150131 | 308.4999 | 56112.7686574074 | 2012-07-04 18:26:52 | 56113.0799421296 | 2012-07-05 01:55:07 | 807120010 | 12.7014 | 10 | 12.7014 | 12.7014 | 0 | 12.7014 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.5005 | 10.5005 | 26.8879 | 1 | PROCESSED | 57606.5642361111 | 2016-08-06 13:32:30 | 56018 | 2012-04-01 00:00:00 | 56141.2151388889 | 2012-08-02 05:09:48 | 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/ver3.0/807120010/ | Quick Look | ![]() |
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686 | VIRGO S10 | 187.554 | 9.2735 | 186.919151 | 9.549665 | 183.210349 | 11.504238 | 286.25782629 | 71.4549429 | 121.999 | 56269.421712963 | 2012-12-08 10:07:16 | 56269.7570717593 | 2012-12-08 18:10:11 | 807124010 | 16.098 | 16 | 16.098 | 16.098 | 0 | 16.098 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.413 | 13.413 | 28.952 | 0 | PROCESSED | 57608.2049074074 | 2016-08-08 04:55:04 | 56018 | 2012-04-01 00:00:00 | 56336.4667824074 | 2013-02-13 11:12:10 | 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/ver3.0/807124010/ | Quick Look | ![]() |
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687 | ABELL 85 S2 | 10.6249 | -9.681 | 9.992851 | -9.954936 | 5.880188 | -13.097469 | 115.61862408 | -72.42570917 | 230.5003 | 56295.6322106482 | 2013-01-03 15:10:23 | 56296.8696064815 | 2013-01-04 20:52:14 | 807136010 | 53.603 | 50 | 53.611 | 53.611 | 0 | 53.603 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.8426 | 51.8426 | 106.8957 | 2 | PROCESSED | 57608.4325347222 | 2016-08-08 10:22:51 | 56702 | 2014-02-14 00:00:00 | 56336.5803240741 | 2013-02-13 13:55:40 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071791 | We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | STEVEN ALLEN | USA | 7 | AO7 | TRACING A MERGER FROM START TO FINISH IN ABELL 85 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807136010/ | Quick Look | ![]() |
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688 | SHAPLEY B | 201.6375 | -31.8605 | 200.934316 | -31.601045 | 212.201419 | -21.080247 | 311.5766773 | 30.42117615 | 110.7883 | 56315.4877893518 | 2013-01-23 11:42:25 | 56316.3245138889 | 2013-01-24 07:47:18 | 807137010 | 30.5052 | 30 | 30.5132 | 30.5052 | 0 | 30.5203 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26.1395 | 26.1395 | 72.2919 | 2 | PROCESSED | 57608.5939814815 | 2016-08-08 14:15:20 | 56709 | 2014-02-21 00:00:00 | 56342.5463888889 | 2013-02-19 13:06:48 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071848 | 29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | MARIE MACHACEK | USA | 7 | AO7 | MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807137010/ | Quick Look | ![]() |
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689 | SHAPLEY C | 202.085 | -31.0332 | 201.382602 | -30.774544 | 212.227549 | -20.169518 | 312.17140577 | 31.17563268 | 109.0374 | 56330.7851273148 | 2013-02-07 18:50:35 | 56331.4147453704 | 2013-02-08 09:57:14 | 807138010 | 30.8744 | 30 | 30.8904 | 30.8744 | 0 | 30.8904 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.966 | 31.966 | 54.392 | 0 | PROCESSED | 57610.5475694444 | 2016-08-10 13:08:30 | 56715 | 2014-02-27 00:00:00 | 56349.523287037 | 2013-02-26 12:33:32 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071848 | 29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | MARIE MACHACEK | USA | 7 | AO7 | MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807138010/ | Quick Look | ![]() |
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690 | A3627_WEST | 243.1701 | -60.6984 | 242.089882 | -60.570358 | 253.528582 | -38.78018 | 325.22376786 | -6.86207305 | 306.0002 | 56546.5563425926 | 2013-09-11 13:21:08 | 56547.2535185185 | 2013-09-12 06:05:04 | 808059010 | 52.7998 | 50 | 52.7998 | 52.8237 | 0 | 52.8078 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.8968 | 42.8968 | 60.2319 | 0 | PROCESSED | 57612.5956481482 | 2016-08-12 14:17:44 | 56956 | 2014-10-26 00:00:00 | 56588.7134837963 | 2013-10-23 17:07:25 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080097 | We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATSUHIRO HAYASHI | JAP | 8 | AO8 | OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808059010/ | Quick Look | ![]() |
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691 | FJ1336+3553_OFFSET | 203.9396 | 35.8517 | 203.380018 | 36.106643 | 185.299819 | 41.923502 | 78.4395295 | 77.15761363 | 299.9998 | 56836.6568171296 | 2014-06-28 15:45:49 | 56837.6530092593 | 2014-06-29 15:40:20 | 809041010 | 43.307 | 45 | 43.307 | 45.5019 | 0 | 45.5179 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3386458333 | 2016-08-15 08:07:39 | 57212 | 2015-07-09 00:00:00 | 56846.5938425926 | 2014-07-08 14:15:08 | 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/ver3.0/809041010/ | Quick Look | ![]() |
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692 | A3528-S OFFSET 4 | 194.1847 | -30.0435 | 193.505704 | -29.773143 | 205.130736 | -22.019409 | 304.29690153 | 32.8141993 | 288.9992 | 56503.6527199074 | 2013-07-30 15:39:55 | 56504.4071064815 | 2013-07-31 09:46:14 | 808107010 | 32.7752 | 30 | 32.7832 | 32.7752 | 0 | 32.7912 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 31.2585 | 31.2585 | 65.1599 | 0 | PROCESSED | 57612.0918634259 | 2016-08-12 02:12:17 | 56955 | 2014-10-25 00:00:00 | 56587.7238310185 | 2013-10-22 17:22:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LORENZO LOVISARI | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808107010/ | Quick Look | ![]() |
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693 | VIRGO E2 | 188.3405 | 12.688 | 187.708685 | 12.963651 | 182.515676 | 14.938652 | 285.71074231 | 74.9520878 | 284.9998 | 56481.5631944444 | 2013-07-08 13:31:00 | 56481.9592824074 | 2013-07-08 23:01:22 | 808117010 | 10.6598 | 10 | 10.6598 | 10.6598 | 0 | 10.6598 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6982 | 10.6982 | 34.22 | 0 | PROCESSED | 57611.7227199074 | 2016-08-11 17:20:43 | 56383 | 2013-04-01 00:00:00 | 56524.654212963 | 2013-08-20 15:42:04 | 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/ver3.0/808117010/ | Quick Look | ![]() |
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694 | VIRGO E4 | 188.894 | 12.9933 | 188.263024 | 13.268562 | 182.897357 | 15.437334 | 287.44169131 | 75.38588793 | 285.0007 | 56482.2160069445 | 2013-07-09 05:11:03 | 56482.4926157407 | 2013-07-09 11:49:22 | 808119010 | 12.9687 | 11 | 12.9927 | 12.9847 | 0 | 12.9687 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.283 | 9.283 | 23.8959 | 0 | PROCESSED | 57611.7741319444 | 2016-08-11 18:34:45 | 56383 | 2013-04-01 00:00:00 | 56496.5935185185 | 2013-07-23 14:14:40 | 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/ver3.0/808119010/ | Quick Look | ![]() |
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695 | VIRGO E9 | 190.3236 | 13.8446 | 189.694982 | 14.118738 | 183.856818 | 16.782028 | 292.32223865 | 76.50695206 | 284.9995 | 56484.1924305556 | 2013-07-11 04:37:06 | 56484.6162268518 | 2013-07-11 14:47:22 | 808124010 | 18.8719 | 18 | 18.8951 | 18.8879 | 0 | 18.8719 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.3674 | 15.3674 | 36.6119 | 0 | PROCESSED | 57611.8197106482 | 2016-08-11 19:40:23 | 56383 | 2013-04-01 00:00:00 | 56498.6214930556 | 2013-07-25 14:54:57 | 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/ver3.0/808124010/ | Quick Look | ![]() |
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696 | VIRGO E11 | 190.8574 | 14.15 | 190.229706 | 14.423674 | 184.22049 | 17.272492 | 294.34392528 | 76.88802661 | 285 | 56485.1965162037 | 2013-07-12 04:42:59 | 56485.8154513889 | 2013-07-12 19:34:15 | 808126010 | 23.3591 | 21 | 23.3671 | 23.3591 | 0 | 23.3737 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.9937 | 19.9937 | 53.4699 | 1 | PROCESSED | 57611.8143171296 | 2016-08-11 19:32:37 | 56383 | 2013-04-01 00:00:00 | 56498.6447106482 | 2013-07-25 15:28:23 | 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/ver3.0/808126010/ | Quick Look | ![]() |
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697 | CEN_A_LOBE_N5 | 198.8206 | -42.0777 | 198.100689 | -41.813564 | 214.682372 | -31.301214 | 307.6547721 | 20.57528449 | 295.9847 | 56865.6873032407 | 2014-07-27 16:29:43 | 56867.2502430556 | 2014-07-29 06:00:21 | 809006010 | 51.9392 | 50 | 51.9392 | 52.5746 | 0 | 52.5746 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6586 | 10.6586 | 20.936 | 0 | PROCESSED | 57615.4722916667 | 2016-08-15 11:20:06 | 57267 | 2015-09-02 00:00:00 | 56898.3358449074 | 2014-08-29 08:03:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809006010/ | Quick Look | ![]() |
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698 | THE MOON | 134.2483 | 11.6812 | 133.56589 | 11.874254 | 133.339832 | -5.352995 | 216.51758385 | 33.11115118 | 281.9606 | 56783.8139699074 | 2014-05-06 19:32:07 | 56783.948125 | 2014-05-06 22:45:18 | 809001030 | 6.4899 | 45 | 6.4979 | 6.4899 | 0 | 6.4979 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.02 | 7.02 | 11.5839 | 0 | PROCESSED | 57615.0497222222 | 2016-08-15 01:11:36 | 57162 | 2015-05-20 00:00:00 | 56793.5289930556 | 2014-05-16 12:41:45 | 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/ver3.0/809001030/ | Quick Look | ![]() |
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699 | THE MOON | 140.1926 | 10.5514 | 139.518228 | 10.7642 | 139.270066 | -4.724239 | 220.86178985 | 37.88683751 | 291.2213 | 56784.325775463 | 2014-05-07 07:49:07 | 56784.4480555556 | 2014-05-07 10:45:12 | 809001070 | 6.405 | 45 | 6.405 | 6.405 | 0 | 6.405 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.677 | 6.677 | 10.5539 | 0 | PROCESSED | 57615.0674074074 | 2016-08-15 01:37:04 | 57218 | 2015-07-15 00:00:00 | 56852.581875 | 2014-07-14 13:57:54 | 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/ver3.0/809001070/ | Quick Look | ![]() |
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700 | RXCJ2157.4-0747 SE | 329.2877 | -7.568 | 328.627588 | -7.806552 | 328.755658 | 4.621414 | 50.03773919 | -44.36639016 | 250.0002 | 56973.0839351852 | 2014-11-12 02:00:52 | 56973.6668055556 | 2014-11-12 16:00:12 | 809022010 | 25.9584 | 20 | 25.9744 | 25.9584 | 0 | 25.9824 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7636111111 | 2016-08-16 18:19:36 | 57352 | 2015-11-26 00:00:00 | 56986.4089351852 | 2014-11-25 09:48:52 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809022010/ | Quick Look | ![]() |
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701 | RXCJ2157.4-0747 SW | 329.5619 | -7.7328 | 328.901524 | -7.972036 | 328.954889 | 4.373264 | 50.03497203 | -44.68420804 | 250.0004 | 56976.2027893518 | 2014-11-15 04:52:01 | 56976.7307175926 | 2014-11-15 17:32:14 | 809023010 | 20.9188 | 20 | 20.9188 | 20.9188 | 0 | 20.9188 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.786099537 | 2016-08-16 18:51:59 | 57361 | 2015-12-05 00:00:00 | 56993.4286921296 | 2014-12-02 10:17:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809023010/ | Quick Look | ![]() |
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702 | A3112E | 49.9177 | -44.1055 | 49.483567 | -44.285626 | 26.168536 | -58.996914 | 252.54334877 | -55.82694751 | 25.0007 | 56829.3656134259 | 2014-06-21 08:46:29 | 56830.3266435185 | 2014-06-22 07:50:22 | 809024010 | 33.435 | 45 | 33.435 | 34.195 | 0 | 34.219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30.293 | 30.293 | 82.9918 | 1 | PROCESSED | 57615.3104398148 | 2016-08-15 07:27:02 | 57239 | 2015-08-05 00:00:00 | 56873.1925 | 2014-08-04 04:37:12 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KOSUKE SATO | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809024010/ | Quick Look | ![]() |
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703 | NGC 891 | 35.645 | 42.3416 | 34.858537 | 42.114299 | 47.830156 | 26.528514 | 140.39047988 | -17.41940889 | 243.1772 | 57072.5035300926 | 2015-02-19 12:05:05 | 57073.2222916667 | 2015-02-20 05:20:06 | 809054010 | 28.8738 | 100 | 28.8738 | 28.8738 | 0 | 28.8738 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6291550926 | 2016-08-17 15:05:59 | 57626 | 2016-08-26 00:00:00 | 57087.4767013889 | 2015-03-06 11:26:27 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091502 | The metallicity of the hot gas in the halos of isolated galaxies distinguishes between two models of galaxy formation, but few galaxies have bright enough halos to make this measurement. Metallicities measured in these systems are applied broadly and used in models, so it is important to understand the limits of the measurement. We address two ilimitations: we estimate the systematic error in the metallicity by comparing Suzaku and XMM-Newton observations, and we determine whether the bright, metal-enriched gas around starburst galaxies represents most of their mass. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | EDMUND HODGES-KLUCK | USA | 9 | AO9 | MEASURING SYSTEMATIC UNCERTAINTY IN THE HALO METALLICITY OF NGC 891 AND NGC 4631 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809054010/ | Quick Look | ![]() |
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704 | RXJ1159+5531 W | 179.7493 | 55.5442 | 179.104587 | 55.822511 | 149.726184 | 49.068198 | 137.82331154 | 60.04203639 | 299.9575 | 56808.2513657407 | 2014-05-31 06:01:58 | 56809.8959490741 | 2014-06-01 21:30:10 | 809064010 | 95.109 | 100 | 95.109 | 96.041 | 0 | 96.033 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1837731482 | 2016-08-15 04:24:38 | 57194 | 2015-06-21 00:00:00 | 56828.5942592593 | 2014-06-20 14:15:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091521 | In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 9 | AO9 | MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809064010/ | Quick Look | ![]() |
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705 | ABELL 98-NORTH | 11.5755 | 20.8389 | 10.914314 | 20.565865 | 18.902557 | 14.584397 | 121.31667052 | -42.01674062 | 67.4405 | 56840.5909259259 | 2014-07-02 14:10:56 | 56841.1634375 | 2014-07-03 03:55:21 | 809078010 | 25.0582 | 100 | 0 | 0 | 0 | 25.0582 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3531481482 | 2016-08-15 08:28:32 | 56748 | 2014-04-01 00:00:00 | 56855.7487268518 | 2014-07-17 17:58:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078010/ | Quick Look | ![]() |
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706 | ABELL 98-NORTH | 11.5799 | 20.8287 | 10.918717 | 20.555669 | 18.902203 | 14.573403 | 121.32183614 | -42.02704716 | 251.2557 | 57012.9175231482 | 2014-12-21 22:01:14 | 57014.2377430556 | 2014-12-23 05:42:21 | 809078030 | 49.5381 | 50 | 49.5381 | 51.7925 | 0 | 51.8085 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5690509259 | 2016-08-17 13:39:26 | 56748 | 2014-04-01 00:00:00 | 57107.4424305556 | 2015-03-26 10:37:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809078030/ | Quick Look | ![]() |
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707 | SWCL1313+0802 | 198.2492 | 8.0414 | 197.620834 | 8.306256 | 193.672615 | 14.576147 | 318.90135946 | 70.24184099 | 291.5304 | 56850.0041435185 | 2014-07-12 00:05:58 | 56850.5002199074 | 2014-07-12 12:00:19 | 809087010 | 20.2705 | 20 | 20.2705 | 20.2705 | 0 | 20.2705 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3782986111 | 2016-08-15 09:04:45 | 57229 | 2015-07-26 00:00:00 | 56861.6452083333 | 2014-07-23 15:29:06 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809087010/ | Quick Look | ![]() |
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708 | SWCL1330+4206 | 202.7226 | 42.119 | 202.178472 | 42.376237 | 179.66908 | 46.823596 | 97.20252966 | 72.98152353 | 144.6477 | 56984.0225347222 | 2014-11-23 00:32:27 | 56985.3840740741 | 2014-11-24 09:13:04 | 809088010 | 15.8612 | 49 | 15.8612 | 15.8776 | 0 | 15.8692 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8069212963 | 2016-08-16 19:21:58 | 57548 | 2016-06-09 00:00:00 | 57009.4143981482 | 2014-12-18 09:56:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809088010/ | Quick Look | ![]() |
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709 | ABELL 2151A | 241.1446 | 17.7141 | 240.581846 | 17.849628 | 234.487601 | 37.662842 | 31.46236827 | 44.65865226 | 285.8808 | 56883.5616898148 | 2014-08-14 13:28:50 | 56883.843900463 | 2014-08-14 20:15:13 | 809098010 | 11.0268 | 10 | 11.0348 | 11.0348 | 0 | 11.0268 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4947569444 | 2016-08-16 11:52:27 | 57270 | 2015-09-05 00:00:00 | 56910.6327893518 | 2014-09-10 15:11:13 | 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 | B | 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/ver3.0/809098010/ | Quick Look | ![]() |
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710 | RX J1347.5-1145 | 206.856 | -11.8093 | 206.189594 | -11.560184 | 209.147124 | -0.679556 | 323.97916756 | 48.76108187 | 292.056 | 53916.7756597222 | 2006-06-30 18:36:57 | 53918.7600115741 | 2006-07-02 18:14:25 | 801013010 | 69.6611 | 75 | 69.6611 | 69.6611 | 69.6611 | 69.6611 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60.982 | 60.982 | 171.3759 | 0 | PROCESSED | 57534.8555671296 | 2016-05-26 20:32:01 | 54394 | 2007-10-21 00:00:00 | 53926.4810300926 | 2006-07-10 11:32:41 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010014 | We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAOMI OTA | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801013010/ | Quick Look | ![]() |
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711 | OPHIUCHUS CLUSTER 5 | 258.0184 | -23.1077 | 257.261763 | -23.048099 | 258.982957 | -0.123527 | 0.73892155 | 9.49336651 | 88.7652 | 54181.8276736111 | 2007-03-22 19:51:51 | 54182.4890277778 | 2007-03-23 11:44:12 | 801026010 | 24.2557 | 15 | 24.2557 | 24.2557 | 0 | 24.2557 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.2271 | 19.2271 | 57.1359 | 0 | PROCESSED | 57537.9767013889 | 2016-05-29 23:26:27 | 54736 | 2008-09-27 00:00:00 | 54186.2070949074 | 2007-03-27 04:58:13 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YUTAKA FUJITA | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801026010/ | Quick Look | ![]() |
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712 | M87 CENTER | 187.7366 | 12.4456 | 187.103964 | 12.721646 | 182.061198 | 14.477269 | 283.82387862 | 74.55209055 | 120.529 | 54068.9187037037 | 2006-11-29 22:02:56 | 54071.1266666667 | 2006-12-02 03:02:24 | 801038010 | 98.1831 | 100 | 98.1831 | 98.1831 | 0 | 98.1831 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 88.2503 | 88.2503 | 190.7308 | 2 | PROCESSED | 57536.2829050926 | 2016-05-28 06:47:23 | 54735 | 2008-09-26 00:00:00 | 54090.4156134259 | 2006-12-21 09:58:29 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010084 | The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIRONORI MATSUMOTO | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801038010/ | Quick Look | ![]() |
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713 | PERSEUS CL OFFSET | 49.6445 | 42.068 | 48.814215 | 41.886236 | 58.537476 | 22.936041 | 150.06631202 | -12.92163855 | 65.996 | 53980.0800925926 | 2006-09-02 01:55:20 | 53980.7668287037 | 2006-09-02 18:24:14 | 801049010 | 29.2438 | 30 | 29.2559 | 29.2479 | 29.2518 | 29.2438 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.6729 | 25.6729 | 59.3299 | 1 | PROCESSED | 57535.4121296296 | 2016-05-27 09:53:28 | 54526 | 2008-03-01 00:00:00 | 54021.3135416667 | 2006-10-13 07:31:30 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049010/ | Quick Look | ![]() |
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714 | PERSEUS CL OFFSET | 50.2242 | 41.1004 | 49.398659 | 40.920786 | 58.698225 | 21.886134 | 150.98569591 | -13.49005998 | 65.9967 | 53981.4552662037 | 2006-09-03 10:55:35 | 53982.1418287037 | 2006-09-04 03:24:14 | 801049030 | 32.8396 | 30 | 32.8556 | 32.8476 | 32.8396 | 32.8636 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 31.0313 | 31.0313 | 59.288 | 0 | PROCESSED | 57535.4291087963 | 2016-05-27 10:17:55 | 54526 | 2008-03-01 00:00:00 | 54020.8372106482 | 2006-10-12 20:05:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801049030/ | Quick Look | ![]() |
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715 | ABELL 2199 OFFSET 2 | 247.3619 | 39.6495 | 246.934152 | 39.757579 | 233.32636 | 60.237575 | 63.07626508 | 43.54039287 | 251.2564 | 54011.5284722222 | 2006-10-03 12:41:00 | 54012.1578587963 | 2006-10-04 03:47:19 | 801058010 | 22.7072 | 25 | 22.7232 | 22.7072 | 22.7232 | 22.7232 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20.704 | 20.704 | 54.36 | 0 | PROCESSED | 57535.7442476852 | 2016-05-27 17:51:43 | 54735 | 2008-09-26 00:00:00 | 54024.6719907407 | 2006-10-16 16:07:40 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801058010/ | Quick Look | ![]() |
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716 | M101 | 210.8841 | 54.3679 | 210.442342 | 54.607302 | 174.405989 | 59.838606 | 101.97854462 | 59.72940376 | 150.2959 | 54062.5790625 | 2006-11-23 13:53:51 | 54064.7182175926 | 2006-11-25 17:14:14 | 801063010 | 98.8522 | 100 | 98.8762 | 98.8522 | 0 | 98.8762 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89.6125 | 89.6125 | 184.802 | 2 | PROCESSED | 57536.2145486111 | 2016-05-28 05:08:57 | 54455 | 2007-12-21 00:00:00 | 54088.707650463 | 2006-12-19 16:59:01 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011402 | We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | K. KUNTZ | USA | 1 | AO1 | SOFT DIFFUSE X-RAY EMISSION FROM M101 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801063010/ | Quick Look | ![]() |
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717 | SN 1987A | 83.9013 | -69.2655 | 83.9928 | -69.294887 | 307.391677 | -86.458548 | 279.69660922 | -31.92548266 | 330.0004 | 53894.6930555556 | 2006-06-08 16:38:00 | 53895.6683449074 | 2006-06-09 16:02:25 | 801090010 | 39.6464 | 40 | 39.6464 | 39.6464 | 39.6464 | 39.6464 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39.2519 | 39.2519 | 84.2399 | 0 | PROCESSED | 57534.6267592593 | 2016-05-26 15:02:32 | 54400 | 2007-10-27 00:00:00 | 53928.1346527778 | 2006-07-12 03:13:54 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012006 | In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | G NTHER HASINGER | EUR | 1 | AO1 | SN 1987A - A RUSTY REMNANT? | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801090010/ | Quick Look | ![]() |
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718 | ABELL 426 S4.5 | 49.6359 | 40.2959 | 48.817105 | 40.114123 | 57.998946 | 21.235515 | 151.06094801 | -14.4070178 | 87.9989 | 55426.0734375 | 2010-08-18 01:45:45 | 55426.4037037037 | 2010-08-18 09:41:20 | 805110010 | 9.1793 | 10 | 9.1793 | 9.1793 | 0 | 9.1793 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6.7459 | 6.7459 | 28.53 | 0 | PROCESSED | 57553.1162384259 | 2016-06-14 02:47:23 | 55287 | 2010-04-01 00:00:00 | 55439.1536342593 | 2010-08-31 03:41:14 | 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/ver3.0/805110010/ | Quick Look | ![]() |
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719 | A2142 OFFSET3 | 239.0356 | 27.7434 | 238.520462 | 27.887676 | 228.29172 | 46.798568 | 44.85726257 | 49.26078026 | 283.7312 | 54341.8454166667 | 2007-08-29 20:17:24 | 54342.3960532407 | 2007-08-30 09:30:19 | 802032010 | 23.7899 | 20 | 23.7899 | 23.7899 | 0 | 23.7899 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.2425 | 14.2425 | 47.5699 | 0 | PROCESSED | 57539.8930671296 | 2016-05-31 21:26:01 | 54724 | 2008-09-15 00:00:00 | 54356.294849537 | 2007-09-13 07:04:35 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020076 | We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKAYA OHASHI | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802032010/ | Quick Look | ![]() |
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720 | NGC 1553 | 64.0253 | -55.7788 | 63.753175 | -55.901382 | 28.715493 | -73.694617 | 265.63371114 | -43.7014546 | 176.9406 | 54429.7042939815 | 2007-11-25 16:54:11 | 54431.9029976852 | 2007-11-27 21:40:19 | 802050010 | 98.7222 | 95 | 98.7222 | 98.7222 | 0 | 98.7222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87.7903 | 87.7903 | 189.9159 | 2 | PROCESSED | 57540.6454976852 | 2016-06-01 15:29:31 | 54806 | 2008-12-06 00:00:00 | 54438.4258101852 | 2007-12-04 10:13:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021401 | As driving engines of metal enrichment, early-type galaxies provide vital laboratories to investigate how it operates. In our Chandra survey of galaxies, we found solar ISM abundances (Zfe), similar to the stars and implying enrichment homology from clusters to moderate-Lx galaxies. The only outlier was NGC1553, for which we found a tantalizing hint of very subsolar Zfe, inconsistent with simple models. Unlike other galaxies with recent reports of low Zfe, NGC1553 has a bright gas halo, so the results are insensitive to the modelling of unresolved LMXB. We propose an 80ks observation of NGC1553 to measure definitively the ISM abundances of Fe and other crucial diagnostic elements. These data will either confirm enrichment bimodality or provide a vital low-Lx data-point to anchor models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | PHILIP HUMPHREY | USA | 2 | AO2 | NGC 1553: PROOF OF BIMODAL METAL ENRICHMENT? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802050010/ | Quick Look | ![]() |
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721 | BOOTES GROUP 7 | 217.7796 | 35.0938 | 217.258508 | 35.314562 | 199.66622 | 46.620571 | 59.62119131 | 67.30227758 | 316.719 | 54266.3117592593 | 2007-06-15 07:28:56 | 54267.3863310185 | 2007-06-16 09:16:19 | 802053010 | 42.1244 | 38 | 42.1324 | 42.1244 | 0 | 42.1324 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37.3384 | 37.3384 | 92.8238 | 0 | PROCESSED | 57538.9915509259 | 2016-05-30 23:47:50 | 54695 | 2008-08-17 00:00:00 | 54322.4630324074 | 2007-08-10 11:06:46 | 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 | B | MARSHALL BAUTZ | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802053010/ | Quick Look | ![]() |
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722 | ABELL 2029 | 227.4644 | 6.0238 | 226.845557 | 6.213105 | 223.157402 | 22.814931 | 6.57368779 | 50.92713703 | 112.4532 | 54473.6848958333 | 2008-01-08 16:26:15 | 54478.0211226852 | 2008-01-13 00:30:25 | 802060010 | 169.2861 | 160 | 169.2861 | 169.2861 | 0 | 169.2861 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150.7661 | 150.7661 | 374.6201 | 4 | PROCESSED | 57541.3859953704 | 2016-06-02 09:15:50 | 54860 | 2009-01-29 00:00:00 | 54490.7163657407 | 2008-01-25 17:11:34 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021433 | The properties of clusters of galaxies in very distant regions encompassing the virial radius (r_vir) are poorly understood yet these regions are sites of very important processes for the cluster formation and evolution. The recent generation of X-ray satellites (Chandra and XMM) thanks to their fine spatial resolution and high sensitivity have provided so far detailed spectral information mainly in the inner bright regions but they have not been very helpful in background dominated regimes typical of cluster outskirts' observations because of their high background. Suzaku has the capabilities to target those regions. We propose to observe the outskirts of the very relaxed cluster of galaxies A2029 with XIS to measure for the first time temperature and metallicity of the ICM up to r_vir. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LUCA ZAPPACOSTA | USA | 2 | AO2 | EXPLORING THE OUTSKIRTS OF THE RELAXED CLUSTER ABELL 2029 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802060010/ | Quick Look | ![]() |
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723 | ABEL 754 | 137.2113 | -9.6361 | 136.602656 | -9.432794 | 142.867226 | -24.832228 | 239.25284371 | 24.7578079 | 295.1878 | 54249.7445833333 | 2007-05-29 17:52:12 | 54252.4495949074 | 2007-06-01 10:47:25 | 802063010 | 108.9779 | 100 | 108.9859 | 108.9859 | 0 | 108.9779 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97.904 | 97.904 | 233.6958 | 2 | PROCESSED | 57538.8549537037 | 2016-05-30 20:31:08 | 54773 | 2008-11-03 00:00:00 | 54257.5596759259 | 2007-06-06 13:25:56 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021445 | We propose a 100 ksec observation of Abell 754 and a 50 ksec observation of Triangulum Australis, in order to measure the spectral shape and flux of possible nonthermal emission from clusters of galaxies. They are bright clusters of galaxies in the BAT all sky survey sample, which is crucial for making good spectral measurements by the HXD. And their spectra have a significant hard excess (power-law component). We intend to constrain the power-law photon index of the nonthermal emission for the first time and to determine the size of hard X-ray emitting region by using both of the HXD and Swift BAT data. We are aiming to test the origin of the hard flux and see whether it originates from either diffuse inverse Compton scattering by relativistic cosmic-ray electrons or an AGN. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKASHI OKAJIMA | USA | 2 | AO2 | OBSERVATIONS OF NONTHERMAL EMISSION FROM CLUSTERS OF GALAXIES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802063010/ | Quick Look | ![]() |
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724 | RCS 1122+2423 | 170.6071 | 24.3899 | 169.945012 | 24.664262 | 161.499487 | 18.645294 | 215.72830536 | 69.79971375 | 120.0624 | 54421.3268518518 | 2007-11-17 07:50:40 | 54421.8891087963 | 2007-11-17 21:20:19 | 802070010 | 20.9729 | 18 | 20.9809 | 20.9809 | 0 | 20.9729 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.022 | 19.022 | 48.5679 | 0 | PROCESSED | 57540.5406828704 | 2016-06-01 12:58:35 | 54797 | 2008-11-27 00:00:00 | 54430.3244097222 | 2007-11-26 07:47:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021451 | We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 2 | AO2 | A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802070010/ | Quick Look | ![]() |
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725 | COMABKG2 | 194.3428 | 28.1403 | 193.738458 | 28.410336 | 180.855412 | 31.302815 | 70.87532192 | 88.34137752 | 297.3385 | 54272.7041550926 | 2007-06-21 16:53:59 | 54273.4897453704 | 2007-06-22 11:45:14 | 802084010 | 31.9731 | 30 | 31.9731 | 33.5956 | 0 | 33.5956 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.853 | 28.853 | 67.8501 | 1 | PROCESSED | 57539.0184143518 | 2016-05-31 00:26:31 | 54695 | 2008-08-17 00:00:00 | 54318.5135648148 | 2007-08-06 12:19:32 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024438 | Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JOEL BREGMAN | Yoh Takei | USJ | 2 | AO2 | THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802084010/ | Quick Look | ![]() |
726 | NGC3556 | 167.883 | 55.6841 | 167.153795 | 55.95585 | 141.585681 | 45.289435 | 148.29932367 | 56.24590288 | 111.9355 | 54795.9750694444 | 2008-11-25 23:24:06 | 54797.8890162037 | 2008-11-27 21:20:11 | 803013010 | 84.1642 | 100 | 84.1702 | 84.1659 | 0 | 84.1642 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.3537 | 60.3537 | 165.2879 | 2 | PROCESSED | 57544.6094212963 | 2016-06-05 14:37:34 | 55175 | 2009-12-10 00:00:00 | 54811.7645717593 | 2008-12-11 18:20:59 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030058 | We propose to observe NGC 3556, a nearby edge-on spiral galaxy, with 100 ks exposure. Galactic coronal X-ray emission in and around several spiral galaxies have been spatially resolved using Chandra and XMM instruments. The target is one of these galaxies showing relatively luminous X-ray emission. Due to limited spectral capability of these instruments, X-ray spectral properties of these diffuse emission have not yet been investigated. We use good spectral capability of the SUZAKU/XIS to investigate the temperature structure and constrain the metal abundance pattern for the first time in galactic corona. We study origin, heating mechanism, and chemical properties of these galactic corona. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAYUKI TAMURA | JAP | 3 | AO3 | GALACTIC CORONA IN AND AROUND THE EDGE-ON GALAXY NGC 3556 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803013010/ | Quick Look | ![]() |
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727 | A2163_NE | 244.026 | -6.0591 | 243.359036 | -5.935716 | 243.191505 | 14.996833 | 6.90407558 | 30.45267126 | 113.8304 | 54870.8869560185 | 2009-02-08 21:17:13 | 54872.1724421296 | 2009-02-10 04:08:19 | 803022010 | 51.7974 | 40 | 51.8054 | 51.8134 | 0 | 51.7974 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.861 | 43.861 | 111.0518 | 1 | PROCESSED | 57545.4990162037 | 2016-06-06 11:58:35 | 55330 | 2010-05-14 00:00:00 | 54895.5963888889 | 2009-03-05 14:18:48 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030094 | We propose 2 pointing observations of a hot cluster A2163 (z=0.2). A2163 is an X-ray brightest object among the violent merger candidates, which possess a huge radio halo and a complex temperature structure. Thus it is a unique target to discover extremely hot (>20keV) gas produced via merger shock. Thanks to the unprecedent high-quality broad-band spectra of Suzaku we can accurately determine the temperature of the hot gas. Which, at the same time, leads to the detection of the buried non-thermal hard X-ray emission. Combining this observation with the high-resolution images of our thermal SZ effect and the XMM observation, we can obtain a spatial distribution of the extremely hot thermal gas in the merging cluster for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 3 | AO3 | BROAD-BAND SPECTROSCOPY OF THE HOTTEST ABELL GALAXY CLUSTER A2163 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803022010/ | Quick Look | ![]() |
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728 | N154 SB | 84.0182 | -69.641 | 84.124614 | -69.669786 | 303.069824 | -86.201105 | 280.12884425 | -31.83619967 | 313.3253 | 54583.7906944444 | 2008-04-27 18:58:36 | 54584.7849305556 | 2008-04-28 18:50:18 | 803037010 | 50.404 | 40 | 50.404 | 50.404 | 0 | 50.404 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56.6171 | 56.6171 | 85.8878 | 1 | PROCESSED | 57542.411724537 | 2016-06-03 09:52:53 | 54964 | 2009-05-13 00:00:00 | 54598.4914699074 | 2008-05-12 11:47:43 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LARRY MADDOX | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803037010/ | Quick Look | ![]() |
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729 | NGC 5846 | 226.6234 | 1.6025 | 225.988646 | 1.794814 | 223.667836 | 18.340527 | 0.42380195 | 48.79350498 | 287.2336 | 54675.6192939815 | 2008-07-28 14:51:47 | 54679.0008564815 | 2008-08-01 00:01:14 | 803042010 | 155.9331 | 150 | 155.9331 | 155.9331 | 0 | 155.9331 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 145.4704 | 145.4704 | 292.1519 | 2 | PROCESSED | 57543.2487152778 | 2016-06-04 05:58:09 | 55059 | 2009-08-16 00:00:00 | 54693.5527546296 | 2008-08-15 13:15:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031404 | We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MICHAEL LOEWENSTEIN | USA | 3 | AO3 | UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803042010/ | Quick Look | ![]() |
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730 | A496 P-OUT | 68.2513 | -13.0087 | 67.67058 | -13.113188 | 64.018052 | -34.510238 | 209.22191803 | -36.52315476 | 62.0525 | 54674.5225347222 | 2008-07-27 12:32:27 | 54675.6050231482 | 2008-07-28 14:31:14 | 803048010 | 37.5516 | 35 | 37.5516 | 37.5596 | 0 | 37.5596 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33.1599 | 33.1599 | 93.4939 | 1 | PROCESSED | 57543.1577314815 | 2016-06-04 03:47:08 | 55055 | 2009-08-12 00:00:00 | 54689.4360416667 | 2008-08-11 10:27:54 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031424 | A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | RENATO DUPKE | USA | 3 | AO3 | LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803048010/ | Quick Look | ![]() |
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731 | RCS2347-3535 | 356.9535 | -35.5892 | 356.30102 | -35.867184 | 341.527794 | -31.116965 | 357.03141214 | -74.03003146 | 61.6856 | 54617.4612384259 | 2008-05-31 11:04:11 | 54617.8890509259 | 2008-05-31 21:20:14 | 803057010 | 15.4812 | 11 | 15.4892 | 15.4892 | 0 | 15.4812 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14.6376 | 14.6376 | 36.9599 | 0 | PROCESSED | 57542.6853703704 | 2016-06-03 16:26:56 | 54999 | 2009-06-17 00:00:00 | 54633.6966087963 | 2008-06-16 16:43:07 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803057010/ | Quick Look | ![]() |
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732 | RCS1102-0340 | 165.6613 | -3.6697 | 165.025025 | -3.400357 | 168.238102 | -9.034138 | 258.27932815 | 49.53254853 | 114.238 | 54817.9779282407 | 2008-12-17 23:28:13 | 54818.8987731482 | 2008-12-18 21:34:14 | 803064010 | 37.789 | 28 | 37.797 | 37.797 | 0 | 37.789 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27.621 | 27.621 | 79.55 | 1 | PROCESSED | 57545.0002893518 | 2016-06-06 00:00:25 | 55206 | 2010-01-10 00:00:00 | 54840.5080439815 | 2009-01-09 12:11:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803064010/ | Quick Look | ![]() |
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733 | A3558 WEST OFF | 201.4503 | -31.5856 | 200.748303 | -31.325817 | 211.928183 | -20.890972 | 311.44383739 | 30.71755895 | 288.4754 | 54657.5304513889 | 2008-07-10 12:43:51 | 54660.0225 | 2008-07-13 00:32:24 | 803072010 | 81.8162 | 80 | 81.8162 | 81.8162 | 0 | 81.8162 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67.3941 | 67.3941 | 215.2857 | 1 | PROCESSED | 57543.1016898148 | 2016-06-04 02:26:26 | 55037 | 2009-07-25 00:00:00 | 54670.5540162037 | 2008-07-23 13:17:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 033089 | We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | MASSIMILIANO GALEAZZAI | JUS | 3 | AO3 | SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803072010/ | Quick Look | ![]() |
734 | FERMI_0265 | 187.7993 | -14.1672 | 187.149588 | -13.891145 | 192.78645 | -9.915447 | 295.5292019 | 48.41340382 | 292.6305 | 55040.2233449074 | 2009-07-28 05:21:37 | 55041.5002777778 | 2009-07-29 12:00:24 | 804017020 | 52.6378 | 54 | 52.6378 | 52.9098 | 0 | 52.9018 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 48.06 | 48.06 | 110.3041 | 0 | PROCESSED | 57547.9908333333 | 2016-06-08 23:46:48 | 55422 | 2010-08-14 00:00:00 | 55050.4462384259 | 2009-08-07 10:42:35 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804017020/ | Quick Look | ![]() |
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735 | FERMI_0291 | 203.2955 | 51.017 | 202.790071 | 51.273115 | 172.022229 | 54.301955 | 107.38909593 | 64.83295576 | 302.8355 | 54983.4258680556 | 2009-06-01 10:13:15 | 54984.4725 | 2009-06-02 11:20:24 | 804019010 | 46.3536 | 40 | 46.3616 | 46.3536 | 0 | 46.3696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42.7073 | 42.7073 | 90.3858 | 1 | PROCESSED | 57547.4428703704 | 2016-06-08 10:37:44 | 55363 | 2010-06-16 00:00:00 | 54994.2756018518 | 2009-06-12 06:36:52 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | JUN KATAOKA | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804019010/ | Quick Look | ![]() |
|
736 | NGC741MOSAICE_P3 | 29.6423 | 5.6966 | 28.988354 | 5.453848 | 29.583767 | -6.010817 | 151.72656453 | -53.38013742 | 71.7748 | 55054.3340509259 | 2009-08-11 08:01:02 | 55054.5765393518 | 2009-08-11 13:50:13 | 804052030 | 9.8918 | 10 | 9.8918 | 9.8918 | 0 | 9.9078 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.9599 | 7.9599 | 20.9439 | 1 | PROCESSED | 57548.1180555556 | 2016-06-09 02:50:00 | 55448 | 2010-09-09 00:00:00 | 55081.2008101852 | 2009-09-07 04:49:10 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052030/ | Quick Look | ![]() |
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737 | NGC741MOSAICS_P2 | 29.298 | 4.8125 | 28.646295 | 4.568934 | 28.95035 | -6.72009 | 151.84866444 | -54.32564909 | 71.7104 | 55052.6950925926 | 2009-08-09 16:40:56 | 55052.9238310185 | 2009-08-09 22:10:19 | 804054020 | 11.4289 | 10 | 11.4529 | 11.4289 | 0 | 11.4529 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6.3123 | 6.3123 | 19.7439 | 0 | PROCESSED | 57548.0884953704 | 2016-06-09 02:07:26 | 55451 | 2010-09-12 00:00:00 | 55085.0388425926 | 2009-09-11 00:55:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054020/ | Quick Look | ![]() |
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738 | ABELL 426 E4 | 51.4246 | 41.5162 | 50.593046 | 41.341069 | 59.755665 | 22.042042 | 151.51141512 | -12.63936589 | 90 | 55042.2912847222 | 2009-07-30 06:59:27 | 55042.7466898148 | 2009-07-30 17:55:14 | 804059010 | 21.8613 | 20 | 21.8613 | 21.8613 | 0 | 21.8613 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19.707 | 19.707 | 39.336 | 0 | PROCESSED | 57547.9976736111 | 2016-06-08 23:56:39 | 55427 | 2010-08-19 00:00:00 | 55060.7938425926 | 2009-08-17 19:03:08 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804059010/ | Quick Look | ![]() |
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739 | ABELL 426 E6 | 52.1705 | 41.5044 | 51.337024 | 41.332096 | 60.333006 | 21.882473 | 151.98723888 | -12.32905015 | 86.9996 | 55043.2937847222 | 2009-07-31 07:03:03 | 55043.9501736111 | 2009-07-31 22:48:15 | 804061010 | 31.9431 | 30 | 31.9431 | 31.9431 | 0 | 31.9431 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29.9436 | 29.9436 | 56.702 | 1 | PROCESSED | 57548.0213657407 | 2016-06-09 00:30:46 | 55427 | 2010-08-19 00:00:00 | 55060.7142013889 | 2009-08-17 17:08:27 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804061010/ | Quick Look | ![]() |
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740 | ABELL 426 N1 | 49.7797 | 41.7196 | 48.951337 | 41.538337 | 58.536882 | 22.573374 | 150.34867405 | -13.15794685 | 59.9997 | 55061.841099537 | 2009-08-18 20:11:11 | 55062.1397453704 | 2009-08-19 03:21:14 | 804063010 | 14.7276 | 10 | 14.7356 | 14.7276 | 0 | 14.737 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.1724 | 13.1724 | 25.7919 | 0 | PROCESSED | 57548.2770833333 | 2016-06-09 06:39:00 | 55441 | 2010-09-02 00:00:00 | 55075.0515740741 | 2009-09-01 01:14:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804063010/ | Quick Look | ![]() |
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741 | ABELL2811-OFF | 10.1781 | -28.7333 | 9.563743 | -29.007637 | 356.740152 | -30.181509 | 358.19144602 | -87.13859798 | 232.6526 | 53702.8821296296 | 2005-11-28 21:10:16 | 53703.731412037 | 2005-11-29 17:33:14 | 800006010 | 33.9494 | 25 | 33.9574 | 33.9654 | 33.9494 | 33.9498 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30.9056 | 30.9056 | 73.3659 | 1 | PROCESSED | 57528.1125115741 | 2016-05-20 02:42:01 | 54247 | 2007-05-27 00:00:00 | 54038.6719560185 | 2006-10-30 16:07:37 | 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/ver3.0/800006010/ | Quick Look | ![]() |
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742 | ABELL 2199 OFFSET 1 | 247.0269 | 39.6504 | 246.598636 | 39.759978 | 232.832467 | 60.158374 | 63.06766091 | 43.79825488 | 251.7923 | 54009.8973958333 | 2006-10-01 21:32:15 | 54010.4467476852 | 2006-10-02 10:43:19 | 801057010 | 24.6315 | 25 | 24.6315 | 24.6315 | 24.6315 | 24.6315 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25.5343 | 25.5343 | 47.454 | 0 | PROCESSED | 57535.7339814815 | 2016-05-27 17:36:56 | 54735 | 2008-09-26 00:00:00 | 54021.2449189815 | 2006-10-13 05:52:41 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801057010/ | Quick Look | ![]() |
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743 | ABELL 2199 OFFSET 3 | 247.3596 | 39.3165 | 246.92934 | 39.424595 | 233.528009 | 59.920137 | 62.61707687 | 43.53145251 | 252.4737 | 54012.1589351852 | 2006-10-04 03:48:52 | 54012.6786921296 | 2006-10-04 16:17:19 | 801059010 | 25.2467 | 25 | 25.2467 | 25.2467 | 25.2467 | 25.2467 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20.505 | 20.505 | 44.8879 | 1 | PROCESSED | 57535.7507291667 | 2016-05-27 18:01:03 | 54735 | 2008-09-26 00:00:00 | 54025.4730092593 | 2006-10-17 11:21:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MADOKA KAWAHARADA | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801059010/ | Quick Look | ![]() |
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744 | N206 SB | 82.6396 | -71.0391 | 82.803839 | -71.074403 | 297.258629 | -84.798656 | 281.83986558 | -32.08582418 | 315.5807 | 54584.7862384259 | 2008-04-28 18:52:11 | 54585.7640509259 | 2008-04-29 18:20:14 | 803038010 | 48.8345 | 40 | 48.8345 | 48.8345 | 0 | 48.8345 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.7297 | 54.7297 | 84.4678 | 1 | PROCESSED | 57542.434837963 | 2016-06-03 10:26:10 | 54964 | 2009-05-13 00:00:00 | 54598.4969444445 | 2008-05-12 11:55:36 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LARRY MADDOX | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803038010/ | Quick Look | ![]() |
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745 | COMA OUTSKIRTS3 | 196.1692 | 28.7094 | 195.570451 | 28.977142 | 182.240031 | 32.536562 | 62.09765822 | 86.67565791 | 116.0002 | 55901.9229513889 | 2011-12-06 22:09:03 | 55902.7161342593 | 2011-12-07 17:11:14 | 806022010 | 31.22 | 30 | 31.244 | 31.22 | 0 | 31.22 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28.7241 | 28.7241 | 68.5199 | 0 | PROCESSED | 57604.0669212963 | 2016-08-04 01:36:22 | 56284 | 2012-12-23 00:00:00 | 55915.1959837963 | 2011-12-20 04:42:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKUYA SATO | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806022010/ | Quick Look | ![]() |
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746 | NGC741S2_P1 | 29.0961 | 5.1589 | 28.443649 | 4.91486 | 28.882528 | -6.325199 | 151.28423043 | -54.09870829 | 71.6444 | 55053.3762962963 | 2009-08-10 09:01:52 | 55053.6078587963 | 2009-08-10 14:35:19 | 804055010 | 8.6016 | 10 | 8.6176 | 8.6016 | 0 | 8.6256 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8.748 | 8.748 | 19.984 | 1 | PROCESSED | 57548.1032291667 | 2016-06-09 02:28:39 | 55465 | 2010-09-26 00:00:00 | 55098.1609375 | 2009-09-24 03:51:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804055010/ | Quick Look | ![]() |
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747 | ABELL 426 E7 | 52.5439 | 41.4965 | 51.709488 | 41.325623 | 60.621576 | 21.801638 | 152.22519414 | -12.17349332 | 85.5 | 55043.9514814815 | 2009-07-31 22:50:08 | 55044.6843055556 | 2009-08-01 16:25:24 | 804062010 | 30.9516 | 30 | 30.9516 | 31.2216 | 0 | 31.2056 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 28.5449 | 28.5449 | 63.314 | 0 | PROCESSED | 57548.0327083333 | 2016-06-09 00:47:06 | 55427 | 2010-08-19 00:00:00 | 55060.8353703704 | 2009-08-17 20:02:56 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804062010/ | Quick Look | ![]() |
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748 | A2204_FIELD_3 | 248.3129 | 5.7152 | 247.698224 | 5.819454 | 245.539745 | 27.332187 | 21.30307351 | 33.20188623 | 261.0004 | 55436.6750347222 | 2010-08-28 16:12:03 | 55437.758587963 | 2010-08-29 18:12:22 | 805058010 | 36.2307 | 40 | 36.2387 | 36.2307 | 0 | 36.2467 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31.6564 | 31.6564 | 93.6018 | 2 | PROCESSED | 57553.2217361111 | 2016-06-14 05:19:18 | 55287 | 2010-04-01 00:00:00 | 55449.3168634259 | 2010-09-10 07:36:17 | 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/ver3.0/805058010/ | Quick Look | ![]() |
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749 | A2744_SW | 3.5132 | -30.5508 | 2.881732 | -30.828827 | 349.850108 | -29.168885 | 8.03425743 | -81.13040471 | 233.4967 | 55540.2569791667 | 2010-12-10 06:10:03 | 55542.2883217593 | 2010-12-12 06:55:11 | 805015010 | 69.7763 | 65 | 69.7763 | 69.7763 | 0 | 69.7763 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59.2396 | 59.2396 | 175.4817 | 0 | PROCESSED | 57554.4226851852 | 2016-06-15 10:08:40 | 55917 | 2011-12-22 00:00:00 | 55551.0433101852 | 2010-12-21 01:02:22 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050013 | We propose Suzaku observations of two merging clusters of galaxies, A2744 and the Bullet Cluster, to map the entropy variation out to the virial radius. Recent numerical simulations indicate that the entropy generation occurs through two-shock propagations, which is to be markedly seen in the cluster outskirts. On the other hand, little observational testing has been done for this regime of merging systems. We thus request three additional pointings to cover regions of large-scale filaments discovered in the optical. This study can only be achieved by Suzaku because of the lowest background level and excellent sensitivity, and will bring us new constraints on the thermodynamical history of the clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 5 | AO5 | MAPPING THE GAS ENTROPY GENERATION IN A SEQUENCE OF MERGING CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805015010/ | Quick Look | ![]() |
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750 | RXCJ0411.2-4819 | 62.816 | -48.3247 | 62.453818 | -48.452722 | 38.950898 | -67.014001 | 255.63059498 | -46.16240445 | 110.1457 | 55461.4637384259 | 2010-09-22 11:07:47 | 55461.7793865741 | 2010-09-22 18:42:19 | 805024010 | 11.3649 | 10 | 11.3649 | 11.3649 | 0 | 11.3649 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10.396 | 10.396 | 27.264 | 0 | PROCESSED | 57553.4942361111 | 2016-06-14 11:51:42 | 55836 | 2011-10-02 00:00:00 | 55470.1084606482 | 2010-10-01 02:36:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050021 | We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAOMI OTA | JAP | 5 | AO5 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805024010/ | Quick Look | ![]() |
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751 | NGC 4697 | 192.1513 | -5.7906 | 191.50498 | -5.518104 | 193.427288 | -0.530434 | 301.63561999 | 57.07401872 | 112.9816 | 55575.4840277778 | 2011-01-14 11:37:00 | 55578.1905324074 | 2011-01-17 04:34:22 | 805041010 | 102.3091 | 100 | 102.3091 | 102.3091 | 0 | 102.3091 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76.0471 | 76.0471 | 233.8161 | 1 | PROCESSED | 57600.7175462963 | 2016-07-31 17:13:16 | 55962 | 2012-02-05 00:00:00 | 55595.5109027778 | 2011-02-03 12:15:42 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050080 | We propose the observation of the elliptical galaxy NGC 4697, whose temperature of interstellar medium is low, 0.3 keV. Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. The different abundance pattern between S0 and elliptical galaxies was reported in recent study. To understand the formation process of early-type galaxies in more detail, it is very important to appreciate whether the different abundance pattern is due to morphology or temperature of system. The purpose of this proposal is to reveal the relation between abundance pattern, morphology, and temperature of system by investigating the abundance pattern of the elliptical galaxy, which has lower temperature. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SAORI KONAMI | JAP | 5 | AO5 | MEASUREMENT OF ABUNDANCE PATTERN IN LOW TEMPARTURE ISM OF ELLIPTICAL GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805041010/ | Quick Look | ![]() |
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752 | A1413_FIELD_2 | 178.6363 | 23.4218 | 177.992083 | 23.700041 | 169.007568 | 20.85313 | 225.87600909 | 76.62442609 | 303.0004 | 55346.1403240741 | 2010-05-30 03:22:04 | 55347.1856828704 | 2010-05-31 04:27:23 | 805060010 | 40.9512 | 40 | 40.9592 | 40.9512 | 0 | 40.9512 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34.5464 | 34.5464 | 90.2959 | 0 | PROCESSED | 57551.669837963 | 2016-06-12 16:04:34 | 55287 | 2010-04-01 00:00:00 | 55365.258912037 | 2010-06-18 06:12:50 | 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/ver3.0/805060010/ | Quick Look | ![]() |
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753 | A383_FIELD_1 | 42.1211 | -3.4616 | 41.492043 | -3.669137 | 38.559838 | -18.768369 | 177.79816007 | -53.37318565 | 60.9988 | 55388.2747337963 | 2010-07-11 06:35:37 | 55389.1376388889 | 2010-07-12 03:18:12 | 805062010 | 40.3915 | 40 | 40.4155 | 40.3915 | 0 | 40.4155 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35.3721 | 35.3721 | 74.52 | 1 | PROCESSED | 57552.5965046296 | 2016-06-13 14:18:58 | 55287 | 2010-04-01 00:00:00 | 55411.2489467593 | 2010-08-03 05:58:29 | 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/ver3.0/805062010/ | Quick Look | ![]() |
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754 | A383_FIELD_3 | 41.9643 | -3.6473 | 41.33581 | -3.855343 | 38.341492 | -18.895957 | 177.84591826 | -53.61436812 | 60.9989 | 55390.0630902778 | 2010-07-13 01:30:51 | 55390.9764930556 | 2010-07-13 23:26:09 | 805064010 | 43.1968 | 40 | 43.1968 | 43.1968 | 0 | 43.1968 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39.5929 | 39.5929 | 78.8959 | 1 | PROCESSED | 57552.6323842593 | 2016-06-13 15:10:38 | 55287 | 2010-04-01 00:00:00 | 55411.2967592593 | 2010-08-03 07:07:20 | 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/ver3.0/805064010/ | Quick Look | ![]() |
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755 | ABELL 426 S1 | 49.8666 | 41.2611 | 49.040997 | 41.080162 | 58.466927 | 22.114789 | 150.66369426 | -13.50507569 | 88 | 55424.9920601852 | 2010-08-16 23:48:34 | 55425.2995138889 | 2010-08-17 07:11:18 | 805096010 | 8.4343 | 10 | 8.4423 | 8.4503 | 0 | 8.4343 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.8611 | 7.8611 | 26.5499 | 0 | PROCESSED | 57553.0919675926 | 2016-06-14 02:12:26 | 55287 | 2010-04-01 00:00:00 | 55439.0952662037 | 2010-08-31 02:17:11 | 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/ver3.0/805096010/ | Quick Look | ![]() |
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756 | ABELL 426 S6 | 49.5399 | 39.884 | 48.723938 | 39.701875 | 57.801339 | 20.859927 | 151.23166434 | -14.79141746 | 87.9993 | 55426.858900463 | 2010-08-18 20:36:49 | 55427.3321759259 | 2010-08-19 07:58:20 | 805101010 | 16.4888 | 15 | 16.5048 | 16.5048 | 0 | 16.4888 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.4845 | 13.4845 | 40.8879 | 1 | PROCESSED | 57553.1336342593 | 2016-06-14 03:12:26 | 55287 | 2010-04-01 00:00:00 | 55439.1815625 | 2010-08-31 04:21:27 | 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/ver3.0/805101010/ | Quick Look | ![]() |
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757 | COMA E1 | 195.2288 | 27.9019 | 194.626316 | 28.170859 | 181.798966 | 31.442311 | 53.6887936 | 87.76083997 | 279.9992 | 55728.9920601852 | 2011-06-16 23:48:34 | 55729.2682523148 | 2011-06-17 06:26:17 | 806030010 | 9.184 | 10 | 9.2 | 9.184 | 0 | 9.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.2038 | 10.2038 | 23.858 | 0 | PROCESSED | 57602.3046296296 | 2016-08-02 07:18:40 | 55652 | 2011-04-01 00:00:00 | 55770.1007407407 | 2011-07-28 02:25:04 | 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/ver3.0/806030010/ | Quick Look | ![]() |
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758 | ABELL 426 W3 | 48.8462 | 41.5856 | 48.021362 | 41.400926 | 57.770933 | 22.640736 | 149.82172461 | -13.64958161 | 93.9989 | 55428.9659722222 | 2010-08-20 23:11:00 | 55429.3022916667 | 2010-08-21 07:15:18 | 805105010 | 11.1661 | 10 | 11.1901 | 11.1821 | 0 | 11.1661 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.1647 | 9.1647 | 29.036 | 0 | PROCESSED | 57553.1487962963 | 2016-06-14 03:34:16 | 55287 | 2010-04-01 00:00:00 | 55445.2284143518 | 2010-09-06 05:28:55 | 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/ver3.0/805105010/ | Quick Look | ![]() |
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759 | ABELL 426 W5 | 48.1001 | 41.6131 | 47.277233 | 41.425733 | 57.199753 | 22.826654 | 149.32075885 | -13.92405492 | 94.0016 | 55429.7828125 | 2010-08-21 18:47:15 | 55429.9946296296 | 2010-08-21 23:52:16 | 805107010 | 9.2192 | 10 | 9.2192 | 9.2192 | 0 | 9.2192 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7.8166 | 7.8166 | 18.2979 | 0 | PROCESSED | 57553.1586689815 | 2016-06-14 03:48:29 | 55287 | 2010-04-01 00:00:00 | 55445.231087963 | 2010-09-06 05:32:46 | 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/ver3.0/805107010/ | Quick Look | ![]() |
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760 | CENTAURUS B | 206.7067 | -60.4086 | 205.850027 | -60.15889 | 231.235341 | -45.192759 | 309.7224369 | 1.73083578 | 275.5009 | 55758.843912037 | 2011-07-16 20:15:14 | 55760.4932060185 | 2011-07-18 11:50:13 | 806017010 | 93.6172 | 120 | 93.645 | 93.6172 | 0 | 93.637 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 27.6959 | 0 | PROCESSED | 57602.5915625 | 2016-08-02 14:11:51 | 56152 | 2012-08-13 00:00:00 | 55830.7256134259 | 2011-09-26 17:24:53 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060070 | X-ray observation of radio lobe is essential to reveal the particle acceleration mechanism in the lobe, because we can obtain magnetic field and electron energy density without assumption of equipartition. The radio lobe of FR I radio galaxy Centaurus B was previously detected by ASCA. For revealing the mechanism of particle acceleration in radio lobes, detailed multi-wavelength observations are very important. We propose a deep observation of the radio lobe by Suzaku, which has the advantage of low background and high sensitivity for diffuse X-ray. Good quality Suzaku data combined with a detailed modeling reveals particle acceleration mechanism working in the radio lobe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YASUYUKI TANAKA | JAP | 6 | AO6 | X-RAY OBSERVATION OF RADIO LOBE OF FR I RADIO GALAXY CENTAURUS B | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806017010/ | Quick Look | ![]() |
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761 | ABELL 426 N2 | 49.5875 | 41.9633 | 48.758073 | 41.781328 | 58.461538 | 22.847366 | 150.08864093 | -13.03246307 | 59.9939 | 55062.1402662037 | 2009-08-19 03:21:59 | 55062.4716898148 | 2009-08-19 11:19:14 | 804064010 | 13.166 | 10 | 13.166 | 13.166 | 0 | 13.166 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.647 | 9.647 | 28.6239 | 0 | PROCESSED | 57548.2750578704 | 2016-06-09 06:36:05 | 55441 | 2010-09-02 00:00:00 | 55075.0035416667 | 2009-09-01 00:05:06 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804064010/ | Quick Look | ![]() |
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762 | ABELL 426 N4 | 49.2103 | 42.4455 | 48.378755 | 42.262141 | 58.317611 | 23.388756 | 149.57911953 | -12.77962749 | 59.999 | 55062.754837963 | 2009-08-19 18:06:58 | 55063.2460532407 | 2009-08-20 05:54:19 | 804066010 | 25.3046 | 20 | 25.3046 | 25.3065 | 0 | 25.3086 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.6295 | 21.6295 | 42.44 | 0 | PROCESSED | 57548.2829282407 | 2016-06-09 06:47:25 | 55441 | 2010-09-02 00:00:00 | 55075.0762384259 | 2009-09-01 01:49:47 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804066010/ | Quick Look | ![]() |
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763 | ABELL 1068 | 160.4236 | 39.9791 | 159.703028 | 40.240763 | 145.773983 | 29.164286 | 178.96037586 | 60.29153459 | 130.001 | 55861.8826273148 | 2011-10-27 21:10:59 | 55863.1258564815 | 2011-10-29 03:01:14 | 806028020 | 52.0056 | 50 | 52.0136 | 52.0056 | 0 | 52.0196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43.2759 | 43.2759 | 107.4038 | 1 | PROCESSED | 57603.6533333333 | 2016-08-03 15:40:48 | 55652 | 2011-04-01 00:00:00 | 55874.1687615741 | 2011-11-09 04:03:01 | 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/ver3.0/806028020/ | Quick Look | ![]() |
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764 | A262 E1 | 28.6322 | 35.9862 | 27.896259 | 35.741034 | 39.692258 | 22.636644 | 136.99532529 | -25.15665513 | 249.9998 | 56694.7928935185 | 2014-02-06 19:01:46 | 56695.3750694444 | 2014-02-07 09:00:06 | 808112010 | 25.9466 | 24 | 25.9546 | 25.9466 | 0 | 25.9626 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7986226852 | 2016-08-13 19:10:01 | 57074 | 2015-02-21 00:00:00 | 56709.7127893518 | 2014-02-21 17:06:25 | 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/ver3.0/808112010/ | Quick Look | ![]() |
765 | A76 EAST | 10.1332 | 6.8374 | 9.486956 | 6.563068 | 11.989309 | 2.27755 | 118.09579875 | -55.93191571 | 260.0024 | 55183.3444212963 | 2009-12-18 08:15:58 | 55183.8752199074 | 2009-12-18 21:00:19 | 804087010 | 23.621 | 15 | 23.637 | 23.621 | 0 | 23.629 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18.6401 | 18.6401 | 45.8559 | 0 | PROCESSED | 57549.8965393518 | 2016-06-10 21:31:01 | 55575 | 2011-01-14 00:00:00 | 55209.4624652778 | 2010-01-13 11:05:57 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042018 | In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HANS BOEHRINGER | EUR | 4 | AO4 | SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804087010/ | Quick Look | ![]() |
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766 | NGC5129 OFF-CENTER1 | 201.3141 | 14.0346 | 200.698603 | 14.294472 | 194.098163 | 21.268391 | 335.68408417 | 74.71314923 | 124.7585 | 55548.0427314815 | 2010-12-18 01:01:32 | 55548.7883101852 | 2010-12-18 18:55:10 | 805072010 | 30.2512 | 30 | 30.2512 | 30.2512 | 0 | 30.2512 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4611 | 24.4611 | 64.4119 | 0 | PROCESSED | 57554.4566203704 | 2016-06-15 10:57:32 | 55960 | 2012-02-03 00:00:00 | 55592.9994444444 | 2011-01-31 23:59:12 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | XINYU DAI | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805072010/ | Quick Look | ![]() |
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767 | MKW 4-OFFSET2 | 181.4291 | 1.9058 | 180.78864 | 2.184142 | 180.549883 | 2.316727 | 277.53009765 | 62.50090006 | 114.4199 | 55530.2508101852 | 2010-11-30 06:01:10 | 55532.2286805556 | 2010-12-02 05:29:18 | 805082010 | 82.9361 | 80 | 82.9401 | 82.9361 | 0 | 82.9441 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70.0619 | 70.0619 | 170.8541 | 2 | PROCESSED | 57554.329525463 | 2016-06-15 07:54:31 | 55910 | 2011-12-15 00:00:00 | 55544.2869328704 | 2010-12-14 06:53:11 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051525 | We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIO GASTALDELLO | USA | 5 | AO5 | THE OUTSKIRTS OF MKW 4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805082010/ | Quick Look | ![]() |
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768 | PKS 0745-191 | 117.0925 | -18.8008 | 116.536214 | -18.67521 | 123.761788 | -39.117935 | 236.11480248 | 3.4506494 | 113.9994 | 55514.1140625 | 2010-11-14 02:44:15 | 55515.1105324074 | 2010-11-15 02:39:10 | 805083010 | 37.2084 | 35 | 37.2164 | 37.2084 | 0 | 37.2164 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31.5228 | 31.5228 | 86.0879 | 1 | PROCESSED | 57554.0728703704 | 2016-06-15 01:44:56 | 55903 | 2011-12-08 00:00:00 | 55537.2095486111 | 2010-12-07 05:01:45 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805083010/ | Quick Look | ![]() |
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769 | PKS 0745-191 | 116.6522 | -19.7838 | 116.101042 | -19.660112 | 123.535239 | -40.170782 | 236.7569882 | 2.59757333 | 114.0013 | 55515.1115162037 | 2010-11-15 02:40:35 | 55516.1335416667 | 2010-11-16 03:12:18 | 805087010 | 37.9286 | 35 | 37.9526 | 37.9446 | 0 | 37.9286 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32.1037 | 32.1037 | 88.2858 | 2 | PROCESSED | 57554.1054976852 | 2016-06-15 02:31:55 | 55895 | 2011-11-30 00:00:00 | 55526.1606018518 | 2010-11-26 03:51:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATTHEW GEORGE | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805087010/ | Quick Look | ![]() |
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770 | SNR 0519-69.0 | 79.8865 | -69.038 | 79.962501 | -69.086742 | 322.357221 | -85.457085 | 279.70295655 | -33.37204199 | 53.6181 | 55782.8380324074 | 2011-08-09 20:06:46 | 55789.4030555556 | 2011-08-16 09:40:24 | 806026010 | 347.5681 | 350 | 347.5681 | 347.5761 | 0 | 347.5761 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 355.0724 | 355.0724 | 395.8115 | 7 | PROCESSED | 57602.9665740741 | 2016-08-02 23:11:52 | 55652 | 2011-04-01 00:00:00 | 55802.468900463 | 2011-08-29 11:15:13 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061102 | We propose two relatively deep observations of the young ejecta-dominated supernova remnants 0509-67.5 and 0519-69.0 in the Large Magellanic Cloud. Our goal is to seek line emission from the trace elements Mn and Cr in these remnants of Type Ia supernovae, and to measure the corresponding abundances using calculated atomic data. The relative masses of Mn and Cr produced in Type Ia supernovae are a diagnostic of the initial metallicity of the progenitor system. Of the supernovae that produced these two remnants, one had a normal luminosity, while the other was over-luminous. Together with existing data for another LMC Ia remnant, N103B, which shows evidence for circumstellar interactions, these observations will provide a broad sample of the variety seen in Ia events. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | UNA HWANG | USA | 6 | AO6-LP | ABUNDANCES OF CR AND MN AND THE PROGENITOR METALLICITY IN TWO TYPE IA MAGELLANIC CLOUD SNRS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806026010/ | Quick Look | ![]() |
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771 | ABELL 773 | 139.6885 | 51.8172 | 138.816003 | 52.028068 | 124.747961 | 34.198508 | 165.93230971 | 43.4884399 | 276.9986 | 55682.3638888889 | 2011-05-01 08:44:00 | 55683.2105902778 | 2011-05-02 05:03:15 | 806027010 | 42.5779 | 50 | 42.5859 | 42.5859 | 0 | 42.5779 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32.7052 | 32.7052 | 73.1439 | 0 | PROCESSED | 57601.9080555556 | 2016-08-01 21:47:36 | 55652 | 2011-04-01 00:00:00 | 55697.2644560185 | 2011-05-16 06:20:49 | 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/ver3.0/806027010/ | Quick Look | ![]() |
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772 | ABELL 1068 | 159.9611 | 39.9499 | 159.238834 | 40.210787 | 145.421786 | 28.986121 | 179.20513519 | 59.95740225 | 130.001 | 55864.5464583333 | 2011-10-30 13:06:54 | 55865.764849537 | 2011-10-31 18:21:23 | 806028040 | 51.1493 | 50 | 51.1573 | 51.1493 | 0 | 51.1653 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.5701 | 46.5701 | 105.2498 | 0 | PROCESSED | 57603.6525810185 | 2016-08-03 15:39:43 | 55652 | 2011-04-01 00:00:00 | 55879.1651967593 | 2011-11-14 03:57:53 | 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/ver3.0/806028040/ | Quick Look | ![]() |
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773 | COMA E5 | 196.4286 | 27.8904 | 195.829087 | 28.157796 | 182.91784 | 31.908863 | 47.28907584 | 86.74411283 | 279.9981 | 55730.3360416667 | 2011-06-18 08:03:54 | 55730.7848726852 | 2011-06-18 18:50:13 | 806034010 | 18.2706 | 20 | 18.2706 | 18.2946 | 0 | 18.2786 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.0751 | 15.0751 | 38.7599 | 0 | PROCESSED | 57602.3384259259 | 2016-08-02 08:07:20 | 55652 | 2011-04-01 00:00:00 | 55770.1405324074 | 2011-07-28 03:22:22 | 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/ver3.0/806034010/ | Quick Look | ![]() |
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774 | COMA NW4 | 194.43 | 28.912 | 193.827069 | 29.181931 | 180.525216 | 32.025522 | 85.44172027 | 87.7408795 | 319.999 | 55732.9798611111 | 2011-06-20 23:31:00 | 55733.468912037 | 2011-06-21 11:15:14 | 806041010 | 21.1196 | 20 | 21.1236 | 21.1434 | 0 | 21.1196 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.5915 | 21.5915 | 42.246 | 0 | PROCESSED | 57602.3778819444 | 2016-08-02 09:04:09 | 55652 | 2011-04-01 00:00:00 | 55768.2688888889 | 2011-07-26 06:27:12 | 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/ver3.0/806041010/ | Quick Look | ![]() |
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775 | NGC5866 | 226.5977 | 55.7554 | 226.254302 | 55.947234 | 186.820283 | 67.076445 | 92.03719886 | 52.50531538 | 352.5583 | 55701.1230092593 | 2011-05-20 02:57:08 | 55703.3466898148 | 2011-05-22 08:19:14 | 806053010 | 101.8346 | 100 | 101.8426 | 101.8346 | 0 | 101.8426 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94.7812 | 94.7812 | 192.0718 | 2 | PROCESSED | 57602.140787037 | 2016-08-02 03:22:44 | 56102 | 2012-06-24 00:00:00 | 55735.3197800926 | 2011-06-23 07:40:29 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061502 | An existing Chandra observation indicates hot gas in the S0 galaxy NGC5866 has a supersolar iron abundance and an unusually low O/Fe ratio. The galaxy is also rich in molecular gas and shows distinct vertical dusty filaments, which most likely represent cold gas blown out by SNe from the disk. We herein propose a 100ks Suzaku observation of it to better measure the hot gas properties and its spatial distribution. The energy resolution and counting statistics of the observation will enable us to greatly improve the measurement of the abundances. By further comparing such measurements among galaxies of different cold gas contents, we will investigate the effect of cold/hot gas interaction on the dynamics of the hot gas, as well as its thermal and chemical properties. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JIANG-TAO LI | USA | 6 | AO6 | X-RAY SPECTROSCOPY OF STELLAR FEEDBACK PROCESSES IN A COOL GAS-RICH S0 GALAXY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806053010/ | Quick Look | ![]() |
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776 | SPT-CL J2341-5119 | 355.3013 | -51.333 | 354.629905 | -51.610408 | 330.126015 | -44.109465 | 326.93544545 | -62.39708341 | 56.9213 | 55703.3602662037 | 2011-05-22 08:38:47 | 55706.0800810185 | 2011-05-25 01:55:19 | 806072010 | 100.2347 | 100 | 100.2427 | 100.2347 | 0 | 100.2507 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88.2081 | 88.2081 | 234.9799 | 3 | PROCESSED | 57602.1463310185 | 2016-08-02 03:30:43 | 56092 | 2012-06-14 00:00:00 | 55725.3016550926 | 2011-06-13 07:14:23 | 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/ver3.0/806072010/ | Quick Look | ![]() |
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777 | RCS044406-2820.4 | 71.0221 | -28.343 | 70.523595 | -28.434713 | 63.530115 | -50.056858 | 228.67801491 | -39.02616141 | 99.3268 | 55827.6316319444 | 2011-09-23 15:09:33 | 55828.8751736111 | 2011-09-24 21:00:15 | 806080010 | 50.6723 | 50 | 50.6723 | 50.6723 | 0 | 50.6723 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41.9027 | 41.9027 | 107.4318 | 3 | PROCESSED | 57603.2531134259 | 2016-08-03 06:04:29 | 56222 | 2012-10-22 00:00:00 | 55854.3160300926 | 2011-10-20 07:35:05 | 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/ver3.0/806080010/ | Quick Look | ![]() |
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778 | A3526 | 192.0509 | -41.0558 | 191.361267 | -40.783129 | 208.811762 | -32.67802 | 302.27518183 | 21.81182444 | 109.9986 | 55942.2296990741 | 2012-01-16 05:30:46 | 55942.6807291667 | 2012-01-16 16:20:15 | 806084010 | 16.9645 | 10 | 16.9645 | 16.9645 | 0 | 16.9645 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12.6605 | 12.6605 | 38.9639 | 0 | PROCESSED | 57604.361875 | 2016-08-04 08:41:06 | 56331 | 2013-02-08 00:00:00 | 55960.1781712963 | 2012-02-03 04:16:34 | 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/ver3.0/806084010/ | Quick Look | ![]() |
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779 | ABELL 426 SE7 | 51.6308 | 40.0717 | 50.808198 | 39.897364 | 59.505151 | 20.607904 | 152.49041219 | -13.73591885 | 87.5626 | 55800.376875 | 2011-08-27 09:02:42 | 55800.6418055556 | 2011-08-27 15:24:12 | 806122010 | 10.3288 | 10 | 10.3288 | 10.3288 | 0 | 10.3288 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.822 | 9.822 | 22.8839 | 0 | PROCESSED | 57602.977337963 | 2016-08-02 23:27:22 | 55652 | 2011-04-01 00:00:00 | 55865.0862731482 | 2011-10-31 02:04:14 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806122010/ | Quick Look | ![]() |
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780 | ABELL 426 NE5 | 51.4212 | 42.371 | 50.583845 | 42.195846 | 60.001331 | 22.866197 | 151.01253218 | -11.93716766 | 89.4976 | 55810.0456481482 | 2011-09-06 01:05:44 | 55810.5418287037 | 2011-09-06 13:00:14 | 806130010 | 17.5276 | 15 | 17.5276 | 17.5356 | 0 | 17.5356 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17.7802 | 17.7802 | 42.862 | 0 | PROCESSED | 57603.0838888889 | 2016-08-03 02:00:48 | 55652 | 2011-04-01 00:00:00 | 55866.1625925926 | 2011-11-01 03:54:08 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806130010/ | Quick Look | ![]() |
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781 | ABELL 426 NE6.5 | 51.8822 | 42.6245 | 51.041802 | 42.451087 | 60.430729 | 23.019323 | 151.15044966 | -11.53522591 | 89.4983 | 55811.0317939815 | 2011-09-07 00:45:47 | 55811.396712963 | 2011-09-07 09:31:16 | 806133010 | 10.2804 | 10 | 10.2959 | 10.2879 | 0 | 10.2804 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.7277 | 13.7277 | 31.5259 | 0 | PROCESSED | 57603.0893634259 | 2016-08-03 02:08:41 | 55652 | 2011-04-01 00:00:00 | 55866.233587963 | 2011-11-01 05:36:22 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806133010/ | Quick Look | ![]() |
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782 | N4438 TAIL | 186.7653 | 12.9509 | 186.13191 | 13.227515 | 180.954769 | 14.552434 | 279.81897455 | 74.71807646 | 119.2941 | 56636.4959259259 | 2013-12-10 11:54:08 | 56639.0884259259 | 2013-12-13 02:07:20 | 808045010 | 102.7738 | 100 | 102.7738 | 102.7738 | 0 | 102.7738 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92.8342 | 92.8342 | 223.962 | 2 | PROCESSED | 57613.6203587963 | 2016-08-13 14:53:19 | 57016 | 2014-12-25 00:00:00 | 56650.8089583333 | 2013-12-24 19:24:54 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080059 | We propose a 100 ks XIS observation to the Halpha/X-ray filament connecting N4438 and M86 in the Virgo cluster. Our main objective is to probe conclusively the OVII line which is marginally detected with the XMM-Newton. If established, by employing line diagnostic and non-equilibrium ionization analysis, we will be able to determine the ionization temperature and elapsed timescale of the multi-phase ISM stripped from N4438, and give constraint on the thermal conductivity and metal enrichment of the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LIYI GU | JAP | 8 | AO8 | A SUZAKU OBSERVATION OF ONGOING IONIZATION OF ISM IN THE VIRGO CLUSTER ICM | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808045010/ | Quick Look | ![]() |
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783 | SDSS J0906+0301 | 136.6571 | 3.0284 | 136.006 | 3.229773 | 138.178094 | -12.954149 | 226.89088068 | 31.22930355 | 109.9836 | 56253.2318981482 | 2012-11-22 05:33:56 | 56253.846099537 | 2012-11-22 20:18:23 | 807059010 | 21.7148 | 20 | 21.7228 | 21.7148 | 0 | 21.7228 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.632 | 20.632 | 53.066 | 0 | PROCESSED | 57608.0815972222 | 2016-08-08 01:57:30 | 56702 | 2014-02-14 00:00:00 | 56336.4694328704 | 2013-02-13 11:15:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807059010/ | Quick Look | ![]() |
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784 | SDSS J1431+0047 | 217.7608 | 0.788 | 217.122744 | 1.009037 | 215.129123 | 14.8431 | 349.30444711 | 54.43383912 | 287.7594 | 56140.9857291667 | 2012-08-01 23:39:27 | 56141.454375 | 2012-08-02 10:54:18 | 807062010 | 22.3553 | 20 | 22.371 | 22.3553 | 0 | 22.363 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16.5809 | 16.5809 | 40.4799 | 1 | PROCESSED | 57606.7190740741 | 2016-08-06 17:15:28 | 56528 | 2013-08-24 00:00:00 | 56162.1265972222 | 2012-08-23 03:02:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ERIC MILLER | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807062010/ | Quick Look | ![]() |
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785 | ABELL 2597 | 351.4175 | -11.9496 | 350.767566 | -12.224675 | 347.389222 | -7.579212 | 65.78537526 | -64.80325971 | 249.1017 | 56261.057650463 | 2012-11-30 01:23:01 | 56262.3299768518 | 2012-12-01 07:55:10 | 807073010 | 51.0526 | 50 | 51.0566 | 51.0674 | 0 | 51.0526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46.3613 | 46.3613 | 109.9139 | 1 | PROCESSED | 57608.180462963 | 2016-08-08 04:19:52 | 56018 | 2012-04-01 00:00:00 | 56278.743587963 | 2012-12-17 17:50:46 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 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 previous cycles, 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 | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807073010/ | Quick Look | ![]() |
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786 | HYDRA A FAR N | 139.5397 | -11.7599 | 138.936601 | -11.549023 | 146.034406 | -26.083857 | 242.64361193 | 25.31151573 | 300.0007 | 56083.9377430556 | 2012-06-05 22:30:21 | 56085.1452662037 | 2012-06-07 03:29:11 | 807089010 | 41.276 | 40 | 41.284 | 41.284 | 0 | 41.276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38.1727 | 38.1727 | 104.3117 | 1 | PROCESSED | 57605.6201851852 | 2016-08-05 14:53:04 | 56465 | 2013-06-22 00:00:00 | 56098.4661689815 | 2012-06-20 11:11:17 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807089010/ | Quick Look | ![]() |
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787 | VIRGO W3 | 186.9593 | 11.946 | 186.325534 | 12.222509 | 181.555181 | 13.711892 | 281.75004157 | 73.83934761 | 99.9993 | 56273.4086921296 | 2012-12-12 09:48:31 | 56273.6403472222 | 2012-12-12 15:22:06 | 807096010 | 10.8424 | 10 | 10.8504 | 10.8504 | 0 | 10.8424 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9.0921 | 9.0921 | 20.0079 | 0 | PROCESSED | 57608.2529282407 | 2016-08-08 06:04:13 | 56018 | 2012-04-01 00:00:00 | 56342.4989699074 | 2013-02-19 11:58:31 | 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/ver3.0/807096010/ | Quick Look | ![]() |
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788 | VIRGO S7 | 187.6096 | 10.2244 | 186.9754 | 10.500529 | 182.869873 | 12.396474 | 285.61941254 | 72.38660135 | 308.5009 | 56113.0805092593 | 2012-07-05 01:55:56 | 56113.4293518518 | 2012-07-05 10:18:16 | 807121010 | 14.9979 | 13 | 14.9979 | 14.9979 | 0 | 14.9979 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.746 | 15.746 | 30.1359 | 0 | PROCESSED | 57606.5659606482 | 2016-08-06 13:34:59 | 56018 | 2012-04-01 00:00:00 | 56141.9783101852 | 2012-08-02 23:28:46 | 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/ver3.0/807121010/ | Quick Look | ![]() |
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789 | A399&A401 FILAMENT | 44.5739 | 13.3044 | 43.887717 | 13.104923 | 46.011939 | -3.472452 | 164.23302583 | -39.1861165 | 71.9992 | 56522.5065972222 | 2013-08-18 12:09:30 | 56523.421724537 | 2013-08-19 10:07:17 | 808005010 | 42.1655 | 40 | 42.1655 | 42.1655 | 0 | 42.1655 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40.981 | 40.981 | 79.0638 | 2 | PROCESSED | 57612.3602083333 | 2016-08-12 08:38:42 | 56956 | 2014-10-26 00:00:00 | 56587.6829398148 | 2013-10-22 16:23:26 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOSHITAKA ISHISAKI | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808005010/ | Quick Look | ![]() |
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790 | A2255_SE | 258.2963 | 63.8192 | 258.210545 | 63.875842 | 203.735886 | 84.382935 | 93.63129587 | 34.92006939 | 200.0025 | 56613.9474537037 | 2013-11-17 22:44:20 | 56615.3084953704 | 2013-11-19 07:24:14 | 808040010 | 64.733 | 60 | 64.741 | 64.741 | 0 | 64.733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8865 | 64.8865 | 117.5879 | 1 | PROCESSED | 57613.3519097222 | 2016-08-13 08:26:45 | 57029 | 2015-01-07 00:00:00 | 56653.6890046296 | 2013-12-27 16:32:10 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080047 | We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HIROKO YOSHIDA | JAP | 8 | AO8 | MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808040010/ | Quick Look | ![]() |
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791 | 3C390.3_VICINITY_2 | 284.1264 | 79.7065 | 284.963939 | 79.636578 | 79.391227 | 76.323687 | 111.42410994 | 26.43157038 | 239.9994 | 56608.493900463 | 2013-11-12 11:51:13 | 56609.4897222222 | 2013-11-13 11:45:12 | 808047010 | 52.8856 | 50 | 52.9066 | 52.8936 | 0 | 52.8856 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48.4013 | 48.4013 | 86.0319 | 0 | PROCESSED | 57613.3036111111 | 2016-08-13 07:17:12 | 56991 | 2014-11-30 00:00:00 | 56625.7010648148 | 2013-11-29 16:49:32 | 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/ver3.0/808047010/ | Quick Look | ![]() |
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792 | NGC1550_45OFFSET_E | 65.5544 | 2.4106 | 64.903424 | 2.293944 | 64.093741 | -18.859585 | 191.40103429 | -31.31407553 | 260.0002 | 56696.1115393518 | 2014-02-08 02:40:37 | 56697.3543634259 | 2014-02-09 08:30:17 | 808060010 | 53.0496 | 50 | 53.0496 | 53.0496 | 0 | 53.0496 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8049421296 | 2016-08-13 19:19:07 | 57075 | 2015-02-22 00:00:00 | 56709.7114351852 | 2014-02-21 17:04:28 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080110 | We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TORU SASAKI | JAP | 8 | AO8 | STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808060010/ | Quick Look | ![]() |
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793 | VIRGO E3 | 188.6166 | 12.8387 | 187.985199 | 13.11416 | 182.706731 | 15.185969 | 286.56417369 | 75.16845975 | 284.999 | 56481.9598032407 | 2013-07-08 23:02:07 | 56482.2154861111 | 2013-07-09 05:10:18 | 808118010 | 12.3275 | 10 | 12.3355 | 12.3355 | 0 | 12.3275 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.334 | 10.334 | 22.0879 | 0 | PROCESSED | 57611.7501851852 | 2016-08-11 18:00:16 | 56383 | 2013-04-01 00:00:00 | 56495.6160185185 | 2013-07-22 14:47:04 | 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/ver3.0/808118010/ | Quick Look | ![]() |
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794 | THE MOON | 141.5744 | 9.879 | 140.90311 | 10.096072 | 140.776608 | -4.942339 | 222.40545014 | 38.80103529 | 285.4041 | 56784.4506712963 | 2014-05-07 10:48:58 | 56784.5827662037 | 2014-05-07 13:59:11 | 809001080 | 5.6107 | 45 | 5.6107 | 5.6107 | 0 | 5.6107 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5.507 | 5.507 | 11.3919 | 0 | PROCESSED | 57615.0708217593 | 2016-08-15 01:41:59 | 57220 | 2015-07-17 00:00:00 | 56854.5770717593 | 2014-07-16 13:50:59 | 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/ver3.0/809001080/ | Quick Look | ![]() |
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795 | THE MOON | 22.6503 | 9.5807 | 21.992046 | 9.323163 | 24.491955 | 0.094055 | 138.76659478 | -52.08288303 | 73.7999 | 56856.8890277778 | 2014-07-18 21:20:12 | 56857.0196412037 | 2014-07-19 00:28:17 | 809001130 | 5.3017 | 45 | 5.3017 | 5.3017 | 0 | 5.3017 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4036574074 | 2016-08-15 09:41:16 | 57267 | 2015-09-02 00:00:00 | 56902.5802314815 | 2014-09-02 13:55:32 | 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/ver3.0/809001130/ | Quick Look | ![]() |
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796 | THE MOON | 26.0744 | 9.9879 | 25.412732 | 9.737134 | 27.784882 | -0.749126 | 143.76867514 | -50.73288629 | 73.7996 | 56857.1528472222 | 2014-07-19 03:40:06 | 56857.2765856482 | 2014-07-19 06:38:17 | 809001150 | 3.9169 | 45 | 3.9169 | 3.9169 | 0 | 3.9169 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4069097222 | 2016-08-15 09:45:57 | 57235 | 2015-08-01 00:00:00 | 56869.6125925926 | 2014-07-31 14:42:08 | 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/ver3.0/809001150/ | Quick Look | ![]() |
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797 | THE MOON | 147.1957 | 8.7504 | 146.531357 | 8.983511 | 146.407447 | -4.210959 | 227.18440299 | 43.16589995 | 105.6994 | 56975.9388541667 | 2014-11-14 22:31:57 | 56976.0626388889 | 2014-11-15 01:30:12 | 809001260 | 6.33 | 45 | 6.33 | 6.442 | 0 | 6.442 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7804513889 | 2016-08-16 18:43:51 | 57359 | 2015-12-03 00:00:00 | 56992.418587963 | 2014-12-01 10:02:46 | 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/ver3.0/809001260/ | Quick Look | ![]() |
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798 | THE MOON | 333.6436 | -6.6185 | 332.98809 | -6.867271 | 333.149604 | 3.9961 | 54.50784287 | -47.51853169 | 249.2061 | 56990.1023958333 | 2014-11-29 02:27:27 | 56990.2084837963 | 2014-11-29 05:00:13 | 809001300 | 3.8788 | 45 | 3.8828 | 3.8788 | 0 | 3.8868 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4075115741 | 2016-08-17 09:46:49 | 57415 | 2016-01-28 00:00:00 | 57049.4536805556 | 2015-01-27 10:53:18 | 3.0.22.44 | 3 | 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/ver3.0/809001300/ | Quick Look | ![]() |
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799 | THE MOON | 339.1671 | -5.6557 | 338.516198 | -5.915354 | 338.624224 | 2.887463 | 60.63287277 | -51.42821416 | 248.2317 | 56990.4856828704 | 2014-11-29 11:39:23 | 56990.608587963 | 2014-11-29 14:36:22 | 809001330 | 6.3646 | 45 | 6.3646 | 6.3646 | 0 | 6.3646 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4115856482 | 2016-08-17 09:52:41 | 57415 | 2016-01-28 00:00:00 | 57006.4031018518 | 2014-12-15 09:40:28 | 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/ver3.0/809001330/ | Quick Look | ![]() |
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800 | RXJ1159+5531 E | 180.1946 | 55.5211 | 179.553068 | 55.799424 | 150.053445 | 49.203071 | 137.37799324 | 60.16358606 | 301.575 | 56806.5416550926 | 2014-05-29 12:59:59 | 56808.2502430556 | 2014-05-31 06:00:21 | 809063010 | 99.1618 | 100 | 99.1778 | 99.1618 | 0 | 99.1778 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1713657407 | 2016-08-15 04:06:46 | 57234 | 2015-07-31 00:00:00 | 56866.7150925926 | 2014-07-28 17:09:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091521 | In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YUANYUAN SU | USA | 9 | AO9 | MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809063010/ | Quick Look | ![]() |
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801 | ABELL 98-CENTER | 11.6247 | 20.5572 | 10.963731 | 20.284211 | 18.829002 | 14.307964 | 121.3687084 | -42.29955696 | 80.8972 | 56837.6648726852 | 2014-06-29 15:57:25 | 56839.2014236111 | 2014-07-01 04:50:03 | 809077010 | 60.781 | 60 | 60.781 | 60.917 | 0 | 60.925 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3554282407 | 2016-08-15 08:31:49 | 56748 | 2014-04-01 00:00:00 | 56854.7844212963 | 2014-07-16 18:49:34 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809077010/ | Quick Look | ![]() |
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802 | ABELL 98-WEST | 11.3131 | 20.6695 | 10.652564 | 20.396219 | 18.599995 | 14.528185 | 120.97936172 | -42.17879703 | 80.8359 | 56841.9624537037 | 2014-07-03 23:05:56 | 56844.7606712963 | 2014-07-06 18:15:22 | 809079010 | 96.6924 | 100 | 96.6924 | 100.6438 | 0 | 100.6598 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3882638889 | 2016-08-15 09:19:06 | 56748 | 2014-04-01 00:00:00 | 56881.441724537 | 2014-08-12 10:36:05 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SCOTT RANDALL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809079010/ | Quick Look | ![]() |
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803 | MKW8 | 220.1793 | 3.4582 | 219.549704 | 3.671881 | 216.616533 | 18.149831 | 355.49716412 | 54.76401984 | 291.2239 | 56859.4682986111 | 2014-07-21 11:14:21 | 56859.7009259259 | 2014-07-21 16:49:20 | 809101010 | 10.412 | 10 | 10.412 | 10.488 | 0 | 10.4956 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4174305556 | 2016-08-15 10:01:06 | 57239 | 2015-08-05 00:00:00 | 56873.5532523148 | 2014-08-04 13:16:41 | 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 | B | 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/ver3.0/809101010/ | Quick Look | ![]() |
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804 | ZWCL0008.8+5215 EAST | 3.1134 | 52.6387 | 2.455083 | 52.360692 | 29.755774 | 45.738765 | 116.94843434 | -9.77955026 | 65.9987 | 56844.7667939815 | 2014-07-06 18:24:11 | 56847.5876273148 | 2014-07-09 14:06:11 | 809118010 | 117.8473 | 120 | 117.8473 | 119.9094 | 0 | 119.9334 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3793518518 | 2016-08-15 09:06:16 | 56748 | 2014-04-01 00:00:00 | 56859.7336111111 | 2014-07-21 17:36:24 | 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/ver3.0/809118010/ | Quick Look | ![]() |
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805 | EN2-109 | 248.6774 | 40.3802 | 248.257276 | 40.482344 | 234.834061 | 61.240527 | 64.11782178 | 42.55568423 | 145.2754 | 55927.5063425926 | 2012-01-01 12:09:08 | 55929.8577314815 | 2012-01-03 20:35:08 | 806075010 | 108.616 | 100 | 108.632 | 108.616 | 0 | 108.64 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 0.571 | 0.571 | 0.5729 | 0 | PROCESSED | 57604.2767592593 | 2016-08-04 06:38:32 | 56065 | 2012-05-18 00:00:00 | 55946.1449537037 | 2012-01-20 03:28:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806075010/ | Quick Look | ![]() |
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806 | ES1-230 | 9.1906 | -44.1805 | 8.591944 | -44.455632 | 346.325718 | -43.236883 | 311.80619624 | -72.69400023 | 239.5046 | 55907.020787037 | 2011-12-12 00:29:56 | 55907.8925694444 | 2011-12-12 21:25:18 | 806076010 | 44.8024 | 40 | 44.8024 | 44.8024 | 0 | 44.8024 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52.0193 | 52.0193 | 75.3199 | 0 | PROCESSED | 57604.1212037037 | 2016-08-04 02:54:32 | 56065 | 2012-05-18 00:00:00 | 55920.9678587963 | 2011-12-25 23:13:43 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806076010/ | Quick Look | ![]() |
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807 | FORNAX CLUSTER NORTH | 54.7022 | -35.2276 | 54.222066 | -35.389468 | 38.999643 | -52.605839 | 236.33819165 | -53.57399329 | 245.0013 | 53740.3046990741 | 2006-01-05 07:18:46 | 53740.493275463 | 2006-01-05 11:50:19 | 800002010 | 7.7635 | 80 | 7.7635 | 7.7635 | 7.7635 | 7.7635 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8.2708 | 8.2708 | 16.2719 | 0 | PROCESSED | 57532.6205324074 | 2016-05-24 14:53:34 | 54247 | 2007-05-27 00:00:00 | 54039.6718518518 | 2006-10-31 16:07:28 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KYOKO MATSUSHITA | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800002010/ | Quick Look | ![]() |
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808 | ABELL 426 SE1 | 50.1688 | 41.3334 | 49.341889 | 41.153578 | 58.72404 | 22.121633 | 150.81714435 | -13.31934713 | 89.5646 | 55797.4683912037 | 2011-08-24 11:14:29 | 55797.7113194444 | 2011-08-24 17:04:18 | 806111010 | 10.8099 | 10 | 10.8099 | 10.8099 | 0 | 10.8099 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10.3733 | 10.3733 | 20.9879 | 0 | PROCESSED | 57602.9312268518 | 2016-08-02 22:20:58 | 55652 | 2011-04-01 00:00:00 | 55855.1291550926 | 2011-10-21 03:05:59 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806111010/ | Quick Look | ![]() |
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809 | ABELL 426 NNE2.5 | 50.1251 | 42.1872 | 49.292647 | 42.007206 | 58.945293 | 22.951312 | 150.30450115 | -12.62617945 | 60.4949 | 55804.3102083333 | 2011-08-31 07:26:42 | 55804.5820833333 | 2011-08-31 13:58:12 | 806137010 | 10.5444 | 10 | 10.5444 | 10.5444 | 0 | 10.5444 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9.962 | 9.962 | 23.4721 | 0 | PROCESSED | 57603.0188773148 | 2016-08-03 00:27:11 | 55652 | 2011-04-01 00:00:00 | 55830.2163888889 | 2011-09-26 05:11:36 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806137010/ | Quick Look | ![]() |
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810 | ABELL 426 NNE5.5 | 50.3796 | 43.0058 | 49.54083 | 42.82674 | 59.388281 | 23.686025 | 150.00098645 | -11.84054635 | 60.4963 | 55806.8935300926 | 2011-09-02 21:26:41 | 55807.3024074074 | 2011-09-03 07:15:28 | 806143010 | 16.4506 | 15 | 16.4727 | 16.4666 | 0 | 16.4506 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.6975 | 11.6975 | 35.3199 | 1 | PROCESSED | 57603.0430208333 | 2016-08-03 01:01:57 | 55652 | 2011-04-01 00:00:00 | 55845.2820486111 | 2011-10-11 06:46:09 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806143010/ | Quick Look | ![]() |
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811 | A262 NE4 | 28.8115 | 37.1901 | 28.070704 | 36.945344 | 40.33412 | 23.695949 | 136.79382783 | -23.95810874 | 249.9999 | 56704.7992476852 | 2014-02-16 19:10:55 | 56705.5321064815 | 2014-02-17 12:46:14 | 808111010 | 30.9305 | 30 | 30.9625 | 30.9305 | 0 | 30.9625 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 27.8027 | 27.8027 | 63.3119 | 2 | PROCESSED | 57613.8474652778 | 2016-08-13 20:20:21 | 57085 | 2015-03-04 00:00:00 | 56719.7343981482 | 2014-03-03 17:37:32 | 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 | A | 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/ver3.0/808111010/ | Quick Look | ![]() |
812 | A1060 OFFSET | 159.5124 | -27.532 | 158.922997 | -27.271679 | 173.074389 | -33.196781 | 269.88117164 | 26.64663217 | 96.4857 | 53694.9817708333 | 2005-11-20 23:33:45 | 53696.6231365741 | 2005-11-22 14:57:19 | 800004010 | 52.4025 | 60 | 52.4025 | 53.2025 | 52.4185 | 52.5385 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46.2039 | 46.2039 | 141.8018 | 1 | PROCESSED | 57528.0764583333 | 2016-05-20 01:50:06 | 54247 | 2007-05-27 00:00:00 | 54038.1216666667 | 2006-10-30 02:55:12 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001021 | A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAKAYA OHASHI | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800004010/ | Quick Look | ![]() |
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813 | COMA SUBHALO4 | 193.8668 | 27.5167 | 193.260337 | 27.78729 | 180.744108 | 30.556584 | 56.62578598 | 89.02439779 | 314.9971 | 56453.5916666667 | 2013-06-10 14:12:00 | 56454.1370717593 | 2013-06-11 03:17:23 | 808022010 | 23.8091 | 20 | 23.8091 | 23.8331 | 0 | 23.8171 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19.6195 | 19.6195 | 47.1139 | 0 | PROCESSED | 57611.5223958333 | 2016-08-11 12:32:15 | 56830 | 2014-06-22 00:00:00 | 56464.6326041667 | 2013-06-21 15:10:57 | 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/ver3.0/808022010/ | Quick Look | ![]() |
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814 | A426VIR E | 49.1256 | 42.621 | 48.293128 | 42.437331 | 58.306623 | 23.574763 | 149.42807458 | -12.66566367 | 271.4976 | 56709.0457986111 | 2014-02-21 01:05:57 | 56709.5683101852 | 2014-02-21 13:38:22 | 808086010 | 25.3703 | 25 | 25.3823 | 25.3703 | 0 | 25.3703 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.322 | 24.322 | 45.14 | 1 | PROCESSED | 57613.8778935185 | 2016-08-13 21:04:10 | 57141 | 2015-04-29 00:00:00 | 56764.7643171296 | 2014-04-17 18:20:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ONDREJ URBAN | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808086010/ | Quick Look | ![]() |
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815 | A85 | 10.4739 | -9.4292 | 9.841504 | -9.703266 | 5.843917 | -12.80705 | 115.23010576 | -72.15810594 | 248.2856 | 54105.4020023148 | 2007-01-05 09:38:53 | 54108.0557175926 | 2007-01-08 01:20:14 | 801041010 | 99.2012 | 100 | 99.2012 | 99.2012 | 0 | 99.2012 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84.8139 | 84.8139 | 229.2421 | 2 | PROCESSED | 57536.5180671296 | 2016-05-28 12:26:01 | 54735 | 2008-09-26 00:00:00 | 54132.9388773148 | 2007-02-01 22:31:59 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010088 | We propose observations of A2199 and A85 clusters of galaxies with an each exposure time of 100 ks, in order to search for excess hard X-ray emission, to constrain the spectral shape, and to discuss the origin of the hard X-ray emission. Both are listed as the clusters which are detected non-thermal emission signal with 2 sigma confidence level by Beppo SAX PDS detector. In addition, these two clusters only have features of brighter X-ray flux, good size, relatively cool ICM temperature, and including no bright member AGNs. Therefore they are suitable target samples for our observational purpose about estimation photon index and flux for the excess hard X-ray emission with high significance wherever possible. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RYO SHIBATA | JAP | 1 | AO1 | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS | HXD | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801041010/ | Quick Look | ![]() |
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816 | PERSEUS OFFSET-G | 50.3247 | 41.3807 | 49.497049 | 41.201455 | 58.859538 | 22.134977 | 150.89015689 | -13.2150361 | 270.0001 | 55596.3541550926 | 2011-02-04 08:29:59 | 55596.8335648148 | 2011-02-04 20:00:20 | 805047010 | 19.6768 | 25 | 19.7008 | 19.6928 | 0 | 19.6768 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.192 | 13.192 | 41.4119 | 1 | PROCESSED | 57600.8412731482 | 2016-07-31 20:11:26 | 55979 | 2012-02-22 00:00:00 | 55613.0840856482 | 2011-02-21 02:01:05 | 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/ver3.0/805047010/ | Quick Look | ![]() |
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817 | ABELL 115 OFFSET | 13.7779 | 26.1853 | 13.1056 | 25.914555 | 23.090334 | 18.655077 | 123.95957255 | -36.67911837 | 45.0019 | 55399.3766666667 | 2010-07-22 09:02:24 | 55401.6050115741 | 2010-07-24 14:31:13 | 805078010 | 101.8065 | 100 | 101.8065 | 101.8065 | 0 | 101.8065 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91.1134 | 91.1134 | 192.5058 | 3 | PROCESSED | 57552.7084259259 | 2016-06-13 17:00:08 | 55779 | 2011-08-06 00:00:00 | 55413.4333449074 | 2010-08-05 10:24:01 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051521 | We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCOTT RANDALL | USA | 5 | AO5 | THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/805078010/ | Quick Look | ![]() |
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818 | ABELL 426 SE2 | 50.4145 | 41.1258 | 49.588274 | 40.946892 | 58.854329 | 21.871316 | 151.09363465 | -13.389164 | 89.5623 | 55797.7118402778 | 2011-08-24 17:05:03 | 55797.9342824074 | 2011-08-24 22:25:22 | 806112010 | 10.8343 | 10 | 10.8383 | 10.8343 | 0 | 10.8423 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6496 | 10.6496 | 19.21 | 0 | PROCESSED | 57602.9407175926 | 2016-08-02 22:34:38 | 55652 | 2011-04-01 00:00:00 | 55855.1191782407 | 2011-10-21 02:51:37 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806112010/ | Quick Look | ![]() |
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819 | A2199 OFFSET12 | 246.9232 | 39.9293 | 246.496885 | 40.039337 | 232.503258 | 60.398142 | 63.45171294 | 43.88430519 | 267.9996 | 55820.7013657407 | 2011-09-16 16:49:58 | 55821.2488078704 | 2011-09-17 05:58:17 | 806158010 | 23.5902 | 20 | 23.5902 | 23.5902 | 0 | 23.5902 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22.1544 | 22.1544 | 47.2919 | 0 | PROCESSED | 57603.1801851852 | 2016-08-03 04:19:28 | 55652 | 2011-04-01 00:00:00 | 55865.2446412037 | 2011-10-31 05:52:17 | 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/ver3.0/806158010/ | Quick Look | ![]() |
820 | ANTLIA EB | 160.0852 | -35.3304 | 159.51241 | -35.06908 | 178.137624 | -39.871032 | 274.84198608 | 20.29194272 | 279.6006 | 56096.5981828704 | 2012-06-18 14:21:23 | 56097.8197106482 | 2012-06-19 19:40:23 | 807071010 | 45.7475 | 45 | 45.7635 | 45.7475 | 0 | 45.7635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40.3619 | 40.3619 | 105.536 | 1 | PROCESSED | 57605.7231481482 | 2016-08-05 17:21:20 | 56477 | 2013-07-04 00:00:00 | 56111.1019328704 | 2012-07-03 02:26:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. 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 test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KA-WAH WONG | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807071010/ | Quick Look | ![]() |
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821 | J2218.2-0350 | 334.573 | -3.8385 | 333.923892 | -4.08927 | 335.019924 | 6.258076 | 58.63251599 | -46.67973864 | 268.0005 | 56260.6621527778 | 2012-11-29 15:53:30 | 56261.0523148148 | 2012-11-30 01:15:20 | 807084010 | 15.7671 | 15 | 15.7751 | 15.7671 | 0 | 15.7831 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11.9145 | 11.9145 | 33.7079 | 0 | PROCESSED | 57608.1412384259 | 2016-08-08 03:23:23 | 56644 | 2013-12-18 00:00:00 | 56275.6610300926 | 2012-12-14 15:51:53 | 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/ver3.0/807084010/ | Quick Look | ![]() |
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822 | FORNAX A EAST LOBE | 51.0149 | -37.2799 | 50.539015 | -37.455999 | 33.113805 | -53.302729 | 240.23704173 | -56.41225665 | 91.5022 | 56506.6358564815 | 2013-08-02 15:15:38 | 56510.623125 | 2013-08-06 14:57:18 | 808043010 | 151.4626 | 150 | 151.4866 | 151.4626 | 0 | 151.4946 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134.0942 | 134.0942 | 344.4353 | 3 | PROCESSED | 57612.2277777778 | 2016-08-12 05:28:00 | 56955 | 2014-10-25 00:00:00 | 56587.7734259259 | 2013-10-22 18:33:44 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080056 | We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 8 | AO8 | COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808043010/ | Quick Look | ![]() |
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823 | ABELL 3112 | 49.4972 | -44.2507 | 49.062824 | -44.43238 | 25.520697 | -58.972198 | 252.95338075 | -56.0704995 | 43.5006 | 56468.5418171296 | 2013-06-25 13:00:13 | 56469.5834259259 | 2013-06-26 14:00:08 | 808068020 | 65.3977 | 200 | 65.4057 | 65.4057 | 0 | 65.3977 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54.0744 | 54.0744 | 89.9838 | 1 | PROCESSED | 57611.633912037 | 2016-08-11 15:12:50 | 56848 | 2014-07-10 00:00:00 | 56481.7677083333 | 2013-07-08 18:25:30 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081522 | 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 | USA | 8 | AO8 | CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/808068020/ | Quick Look | ![]() |
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824 | THE MOON | 148.554 | 8.0651 | 147.892313 | 8.301757 | 147.907786 | -4.401986 | 228.92553687 | 43.99318882 | 105.699 | 56976.0638541667 | 2014-11-15 01:31:57 | 56976.1876388889 | 2014-11-15 04:30:12 | 809001270 | 5.9536 | 45 | 5.9536 | 5.9616 | 0 | 5.9616 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7826967593 | 2016-08-16 18:47:05 | 57359 | 2015-12-03 00:00:00 | 56992.4196527778 | 2014-12-01 10:04:18 | 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/ver3.0/809001270/ | Quick Look | ![]() |
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825 | CEN_A_LOBE_N3 | 200.614 | -42.0794 | 199.886702 | -41.818146 | 216.080144 | -30.721221 | 309.06646515 | 20.4225822 | 293.3211 | 56862.6955439815 | 2014-07-24 16:41:35 | 56864.2709722222 | 2014-07-26 06:30:12 | 809004010 | 51.4894 | 50 | 51.4894 | 51.4894 | 0 | 51.4894 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.6384 | 10.6384 | 21.48 | 0 | PROCESSED | 57615.4562384259 | 2016-08-15 10:56:59 | 57242 | 2015-08-08 00:00:00 | 56875.2082175926 | 2014-08-06 04:59:50 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HIROMI SETA | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809004010/ | Quick Look | ![]() |
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826 | CENCL OFFSET1 | 192.2015 | -41.4461 | 191.510562 | -41.173577 | 209.146138 | -32.971575 | 302.40210867 | 21.42294125 | 106.2765 | 53732.1811689815 | 2005-12-28 04:20:53 | 53733.2502199074 | 2005-12-29 06:00:19 | 800015010 | 44.8802 | 40 | 44.8962 | 44.9042 | 44.8802 | 44.9196 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37.2267 | 37.2267 | 92.3478 | 2 | PROCESSED | 57532.5827893518 | 2016-05-24 13:59:13 | 54247 | 2007-05-27 00:00:00 | 54039.5403472222 | 2006-10-31 12:58:06 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YASUSHI FUKAZAWA | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/800015010/ | Quick Look | ![]() |
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827 | N1550_CENTER | 64.9488 | 2.4105 | 64.297881 | 2.291179 | 63.464463 | -18.753248 | 191.00239213 | -31.81480775 | 89.9981 | 54694.185474537 | 2008-08-16 04:27:05 | 54696.3009143518 | 2008-08-18 07:13:19 | 803017010 | 83.2702 | 80 | 83.7102 | 83.2702 | 0 | 83.7102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64.8874 | 64.8874 | 182.756 | 4 | PROCESSED | 57543.367974537 | 2016-06-04 08:49:53 | 55080 | 2009-09-06 00:00:00 | 54713.2652546296 | 2008-09-04 06:21:58 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030070 | We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KOSUKE SATO | JAP | 3 | AO3 | OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803017010/ | Quick Look | ![]() |
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828 | A262 NE3 | 28.6712 | 36.9514 | 27.931716 | 36.706321 | 40.12197 | 23.517818 | 136.74540455 | -24.21802206 | 250.0003 | 56703.8826388889 | 2014-02-15 21:11:00 | 56704.7987731482 | 2014-02-16 19:10:14 | 808110010 | 40.4903 | 40 | 40.5134 | 40.4903 | 0 | 40.4966 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.2624 | 34.2624 | 69.899 | 1 | PROCESSED | 57613.8476041667 | 2016-08-13 20:20:33 | 57081 | 2015-02-28 00:00:00 | 56715.76 | 2014-02-27 18:14:24 | 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 | A | 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/ver3.0/808110010/ | Quick Look | ![]() |
829 | A963E | 154.4148 | 39.0556 | 153.674896 | 39.305871 | 141.440839 | 26.400688 | 182.51717965 | 55.95361494 | 109.3314 | 54427.8082060185 | 2007-11-23 19:23:49 | 54428.4745833333 | 2007-11-24 11:23:24 | 802011010 | 29.0825 | 25 | 29.0825 | 29.0825 | 0 | 29.0825 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24.4699 | 24.4699 | 57.5679 | 0 | PROCESSED | 57540.5746412037 | 2016-06-01 13:47:29 | 54804 | 2008-12-04 00:00:00 | 54434.1859837963 | 2007-11-30 04:27:49 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020018 | 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 10% precision in a few arcmin scale, which has not been done before to any cluster. 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 | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802011010/ | Quick Look | ![]() |
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830 | NGC 253 OFFSET | 12.0926 | -25.0475 | 11.478671 | -25.320084 | 0.364314 | -27.643554 | 104.44696227 | -87.8082396 | 247.2843 | 54829.0152430556 | 2008-12-29 00:21:57 | 54830.2502430556 | 2008-12-30 06:00:21 | 803004010 | 56.7104 | 50 | 56.7104 | 56.7104 | 0 | 56.7104 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51.3026 | 51.3026 | 106.6718 | 1 | PROCESSED | 57545.0814351852 | 2016-06-06 01:57:16 | 55213 | 2010-01-17 00:00:00 | 54847.4571296296 | 2009-01-16 10:58:16 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030027 | Suzaku observations of a hot halo of nearby, edge-on starburst galaxy NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by an offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and the dynamics of the galaxy outflow to the intergalactic space. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NORIKO YAMASAKI | JAP | 3 | AO3 | SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803004010/ | Quick Look | ![]() |
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831 | NGC 1550-OFFSET1 | 65.1493 | 2.6086 | 64.497489 | 2.490158 | 63.709607 | -18.593747 | 190.9426677 | -31.53770965 | 265.5852 | 54901.8171875 | 2009-03-11 19:36:45 | 54903.699525463 | 2009-03-13 16:47:19 | 803046010 | 66.8274 | 62 | 66.8274 | 66.8274 | 0 | 66.8274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60.9307 | 60.9307 | 162.6001 | 2 | PROCESSED | 57545.8588541667 | 2016-06-06 20:36:45 | 55329 | 2010-05-13 00:00:00 | 54917.3952314815 | 2009-03-27 09:29:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031422 | We propose a set of two 19 arcmin offset observations of the galaxy groups NGC 1550 and MKW 4 to measure spatially resolved densities, temperatures and iron abundances out to r_500. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to their brightness, regularity and low temperature, the two objects are ideal candidates for an offset observation of their peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FABIO GASTALDELLO | USA | 3 | AO3 | THE OUTSKIRTS OF NGC 1550 AND MKW 4 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803046010/ | Quick Look | ![]() |
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832 | NGC741MOSAICE_P2 | 29.9595 | 5.5362 | 29.305812 | 5.294206 | 29.82553 | -6.270862 | 152.32010482 | -53.38732445 | 71.7775 | 55054.083912037 | 2009-08-11 02:00:50 | 55054.3334837963 | 2009-08-11 08:00:13 | 804052020 | 12.7341 | 10 | 12.7341 | 12.7421 | 0 | 12.7421 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.0159 | 12.0159 | 21.5599 | 0 | PROCESSED | 57548.1149884259 | 2016-06-09 02:45:35 | 55448 | 2010-09-09 00:00:00 | 55081.2532060185 | 2009-09-07 06:04:37 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804052020/ | Quick Look | ![]() |
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833 | ABELL 426 S3 | 49.7347 | 40.7118 | 48.913 | 40.530382 | 58.200048 | 21.614452 | 150.88956259 | -14.01841244 | 87.9998 | 55425.5951273148 | 2010-08-17 14:16:59 | 55425.804375 | 2010-08-17 19:18:18 | 805098010 | 11.0308 | 10 | 11.0548 | 11.0468 | 0 | 11.0308 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.7896 | 7.7896 | 18.0719 | 0 | PROCESSED | 57553.1040162037 | 2016-06-14 02:29:47 | 55287 | 2010-04-01 00:00:00 | 55439.0928935185 | 2010-08-31 02:13:46 | 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/ver3.0/805098010/ | Quick Look | ![]() |
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834 | A1750R | 202.8691 | -2.0415 | 202.224847 | -1.784379 | 201.912931 | 6.996197 | 322.80853082 | 59.27632496 | 111.4517 | 55918.5150810185 | 2011-12-23 12:21:43 | 55918.843912037 | 2011-12-23 20:15:14 | 806098020 | 16.062 | 13 | 16.062 | 16.062 | 0 | 16.062 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11.964 | 11.964 | 28.4079 | 0 | PROCESSED | 57604.214375 | 2016-08-04 05:08:42 | 56311 | 2013-01-19 00:00:00 | 55972.6764236111 | 2012-02-15 16:14:03 | 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 | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806098020/ | Quick Look | ![]() |
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835 | A3391&A3395 FILAMENT | 96.6913 | -54.1225 | 96.432969 | -54.090694 | 107.900065 | -77.146986 | 262.85175229 | -25.18315788 | 316.4875 | 56791.0860532407 | 2014-05-14 02:03:55 | 56792.4794328704 | 2014-05-15 11:30:23 | 809033010 | 88.6134 | 92 | 88.6134 | 88.6134 | 0 | 88.6134 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15.2448 | 15.2448 | 23.346 | 0 | PROCESSED | 57615.0916319445 | 2016-08-15 02:11:57 | 57227 | 2015-07-24 00:00:00 | 56861.4967361111 | 2014-07-23 11:55:18 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090082 | To investigate hot gas properties of a large scale filament, we propose Suzaku observation (92 ks) of a filamentary structure between Abell 3391 and Abell 3395. A3391 and A3395 are located in Horologium supercluster and expected to be in an initial phase of a cluster merger. With Suzaku fs high sensitivity observation, we will (i) determine the physical conditions of IntraCluster Medium by measuring the temperature and density distribution, (ii) unveil the origin of the filamentary structure from distribution of abundance, pressure and entropy. Our study will reveal the formation history of the filament and provide a useful information for the future Sunyaev-Zeldovich effect observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | YOSHITAKA ISHISAKI | JAP | 9 | AO9 | INVESTIGATION OF THE ORIGIN OF THE FILAMENTARY STRUCTURE BETWEEN ABELL 3391 AND ABELL 3395 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809033010/ | Quick Look | ![]() |
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836 | RXCJ0605 | 91.4958 | -35.4837 | 91.05364 | -35.477523 | 92.366503 | -58.913023 | 241.98342334 | -24.04647163 | 309.0856 | 55321.4301041667 | 2010-05-05 10:19:21 | 55322.221712963 | 2010-05-06 05:19:16 | 805065010 | 40.9762 | 40 | 40.9762 | 40.9762 | 0 | 40.9762 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35.5095 | 35.5095 | 68.3681 | 0 | PROCESSED | 57551.3998032407 | 2016-06-12 09:35:43 | 55287 | 2010-04-01 00:00:00 | 55341.4983217593 | 2010-05-25 11:57:35 | 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/ver3.0/805065010/ | Quick Look | ![]() |
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837 | ABELL 426 SE6.5 | 51.5164 | 40.175 | 50.693426 | 40.000231 | 59.444153 | 20.730657 | 152.35568667 | -13.7013792 | 87.5613 | 55800.1546990741 | 2011-08-27 03:42:46 | 55800.3765856482 | 2011-08-27 09:02:17 | 806121010 | 10.1899 | 10 | 10.1979 | 10.1899 | 0 | 10.2055 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.353 | 7.353 | 19.1679 | 0 | PROCESSED | 57602.9755324074 | 2016-08-02 23:24:46 | 55652 | 2011-04-01 00:00:00 | 55865.0897569444 | 2011-10-31 02:09:15 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806121010/ | Quick Look | ![]() |
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838 | VIRGO S8 | 187.5886 | 9.916 | 186.954186 | 10.192142 | 182.977842 | 12.105979 | 285.82444468 | 72.08390522 | 307.999 | 56113.4301041667 | 2012-07-05 10:19:21 | 56113.7523148148 | 2012-07-05 18:03:20 | 807122010 | 16.053 | 13 | 16.053 | 16.053 | 0 | 16.053 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.15 | 15.15 | 27.8319 | 1 | PROCESSED | 57606.5675578704 | 2016-08-06 13:37:17 | 56018 | 2012-04-01 00:00:00 | 56226.5896296296 | 2012-10-26 14:09:04 | 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/ver3.0/807122010/ | Quick Look | ![]() |
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839 | BOOTES_GROUP_32 | 217.4805 | 33.2976 | 216.950847 | 33.519259 | 200.513031 | 44.906456 | 55.13369931 | 67.90745799 | 91.5977 | 54868.4415740741 | 2009-02-06 10:35:52 | 54869.3619675926 | 2009-02-07 08:41:14 | 803045010 | 40.7287 | 40 | 40.7447 | 40.7287 | 0 | 40.7447 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34.6563 | 34.6563 | 79.4878 | 2 | PROCESSED | 57545.4809490741 | 2016-06-06 11:32:34 | 55328 | 2010-05-12 00:00:00 | 54880.5918518518 | 2009-02-18 14:12:16 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031411 | Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 3 | AO3 | UNDERSTANDING GROUP EVOLUTION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803045010/ | Quick Look | ![]() |
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840 | BOOTES_GROUP_37 | 216.3696 | 32.9366 | 215.835617 | 33.161488 | 199.570858 | 44.168282 | 54.59315934 | 68.88543442 | 308.8196 | 54640.4539467593 | 2008-06-23 10:53:41 | 54641.6898611111 | 2008-06-24 16:33:24 | 803044010 | 52.9034 | 40 | 52.9114 | 52.9114 | 0 | 52.9034 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47.6527 | 47.6527 | 106.7658 | 2 | PROCESSED | 57542.9257638889 | 2016-06-03 22:13:06 | 55020 | 2009-07-08 00:00:00 | 54651.1591319444 | 2008-07-04 03:49:09 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031411 | Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | ERIC MILLER | USA | 3 | AO3 | UNDERSTANDING GROUP EVOLUTION WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/803044010/ | Quick Look | ![]() |
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841 | ABELL 2259 | 259.8931 | 27.621 | 259.395788 | 27.671022 | 255.818642 | 50.564036 | 50.28820146 | 31.27138653 | 102.8681 | 57093.1224305556 | 2015-03-12 02:56:18 | 57094.3141203704 | 2015-03-13 07:32:20 | 809081040 | 43.027 | 42.5 | 43.027 | 43.027 | 0 | 43.5266 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7751736111 | 2016-08-17 18:36:15 | 57475 | 2016-03-28 00:00:00 | 57108.4150578704 | 2015-03-27 09:57:41 | 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/ver3.0/809081040/ | Quick Look | ![]() |
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842 | ABELL 426 N5 | 49.0181 | 42.6863 | 48.185508 | 42.502238 | 58.244167 | 23.659861 | 149.32374876 | -12.65326208 | 59.9992 | 55063.2465740741 | 2009-08-20 05:55:04 | 55063.8238310185 | 2009-08-20 19:46:19 | 804067010 | 23.6074 | 20 | 23.6314 | 23.6074 | 0 | 23.6394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21.1435 | 21.1435 | 49.8659 | 1 | PROCESSED | 57548.2975115741 | 2016-06-09 07:08:25 | 55441 | 2010-09-02 00:00:00 | 55075.0347685185 | 2009-09-01 00:50:04 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | STEVEN ALLEN | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804067010/ | Quick Look | ![]() |
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843 | ABELL 426 W6 | 47.7251 | 41.6255 | 46.903246 | 41.436792 | 56.912386 | 22.919663 | 149.06845077 | -14.06119334 | 94.0002 | 55430.3630324074 | 2010-08-22 08:42:46 | 55430.696724537 | 2010-08-22 16:43:17 | 805108010 | 15.3996 | 15 | 15.4076 | 15.3996 | 0 | 15.4076 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13.6106 | 13.6106 | 28.8239 | 0 | PROCESSED | 57553.1647569444 | 2016-06-14 03:57:15 | 55287 | 2010-04-01 00:00:00 | 55446.1712384259 | 2010-09-07 04:06:35 | 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/ver3.0/805108010/ | Quick Look | ![]() |
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844 | A1750R | 202.8633 | -2.0722 | 202.218991 | -1.815068 | 201.918925 | 6.965529 | 322.77954726 | 59.24881782 | 293.5198 | 55748.0658796296 | 2011-07-06 01:34:52 | 55750.0419097222 | 2011-07-08 01:00:21 | 806098010 | 66.5035 | 80 | 66.5115 | 66.5035 | 0 | 66.5115 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 54.7821 | 54.7821 | 170.7128 | 3 | PROCESSED | 57602.5535763889 | 2016-08-02 13:17:09 | 56311 | 2013-01-19 00:00:00 | 55795.163912037 | 2011-08-22 03:56:02 | 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/ver3.0/806098010/ | Quick Look | ![]() |
845 | COMA E6 | 196.7721 | 27.8867 | 196.173433 | 28.153627 | 183.239501 | 32.041991 | 46.15941504 | 86.44797144 | 279.9997 | 55731.2742013889 | 2011-06-19 06:34:51 | 55731.589837963 | 2011-06-19 14:09:22 | 806036010 | 12.4586 | 15 | 12.4666 | 12.4586 | 0 | 12.4666 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12.2065 | 12.2065 | 27.2519 | 0 | PROCESSED | 57602.3498263889 | 2016-08-02 08:23:45 | 55652 | 2011-04-01 00:00:00 | 55770.1165046296 | 2011-07-28 02:47:46 | 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/ver3.0/806036010/ | Quick Look | ![]() |
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846 | ABELL 426 SE4 | 50.9063 | 40.7039 | 50.081498 | 40.526831 | 59.116004 | 21.364386 | 151.65332772 | -13.52999243 | 89.5612 | 55798.708912037 | 2011-08-25 17:00:50 | 55798.9210300926 | 2011-08-25 22:06:17 | 806116010 | 10.8357 | 10 | 10.8406 | 10.8446 | 0 | 10.8357 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10.8394 | 10.8394 | 18.32 | 0 | PROCESSED | 57602.9537615741 | 2016-08-02 22:53:25 | 55652 | 2011-04-01 00:00:00 | 55855.1658449074 | 2011-10-21 03:58:49 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | 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 | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/806116010/ | Quick Look | ![]() |
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847 | THE MOON | 132.8593 | 12.3218 | 132.173537 | 12.509929 | 131.851232 | -5.111118 | 215.15290673 | 32.14399459 | 282.2504 | 56783.6861921296 | 2014-05-06 16:28:07 | 56783.8127083333 | 2014-05-06 19:30:18 | 809001020 | 4.6445 | 45 | 4.6445 | 4.6445 | 0 | 4.6605 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4.9299 | 4.9299 | 10.9199 | 0 | PROCESSED | 57615.0434143518 | 2016-08-15 01:02:31 | 57162 | 2015-05-20 00:00:00 | 56793.5180324074 | 2014-05-16 12:25:58 | 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/ver3.0/809001020/ | Quick Look | ![]() |
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848 | ABELL 3411 | 130.503 | -17.558 | 129.929319 | -17.378234 | 138.643901 | -34.411415 | 242.03718903 | 14.84069283 | 105.0003 | 56964.4121759259 | 2014-11-03 09:53:32 | 56967.3091898148 | 2014-11-06 07:25:14 | 809082010 | 126.6792 | 130 | 126.6792 | 131.2712 | 0 | 131.2632 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.749525463 | 2016-08-16 17:59:19 | 57358 | 2015-12-02 00:00:00 | 56982.4526273148 | 2014-11-21 10:51:47 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091528 | Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | REINOUT VAN WEEREN | USA | 9 | AO9 | ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY? | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809082010/ | Quick Look | ![]() |
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849 | ABELL 426 S7.5 | 49.4444 | 39.4701 | 48.631245 | 39.287629 | 57.603638 | 20.482404 | 151.40364882 | -15.177571 | 87.9989 | 55428.0734375 | 2010-08-20 01:45:45 | 55428.5321180556 | 2010-08-20 12:46:15 | 805113010 | 14.87 | 15 | 14.87 | 14.87 | 0 | 14.87 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.0723 | 13.0723 | 39.628 | 0 | PROCESSED | 57553.1466898148 | 2016-06-14 03:31:14 | 55287 | 2010-04-01 00:00:00 | 55439.2152546296 | 2010-08-31 05:09:58 | 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/ver3.0/805113010/ | Quick Look | ![]() |
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850 | ABELL2804 | 9.8968 | -28.9096 | 9.281885 | -29.184169 | 356.393467 | -30.22696 | 357.98440451 | -86.83577265 | 234.7036 | 53706.3688078704 | 2005-12-02 08:51:05 | 53707.166875 | 2005-12-03 04:00:18 | 800007010 | 31.6129 | 25 | 31.6129 | 31.6129 | 31.6129 | 31.6129 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26.9145 | 26.9145 | 68.95 | 2 | PROCESSED | 57532.3559259259 | 2016-05-24 08:32:32 | 54247 | 2007-05-27 00:00:00 | 54038.8727893518 | 2006-10-30 20:56:49 | 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/ver3.0/800007010/ | Quick Look | ![]() |
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851 | A2142 | 239.5312 | 27.2879 | 239.014287 | 27.430116 | 229.09968 | 46.49364 | 44.29837206 | 48.74478569 | 138.1624 | 54104.1546990741 | 2007-01-04 03:42:46 | 54105.3891666667 | 2007-01-05 09:20:24 | 801055010 | 51.4525 | 60 | 51.4605 | 51.4525 | 0 | 51.4605 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49.2098 | 49.2098 | 106.632 | 1 | PROCESSED | 57536.4705555556 | 2016-05-28 11:17:36 | 54735 | 2008-09-26 00:00:00 | 54111.417037037 | 2007-01-11 10:00:32 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010106 | We propose to reveal the formation and evolution of dense core with cold fronts with SUZAKU/XIS. Our strategy of observation is based on the results of Chandra, ROSAT and weak lensing analysis. A2142 is a galaxy cluster which has contact discontinuities, "cold fronts", between cold-dense cores and hot-thin surrounding gas. We have carried out "weak lensing analysis" and derived mass map in A2142. We measure the bulk velocity via Fe-K line in the central region. We derive the merger velocity by observing the temperatures of the heating and non-heating which are expected by our observational results. It leads to understand the formation and evolution of dense core with cold fronts, since the merger and core velocities are closely related to the evolution of dense cores with cold fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NOBUHIRO OKABE | JAP | 1 | AO1 | REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/801055010/ | Quick Look | ![]() |
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852 | PKS 0745-191 | 116.6543 | -19.2063 | 116.100315 | -19.082609 | 123.362638 | -39.608686 | 236.25768919 | 2.88874721 | 294.0002 | 54231.8221180556 | 2007-05-11 19:43:51 | 54232.5001041667 | 2007-05-12 12:00:09 | 802062020 | 31.2266 | 30 | 31.2266 | 31.2266 | 0 | 31.2266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25.967 | 25.967 | 58.5739 | 1 | PROCESSED | 57538.6330208333 | 2016-05-30 15:11:33 | 54695 | 2008-08-17 00:00:00 | 54238.8889814815 | 2007-05-18 21:20:08 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ANDREW YOUNG | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802062020/ | Quick Look | ![]() |
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853 | RCS 1104-0445 | 166.1645 | -4.748 | 165.529365 | -4.478046 | 169.133755 | -9.830173 | 259.90521833 | 48.99506028 | 108.5039 | 54420.9087037037 | 2007-11-16 21:48:32 | 54421.3210532407 | 2007-11-17 07:42:19 | 802068010 | 19.335 | 15 | 19.335 | 19.335 | 0 | 19.335 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15.1627 | 15.1627 | 35.6159 | 0 | PROCESSED | 57540.5367013889 | 2016-06-01 12:52:51 | 54797 | 2008-11-27 00:00:00 | 54430.2980787037 | 2007-11-26 07:09:14 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021451 | We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AMALIA HICKS | USA | 2 | AO2 | A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/802068010/ | Quick Look | ![]() |
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854 | NGC741MOSAICS_P3 | 28.9813 | 4.9712 | 28.329333 | 4.726893 | 28.70862 | -6.461023 | 151.24323938 | -54.31718683 | 71.7124 | 55052.9243981482 | 2009-08-09 22:11:08 | 55053.1529976852 | 2009-08-10 03:40:19 | 804054030 | 9.4013 | 10 | 9.4093 | 9.4013 | 0 | 9.415 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7.0683 | 7.0683 | 19.72 | 0 | PROCESSED | 57548.0955671296 | 2016-06-09 02:17:37 | 55451 | 2010-09-12 00:00:00 | 55085.0001736111 | 2009-09-11 00:00:15 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | JOEL BREGMAN | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/804054030/ | Quick Look | ![]() |
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855 | FG14 | 176.6962 | 9.8632 | 176.052451 | 10.141025 | 173.028517 | 7.733182 | 258.4262435 | 66.96745764 | 295.6185 | 56076.7125925926 | 2012-05-29 17:06:08 | 56077.2168171296 | 2012-05-30 05:12:13 | 807055010 | 12.4926 | 10 | 12.5006 | 12.495 | 0 | 12.4926 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13.535 | 13.535 | 43.5539 | 1 | PROCESSED | 57605.5555671296 | 2016-08-05 13:20:01 | 56452 | 2013-06-09 00:00:00 | 56086.1554861111 | 2012-06-08 03:43:54 | 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/ver3.0/807055010/ | Quick Look | ![]() |
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856 | HYDRA A SE | 139.5641 | -12.2366 | 138.96256 | -12.025643 | 146.239045 | -26.524458 | 243.07517911 | 25.03717361 | 300.0006 | 56085.6674421296 | 2012-06-07 16:01:07 | 56086.2926388889 | 2012-06-08 07:01:24 | 807087010 | 21.4898 | 20 | 21.4898 | 21.4898 | 0 | 21.4898 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20.3651 | 20.3651 | 54.012 | 0 | PROCESSED | 57605.6279976852 | 2016-08-05 15:04:19 | 56465 | 2013-06-22 00:00:00 | 56099.0036921296 | 2012-06-21 00:05:19 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DOMINIQUE ECKERT | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/807087010/ | Quick Look | ![]() |
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857 | VIRGO S18 | 187.3413 | 6.4206 | 186.704552 | 6.696898 | 184.175793 | 8.806296 | 287.72310531 | 68.63810092 | 122.5021 | 56272.526400463 | 2012-12-11 12:38:01 | 56272.9307175926 | 2012-12-11 22:20:14 | 807132010 | 19.8676 | 18 | 19.8756 | 19.8676 | 0 | 19.8836 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18.8251 | 18.8251 | 34.9319 | 0 | PROCESSED | 57608.2443055556 | 2016-08-08 05:51:48 | 56018 | 2012-04-01 00:00:00 | 56291.7121296296 | 2012-12-30 17:05:28 | 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/ver3.0/807132010/ | Quick Look | ![]() |
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858 | SWCL0759+3244 | 119.7517 | 32.7514 | 118.954635 | 32.88785 | 115.246831 | 11.881047 | 188.23731341 | 27.65711067 | 99.0622 | 56961.3067708333 | 2014-10-31 07:21:45 | 56962.2286574074 | 2014-11-01 05:29:16 | 809085010 | 42.3039 | 41 | 42.3039 | 42.3039 | 0 | 42.3039 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7390277778 | 2016-08-16 17:44:12 | 57345 | 2015-11-19 00:00:00 | 56979.4492708333 | 2014-11-18 10:46:57 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | XINYU DAI | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y | https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/809085010/ | Quick Look | ![]() |
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