DARTS Astro

total 241

No.
target_name
center_ra
center_dec
center_ra_b1950
center_dec_b1950
center_ecliptic_lon
center_ecliptic_lat
center_galactic_lon
center_galactic_lat
roll_angle
observation_start_time_mjd
observation_start_time
observation_end_time_mjd
observation_end_time
observation_id
exposure
proposal_exposure
xis0_exposure
xis1_exposure
xis2_exposure
xis3_exposure
xis0_observation_mode
xis1_observation_mode
xis2_observation_mode
xis3_observation_mode
hxd_observation_mode
hxd_coarse_clock_rate_exposure
hxd_first_clock_rate_exposure
hxd_normal_clock_rate_exposure
hxd_all_clock_rate_exposure
hxd_wam_exposure
hxd_burst_num
processing_status
processing_end_time_mjd
processing_end_time
public_date_mjd
public_date
distribute_start_date_mjd
distribute_start_date
processing_version
processing_quantity
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle_count
observation_type
proposal_title
main_detector
xis_injection_flag
data_access_url
ql_access_url
ql_image_url
1 4U0142+61 26.5176 61.8112 25.649771 61.561225 52.160955 46.451759 129.33625727 -0.37933599 61.041 55055.0703125 2009-08-12 01:41:15 55057.3654976852 2009-08-14 08:46:19 404079010 107.4129 100 107.4129 107.4209 0 107.4227 2 2 0 2 1 0 0 99.7576 99.7576 198.2838 2 PROCESSED 57548.2012152778 2016-06-09 04:49:45 54922 2009-04-01 00:00:00 55068.3037268518 2009-08-25 07:17:22 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404079010/ Quick Look
2 PSR J1846-0258 281.5972 -2.9106 280.942424 -2.965017 282.329422 20.034924 29.7662115 -0.20474108 86.0001 54936.8175578704 2009-04-15 19:37:17 54939.6779398148 2009-04-18 16:16:14 404081010 104.3451 100 104.3451 104.3675 0 104.3531 2 2 0 2 1 0 0 76.0065 76.0065 247.1018 1 PROCESSED 57546.2746990741 2016-06-07 06:35:34 54922 2009-04-01 00:00:00 54959.5006018518 2009-05-08 12:00:52 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404081010/ Quick Look
3 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
4 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
5 GALACTIC_BULGE10 268.297 -31.6627 267.484676 -31.652449 268.525852 -8.230314 358.49964198 -2.80216044 277.1297 55091.579525463 2009-09-17 13:54:31 55093.1508564815 2009-09-19 03:37:14 504093010 53.2416 50 53.2495 53.2416 0 53.2575 2 2 0 2 1 0 0 46.9072 46.9072 135.734 1 PROCESSED 57548.6254513889 2016-06-09 15:00:39 54922 2009-04-01 00:00:00 55110.3193865741 2009-10-06 07:39:55 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504093010/ Quick Look
6 GALACTIC_BULGE8 267.0897 -31.0498 266.281644 -31.033699 267.475091 -7.634163 358.49976827 -1.60277837 260.4349 55088.8177777778 2009-09-14 19:37:36 55090.3043287037 2009-09-16 07:18:14 504091010 51.3316 50 51.3316 51.3392 0 51.3316 2 2 0 2 1 0 0 47.7514 47.7514 128.4258 2 PROCESSED 57548.5976041667 2016-06-09 14:20:33 54922 2009-04-01 00:00:00 55109.4226736111 2009-10-05 10:08:39 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504091010/ Quick Look
7 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
8 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
9 SGR 1900+14 286.7986 9.3873 286.201777 9.308221 289.568815 31.69386 43.07377535 0.80526184 82.6704 54947.7664814815 2009-04-26 18:23:44 54949.0807175926 2009-04-28 01:56:14 404077010 53.1374 50 53.3934 53.3934 0 53.1374 2 2 0 2 1 0 0 42.1011 42.1011 113.5479 1 PROCESSED 57546.4694444444 2016-06-07 11:16:00 54922 2009-04-01 00:00:00 54973.4547222222 2009-05-22 10:54:48 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404077010/ Quick Look
10 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
11 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
12 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
13 GRXE_E_10 267.9015 -25.9408 267.12546 -25.928719 268.101648 -2.513628 3.25115356 0.4070413 105.0001 56362.3793865741 2013-03-11 09:06:19 56364.8778472222 2013-03-13 21:04:06 507075010 101.3428 100 101.3428 101.3428 0 101.3428 2 2 0 2 1 0 0 88.2422 88.2422 215.806 2 PROCESSED 57610.8450462963 2016-08-10 20:16:52 56018 2012-04-01 00:00:00 56377.5882175926 2013-03-26 14:07:02 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507075010/ Quick Look
14 MBM16 49.7694 11.5801 49.085806 11.399029 50.444533 -6.508969 170.60605682 -37.27197306 254.9211 56331.4284606482 2013-02-08 10:16:59 56333.553587963 2013-02-10 13:17:10 507076020 80.9506 80 80.9746 80.9506 0 80.9746 2 2 0 2 1 0 0 69.3076 69.3076 183.5839 2 PROCESSED 57610.5874074074 2016-08-10 14:05:52 56018 2012-04-01 00:00:00 56349.5813657407 2013-02-26 13:57:10 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076020/ Quick Look
15 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
16 MBM36 238.3613 -4.7912 237.701072 -4.643799 237.20756 15.120262 4.0047136 35.6981582 275.8793 56894.6980324074 2014-08-25 16:45:10 56896.6598958333 2014-08-27 15:50:15 509074010 83.1887 80 83.1967 83.1887 0 83.1967 2 2 0 2 1 0 0 3.755 3.755 8.94 0 PROCESSED 57616.559525463 2016-08-16 13:25:43 56748 2014-04-01 00:00:00 56929.2087615741 2014-09-29 05:00:37 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096001 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 9 AO9 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509074010/ Quick Look
17 GB_NORTH_4 264.8998 -28.3109 264.109826 -28.284233 265.484852 -4.949634 359.83607677 1.45248781 106.6967 57110.9717708333 2015-03-29 23:19:21 57113.0203472222 2015-04-01 00:29:18 509080010 88.1941 100 88.1941 95.0455 0 95.0615 3 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.8835648148 2016-08-17 21:12:20 56748 2014-04-01 00:00:00 57125.4051736111 2015-04-13 09:43:27 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096002 The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 9 AO9 MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509080010/ Quick Look
18 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
19 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
20 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
21 SN1006_SE1 225.8641 -42.0384 225.045074 -41.843059 235.594631 -23.72201 327.62177329 14.41744154 286.0629 56883.8521064815 2014-08-14 20:27:02 56887.5210648148 2014-08-18 12:30:20 509082010 201.8322 480 201.8322 202.4881 0 202.5201 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57616.5228240741 2016-08-16 12:32:52 56748 2014-04-01 00:00:00 56910.6390509259 2014-09-10 15:20:14 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096004 We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. GALACTIC DIFFUSE EMISSION 5 A HIROYA YAMAGUCHI USA 9 AO9 THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082010/ Quick Look
22 SN1006_SE1 225.857 -42.039 225.037992 -41.843634 235.58934 -23.724178 327.61674963 14.4195613 107.6985 57063.4521643518 2015-02-10 10:51:07 57069.9807060185 2015-02-16 23:32:13 509082020 258.382 280 258.382 278.7901 0 278.8541 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.6457523148 2016-08-17 15:29:53 56748 2014-04-01 00:00:00 57080.4416898148 2015-02-27 10:36:02 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096004 We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. GALACTIC DIFFUSE EMISSION 5 A HIROYA YAMAGUCHI USA 9 AO9 THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509082020/ Quick Look
23 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
24 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
25 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
26 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
27 GALACTIC_BULGE1 267.2201 -29.3677 266.422949 -29.352259 267.554885 -5.950193 359.99969448 -0.83243485 274.7 55118.4798148148 2009-10-14 11:30:56 55119.6453587963 2009-10-15 15:29:19 504088010 47.23 50 47.23 47.23 0 47.23 2 2 0 2 1 0 0 32.6139 32.6139 100.7 2 PROCESSED 57548.8825231482 2016-06-09 21:10:50 54922 2009-04-01 00:00:00 55134.0688425926 2009-10-30 01:39:08 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504088010/ Quick Look
28 GALACTIC_BULGE9 267.6768 -31.2805 266.867115 -31.267244 267.986252 -7.855618 358.55970985 -2.15232996 265.3076 55090.3066550926 2009-09-16 07:21:35 55091.5758564815 2009-09-17 13:49:14 504092010 50.9199 50 50.9439 50.9359 0 50.9199 2 2 0 2 1 0 0 45.5744 45.5744 109.6459 1 PROCESSED 57548.6135069444 2016-06-09 14:43:27 54922 2009-04-01 00:00:00 55109.4315740741 2009-10-05 10:21:28 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504092010/ Quick Look
29 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
30 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
31 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
32 KEPLER_BG_GE 263.5357 -20.2632 262.792974 -20.230061 263.919291 3.041451 5.99779838 6.79710869 273.0028 55072.0030208333 2009-08-29 00:04:21 55072.5002662037 2009-08-29 12:00:23 504101020 24.7227 60 24.7467 24.7387 0 24.7227 2 2 0 2 1 0 0 19.2528 19.2528 42.9559 0 PROCESSED 57548.3891550926 2016-06-09 09:20:23 54922 2009-04-01 00:00:00 55109.4155324074 2009-10-05 09:58:22 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101020/ Quick Look
33 KEPLER_BG_GW 261.806 -22.7684 261.049806 -22.726898 262.438757 0.457902 2.99933771 6.7960859 273.0885 55109.2984143518 2009-10-05 07:09:43 55111.1057175926 2009-10-07 02:32:14 504102010 65.2949 60 65.3029 65.2949 0 65.3029 2 2 0 2 1 0 0 50.7821 50.7821 156.128 1 PROCESSED 57548.8038425926 2016-06-09 19:17:32 54922 2009-04-01 00:00:00 55125.6963888889 2009-10-21 16:42:48 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504102010/ Quick Look
34 KEPLER_BG_GS 263.1005 -22.949 262.342899 -22.913725 263.639389 0.339875 3.49961978 5.69692486 272.6396 55107.43 2009-10-03 10:19:12 55109.2973842593 2009-10-05 07:08:14 504104010 67.2508 60 67.2508 67.2805 0 67.2748 2 2 0 2 1 0 0 53.1585 53.1585 161.3298 1 PROCESSED 57548.7538425926 2016-06-09 18:05:32 54922 2009-04-01 00:00:00 55125.3521180556 2009-10-21 08:27:03 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504104010/ Quick Look
35 GALACTIC_BULGE3 267.9488 -29.7963 267.148788 -29.784389 268.199437 -6.368042 359.95634845 -1.5962466 107.1729 55624.8013310185 2011-03-04 19:13:55 55626.2292939815 2011-03-06 05:30:11 505078010 51.2756 50 51.2756 51.2756 0 51.2756 2 2 0 2 1 0 0 39.3124 39.3124 123.3618 0 PROCESSED 57601.0957407407 2016-08-01 02:17:52 55287 2010-04-01 00:00:00 55642.1205787037 2011-03-22 02:53:38 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505078010/ Quick Look
36 GALACTIC_BULGE15 265.6963 -32.7784 264.876935 -32.755516 266.323781 -9.39206 356.40742505 -1.49294303 89.8786 55626.2338425926 2011-03-06 05:36:44 55627.5424884259 2011-03-07 13:01:11 505084010 50.3097 50 50.3172 50.3097 0 50.3252 1 1 0 1 1 0 0 37.5095 37.5095 113.0559 0 PROCESSED 57601.1030439815 2016-08-01 02:28:23 55287 2010-04-01 00:00:00 55645.2697222222 2011-03-25 06:28:24 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505084010/ Quick Look
37 GALACTIC_BULGE16 266.5113 -33.2224 265.68867 -33.203457 267.02907 -9.817155 356.38592507 -2.30771737 275.4625 55482.2533217593 2010-10-13 06:04:47 55483.5626967593 2010-10-14 13:30:17 505085010 55.0315 50 55.0315 55.0315 0 55.0315 2 2 0 2 1 0 0 48.6341 48.6341 113.1139 1 PROCESSED 57553.750787037 2016-06-14 18:01:08 55287 2010-04-01 00:00:00 55502.290150463 2010-11-02 06:57:49 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505085010/ Quick Look
38 GALACTIC_BULGE17 267.7467 -33.8391 266.919516 -33.82614 268.087567 -10.412886 356.3863118 -3.50805248 275.261 55483.5637731482 2010-10-14 13:31:50 55485.0627893518 2010-10-16 01:30:25 505086010 53.1266 50 53.1266 54.0895 0 54.0895 2 2 0 2 1 0 0 46.2769 46.2769 129.4938 1 PROCESSED 57553.7652430556 2016-06-14 18:21:57 55287 2010-04-01 00:00:00 55508.2025694444 2010-11-08 04:51:42 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505086010/ Quick Look
39 HESS J1841-55 3 280.1471 -5.609 279.479279 -5.656459 280.581257 17.459575 26.70525302 -0.15199861 87.0298 55647.6397685185 2011-03-27 15:21:16 55648.791875 2011-03-28 19:00:18 505090010 49.549 50 49.581 49.549 0 49.581 2 2 0 2 1 0 0 42.7935 42.7935 99.5239 1 PROCESSED 57601.3633101852 2016-08-01 08:43:10 55287 2010-04-01 00:00:00 55666.2655439815 2011-04-15 06:22:23 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505090010/ Quick Look
40 KES 27 237.1872 -53.7777 236.229597 -53.624833 247.581589 -32.858337 327.32071311 0.47884394 101.6269 55983.5400231482 2012-02-26 12:57:38 55985.4633217593 2012-02-28 11:07:11 506063010 109.3535 120 109.4015 109.3535 0 109.4015 3 2 0 2 1 0 0 115.3321 115.3321 166.148 4 PROCESSED 57604.7717592593 2016-08-04 18:31:20 55652 2011-04-01 00:00:00 55995.1904976852 2012-03-09 04:34:19 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506063010/ Quick Look
41 G349.7+0.2 259.4954 -37.4452 258.645482 -37.392398 261.399155 -14.316641 349.72102569 0.17051597 282.4112 55833.4324537037 2011-09-29 10:22:44 55838.1341898148 2011-10-04 03:13:14 506064010 160.4024 160 160.4264 160.4024 0 160.4344 2 2 0 2 1 0 0 144.6151 144.6151 404.22 5 PROCESSED 57603.3931134259 2016-08-03 09:26:05 55652 2011-04-01 00:00:00 55858.5356018518 2011-10-24 12:51:16 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506064010/ Quick Look
42 GRXE_E_2 267.6193 -27.2463 266.835371 -27.232829 267.869305 -3.822869 2.00029183 -0.04392641 105.0002 56366.4085532407 2013-03-15 09:48:19 56368.7772569444 2013-03-17 18:39:15 507069010 103.6873 100 103.6873 103.6873 0 103.6873 2 2 0 2 1 0 0 95.5834 95.5834 204.6259 2 PROCESSED 57610.8702314815 2016-08-10 20:53:08 56018 2012-04-01 00:00:00 56379.6047106482 2013-03-28 14:30:47 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507069010/ Quick Look
43 GRXE_E_3 267.7634 -27.0307 266.980773 -27.017932 267.994323 -3.605243 2.25114568 -0.04369036 105.0001 56368.7777314815 2013-03-17 18:39:56 56371.1111458333 2013-03-20 02:40:03 507070010 101.1726 100 101.1806 101.1726 0 101.1806 2 2 0 2 1 0 0 103.6028 103.6028 201.5898 0 PROCESSED 57610.8916782407 2016-08-10 21:24:01 56018 2012-04-01 00:00:00 56380.5799768518 2013-03-29 13:55:10 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507070010/ Quick Look
44 MBM36 238.3612 -4.7913 237.700971 -4.643898 237.207481 15.120143 4.00454082 35.69817373 279.4993 56155.0155787037 2012-08-16 00:22:26 56156.7563425926 2012-08-17 18:09:08 507077010 81.0158 80 81.0158 81.0176 0 81.0176 2 2 0 2 1 0 0 80.3301 80.3301 150.3877 4 PROCESSED 57606.8991782407 2016-08-06 21:34:49 56018 2012-04-01 00:00:00 56170.1653240741 2012-08-31 03:58:04 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507077010/ Quick Look
45 MBM20 68.9377 -14.6308 68.365051 -14.732172 64.468357 -36.225149 211.4041789 -36.56532035 78.376 56164.0544328704 2012-08-25 01:18:23 56166.3530092593 2012-08-27 08:28:20 507079010 82.8814 80 82.8814 82.8814 0 82.8814 2 2 0 2 1 0 0 73.8668 73.8668 198.5577 2 PROCESSED 57606.9726851852 2016-08-06 23:20:40 56018 2012-04-01 00:00:00 56212.7316087963 2012-10-12 17:33:31 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507079010/ Quick Look
46 GRXE_E_1 267.4747 -27.4596 266.689479 -27.445424 267.744238 -4.038324 1.75131157 -0.04310182 105.3995 56726.0649537037 2014-03-10 01:33:32 56728.6459722222 2014-03-12 15:30:12 508075010 103.5331 100 103.5491 103.5331 0 103.5559 3 2 0 2 1 0 0 85.3446 85.3446 222.9818 2 PROCESSED 57614.0622453704 2016-08-14 01:29:38 56383 2013-04-01 00:00:00 56740.8547453704 2014-03-24 20:30:50 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 086001 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 8 AO8 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508075010/ Quick Look
47 LDN1563 75.5195 13.8744 74.812622 13.803125 75.779261 -8.85474 187.14092451 -16.70693442 81.1182 56523.4274768518 2013-08-19 10:15:34 56525.2535648148 2013-08-21 06:05:08 508080010 83.588 80 83.588 83.596 0 83.604 2 2 0 2 1 0 0 79.6741 79.6741 157.7538 2 PROCESSED 57612.368912037 2016-08-12 08:51:14 56383 2013-04-01 00:00:00 56587.8175694445 2013-10-22 19:37:18 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 086002 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 8 AO8 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508080010/ Quick Look
48 MBM16 49.7701 11.5795 49.086508 11.398432 50.445044 -6.509726 170.60720168 -37.27195697 254.3636 57057.0973726852 2015-02-04 02:20:13 57059.5349421296 2015-02-06 12:50:19 509073020 92.0425 80 92.0425 92.0665 0 92.0665 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.6060763889 2016-08-17 14:32:45 56748 2014-04-01 00:00:00 57107.434224537 2015-03-26 10:25:17 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096001 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 9 AO9 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073020/ Quick Look
49 NGC3783 174.7201 -37.7846 174.100385 -37.507469 192.672057 -36.228861 287.44066962 22.89477473 305.9228 55022.9100115741 2009-07-10 21:50:25 55027.0016087963 2009-07-15 00:02:19 704063010 209.5034 200 209.5034 210.3114 0 210.3194 3 2 0 2 1 0 0 174.0404 174.0404 353.4535 2 PROCESSED 57547.9411342593 2016-06-08 22:35:14 54922 2009-04-01 00:00:00 55040.5612615741 2009-07-28 13:28:13 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A CHRISTOPHER REYNOLDS USA 4 AO4 A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704063010/ Quick Look
50 FAIRALL 9 20.848 -58.7784 20.369866 -59.039074 340.553777 -59.094561 295.14856402 -57.86436534 32.7271 55335.1255671296 2010-05-19 03:00:49 55338.764837963 2010-05-22 18:21:22 705063010 229.2963 250 229.302 229.302 0 229.2963 2 2 0 2 1 0 0 174.9412 174.9412 288.656 1 PROCESSED 57551.9874074074 2016-06-12 23:41:52 55287 2010-04-01 00:00:00 55434.4437615741 2010-08-26 10:39:01 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A CHRISTOPHER REYNOLDS USA 5 AO5 A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/705063010/ Quick Look
51 3C120 68.2984 5.3496 67.633882 5.245152 67.432526 -16.407924 190.37864439 -27.39774516 260.9996 55966.4234143518 2012-02-09 10:09:43 55970.8752083333 2012-02-13 21:00:18 706042010 183.0015 300 183.0255 183.0015 0 183.0255 3 2 0 2 1 0 0 158.0306 158.0306 384.5957 3 PROCESSED 57604.7163310185 2016-08-04 17:11:31 55652 2011-04-01 00:00:00 55992.4178819444 2012-03-06 10:01:45 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A CHRISTOPHER REYNOLDS USA 6 AO6-KP A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706042010/ Quick Look
52 3C120 68.2996 5.3511 67.635075 5.246657 67.433996 -16.406625 190.37800916 -27.39591229 261.0003 55971.7483564815 2012-02-14 17:57:38 55974.8819907407 2012-02-17 21:10:04 706042020 118.0689 120 118.0689 118.0689 0 118.0689 2 2 0 2 1 0 0 103.5365 103.5365 270.7359 2 PROCESSED 57604.7019791667 2016-08-04 16:50:51 55652 2011-04-01 00:00:00 55992.3150694444 2012-03-06 07:33:42 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A CHRISTOPHER REYNOLDS USA 6 AO6-KP A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/706042020/ Quick Look
53 GALACTIC_BULGE11 269.3164 -32.1646 268.50059 -32.159293 269.404915 -8.724949 358.50010375 -3.80248777 271.7893 55093.1531365741 2009-09-19 03:40:31 55095.6064699074 2009-09-21 14:33:19 504094010 93.1403 50 93.1403 93.1403 0 93.1403 2 2 0 2 1 0 0 82.9543 82.9543 211.9538 1 PROCESSED 57548.674224537 2016-06-09 16:10:53 54922 2009-04-01 00:00:00 55110.4114236111 2009-10-06 09:52:27 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504094010/ Quick Look
54 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
55 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
56 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
57 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
58 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
59 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
60 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
61 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
62 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
63 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
64 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
65 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
66 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
67 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
68 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
69 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
70 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
71 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
72 MBM16 49.752 11.6015 49.068335 11.420365 50.433531 -6.483887 170.57212752 -37.26756171 73.5786 56139.0841666667 2012-07-31 02:01:12 56140.9710416667 2012-08-01 23:18:18 507076010 24.9499 80 24.9499 24.9499 0 24.9499 2 2 0 2 1 0 0 18.2376 18.2376 162.962 1 PROCESSED 57606.7578703704 2016-08-06 18:11:20 56018 2012-04-01 00:00:00 56260.533125 2012-11-29 12:47:42 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076003 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 7 AO7 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507076010/ Quick Look
73 1E 2259+586 345.2716 58.9493 344.749816 58.680435 23.84389 56.952455 109.11022544 -0.92895504 86.3239 54976.8335300926 2009-05-25 20:00:17 54978.6446064815 2009-05-27 15:28:14 404076010 122.5791 120 122.5809 122.5809 0 122.5791 2 2 0 2 1 0 0 103.4462 103.4462 156.4638 1 PROCESSED 57546.7298726852 2016-06-07 17:31:01 54922 2009-04-01 00:00:00 54992.6935069444 2009-06-10 16:38:39 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 4 AO4 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/404076010/ Quick Look
74 1RXS J1708-4009 257.2038 -40.2142 256.334135 -40.15046 259.790997 -17.224743 346.43162325 -0.00870489 267.1357 55466.6124074074 2010-09-27 14:41:52 55467.7738425926 2010-09-28 18:34:20 405076010 62.8109 60 62.8189 62.8226 0 62.8109 3 2 0 2 1 0 0 59.5114 59.5114 100.3239 1 PROCESSED 57553.5661342593 2016-06-14 13:35:14 55287 2010-04-01 00:00:00 55477.2762268518 2010-10-08 06:37:46 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056002 We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". GALACTIC POINT SOURCES 4 A KAZUO MAKISHIMA JAP 5 AO5 A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/405076010/ Quick Look
75 GALACTIC_BULGE2 267.5552 -29.599 266.756514 -29.585181 267.852413 -6.176134 359.95115697 -1.20153587 277.9812 55113.1708217593 2009-10-09 04:05:59 55114.5903472222 2009-10-10 14:10:06 504089010 55.2601 50 55.2671 55.2601 0 55.2736 2 2 0 2 1 0 0 40.226 40.226 122.6338 1 PROCESSED 57548.8316666667 2016-06-09 19:57:36 54922 2009-04-01 00:00:00 55131.3309953704 2009-10-27 07:56:38 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504089010/ Quick Look
76 KEPLER_BG_GE 263.5353 -20.2634 262.792573 -20.230259 263.918925 3.041235 5.99742641 6.79731937 272.7609 55087.1593171296 2009-09-13 03:49:25 55088.3606365741 2009-09-14 08:39:19 504101010 46.9895 60 46.9895 46.9895 0 46.9895 2 2 0 2 1 0 0 40.8993 40.8993 103.786 0 PROCESSED 57548.5758564815 2016-06-09 13:49:14 54922 2009-04-01 00:00:00 55099.2516782407 2009-09-25 06:02:25 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 4 AO4 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504101010/ Quick Look
77 THE KEPLER SNR 262.6737 -21.5073 261.92432 -21.469989 263.173689 1.760317 4.50532186 6.80830692 272.2663 55475.6914583333 2010-10-06 16:35:42 55478.2863194445 2010-10-09 06:52:18 505092020 111.1941 620 111.1941 111.2021 0 111.2021 2 2 0 2 1 0 0 99.8413 99.8413 224.1437 2 PROCESSED 57553.7268402778 2016-06-14 17:26:39 55287 2010-04-01 00:00:00 55488.3311689815 2010-10-19 07:56:53 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092020/ Quick Look
78 THE KEPLER SNR 262.671 -21.4826 261.921758 -21.445276 263.169925 1.784856 4.5248811 6.82377384 98.1034 55628.0376736111 2011-03-08 00:54:15 55632.2696643518 2011-03-12 06:28:19 505092050 84.5913 100 84.5913 85.6632 0 85.7192 4 3 0 3 1 0 0 122.4881 122.4881 365.616 3 PROCESSED 57601.284537037 2016-08-01 06:49:44 55287 2010-04-01 00:00:00 55648.4964699074 2011-03-28 11:54:55 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092050/ Quick Look
79 G272.2-3.2 136.7067 -52.1223 136.311595 -51.920282 170.81242 -63.078479 272.22054405 -3.18534238 101.7643 55877.9477777778 2011-11-12 22:44:48 55878.6272916667 2011-11-13 15:03:18 506060020 25.5265 20 25.5345 25.5345 0 25.5265 2 2 0 2 1 0 0 27.028 27.028 58.706 0 PROCESSED 57603.7829282407 2016-08-03 18:47:25 55652 2011-04-01 00:00:00 55895.0737962963 2011-11-30 01:46:16 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506060020/ Quick Look
80 G290.1-0.8 165.7447 -60.8884 165.228717 -60.618807 206.73964 -58.122992 290.11957377 -0.7436408 293.2659 55737.4551388889 2011-06-25 10:55:24 55740.5883333333 2011-06-28 14:07:12 506061010 110.5931 110 110.6091 110.5931 0 110.6011 2 2 0 2 1 0 0 99.3596 99.3596 270.6596 4 PROCESSED 57602.4993634259 2016-08-02 11:59:05 55652 2011-04-01 00:00:00 55775.3693287037 2011-08-02 08:51:50 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506061010/ Quick Look
81 GRXE_E_4 267.9068 -26.8159 267.125467 -26.803832 268.119163 -3.388548 2.50111874 -0.04382328 104.4995 56371.1118518518 2013-03-20 02:41:04 56373.3049421296 2013-03-22 07:19:07 507071010 101.2086 100 101.2166 101.2086 0 101.2166 2 2 0 2 1 0 0 105.6491 105.6491 189.4519 1 PROCESSED 57610.9065625 2016-08-10 21:45:27 56018 2012-04-01 00:00:00 56384.6094560185 2013-04-02 14:37:37 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507071010/ Quick Look
82 G355.6-0.0 263.7798 -32.6083 262.962219 -32.576152 264.68406 -9.281685 355.69106204 -0.03789327 90.0013 55246.5249074074 2010-02-19 12:35:52 55247.6293287037 2010-02-20 15:06:14 504098010 52.5044 50 52.5275 52.5204 0 52.5044 2 2 0 2 1 0 0 43.7346 43.7346 95.4118 0 PROCESSED 57550.6569560185 2016-06-11 15:46:01 54922 2009-04-01 00:00:00 55257.1119444444 2010-03-02 02:41:12 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504098010/ Quick Look
83 MBM36 238.3604 -4.7951 237.700156 -4.647695 237.207526 15.116261 4.00027103 35.69642682 294.5973 56525.2685300926 2013-08-21 06:26:41 56526.5655092593 2013-08-22 13:34:20 508079010 49.6555 80 49.6555 49.6555 0 49.6555 2 2 0 2 1 0 0 42.8799 42.8799 112.0458 2 PROCESSED 57612.3808912037 2016-08-12 09:08:29 56383 2013-04-01 00:00:00 56587.6359027778 2013-10-22 15:15:42 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 086002 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 8 AO8 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508079010/ Quick Look
84 MBM20 68.9307 -14.6229 68.358009 -14.724304 64.461829 -36.216174 211.39181931 -36.56844204 64.9904 56520.8174074074 2013-08-16 19:37:04 56522.5001967593 2013-08-18 12:00:17 508081010 56.4905 80 56.4905 56.4905 0 56.4905 2 2 0 2 1 0 0 55.086 55.086 145.38 1 PROCESSED 57612.3311111111 2016-08-12 07:56:48 56383 2013-04-01 00:00:00 56587.6432291667 2013-10-22 15:26:15 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 086002 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 8 AO8 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508081010/ Quick Look
85 MBM16 49.7641 11.5835 49.080496 11.40241 50.44037 -6.504342 170.59835317 -37.27294118 77.8263 56867.2632638889 2014-07-29 06:19:06 56869.0606018518 2014-07-31 01:27:16 509073010 78.81 80 78.818 78.818 0 78.81 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57616.4583449074 2016-08-16 11:00:01 56748 2014-04-01 00:00:00 56902.6996180556 2014-09-02 16:47:27 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096001 Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. GALACTIC DIFFUSE EMISSION 5 A MASSIMILIANO GALEAZZI USA 9 AO9 CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509073010/ Quick Look
86 GB_NORTH_1 266.1004 -28.3619 265.30982 -28.341045 266.546613 -4.967513 0.35022505 0.52781175 106.0661 57104.6393981482 2015-03-23 15:20:44 57106.6752777778 2015-03-25 16:12:24 509077010 98.2407 100 98.2407 98.4407 0 98.4407 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.8715277778 2016-08-17 20:55:00 56748 2014-04-01 00:00:00 57120.4153125 2015-04-08 09:58:03 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096002 The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 9 AO9 MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509077010/ Quick Look
87 GALACTIC_BULGE7 266.6764 -30.8281 265.869887 -30.809998 267.112733 -7.42025 358.50617228 -1.18471698 274.4326 55117.1787037037 2009-10-13 04:17:20 55118.4785416667 2009-10-14 11:29:06 504090010 41.2607 50 41.2607 52.9033 0 52.9033 3 2 0 2 1 0 0 34.964 34.964 112.2938 2 PROCESSED 57548.8825694444 2016-06-09 21:10:54 54922 2009-04-01 00:00:00 55133.2421643518 2009-10-29 05:48:43 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 4 AO4 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/504090010/ Quick Look
88 GALACTIC_BULGE4 269.1417 -30.4015 268.337633 -30.395373 269.244618 -6.962713 359.95546853 -2.79264334 69.3552 55632.2752314815 2011-03-12 06:36:20 55633.4287152778 2011-03-13 10:17:21 505079010 50.2193 50 50.2273 50.2193 0 50.2273 2 2 0 2 1 0 0 43.375 43.375 99.648 1 PROCESSED 57601.1540277778 2016-08-01 03:41:48 55287 2010-04-01 00:00:00 55645.5706134259 2011-03-25 13:41:41 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505079010/ Quick Look
89 GALACTIC_BULGE5 270.1525 -30.903 269.345086 -30.901777 270.122341 -7.462063 359.95222621 -3.79644913 86.7823 55293.7188657407 2010-04-07 17:15:10 55295.8849074074 2010-04-09 21:14:16 505080010 56.1396 50 56.1396 56.1396 0 56.1396 2 2 0 2 1 0 0 55.1498 55.1498 185.0058 1 PROCESSED 57553.0630439815 2016-06-14 01:30:47 55287 2010-04-01 00:00:00 55441.4355555556 2010-09-02 10:27:12 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056001 We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 5 AO5 SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505080010/ Quick Look
90 THE KEPLER SNR 262.6707 -21.4823 261.92146 -21.444975 263.169631 1.785142 4.52498329 6.82417088 98.3356 55620.8079166667 2011-02-28 19:23:24 55624.797337963 2011-03-04 19:08:10 505092040 146.2337 250 146.2337 146.2541 0 146.2577 2 2 0 2 1 0 0 113.8022 113.8022 344.6577 6 PROCESSED 57601.192337963 2016-08-01 04:36:58 55287 2010-04-01 00:00:00 55642.4090046296 2011-03-22 09:48:58 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 056004 The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. GALACTIC DIFFUSE EMISSION 5 A SANGWOOK PARK USA 5 AO5 A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/505092040/ Quick Look
91 G350.1-0.3 260.2697 -37.4549 259.419167 -37.405796 262.032562 -14.282003 350.06545974 -0.33871818 266.4234 55821.2580787037 2011-09-17 06:11:38 55822.9126388889 2011-09-18 21:54:12 506065010 70.1813 70 70.1973 70.1813 0 70.1973 2 2 0 2 1 0 0 60.0704 60.0704 142.9159 0 PROCESSED 57603.2088541667 2016-08-03 05:00:45 55652 2011-04-01 00:00:00 55865.2679282407 2011-10-31 06:25:49 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 066001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 6 AO6-KP NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/506065010/ Quick Look
92 G337.2-0.7 249.8782 -47.8314 248.950154 -47.733478 255.175293 -25.419144 337.20769447 -0.7291284 280.8005 56172.5530439815 2012-09-02 13:16:23 56181.2598263889 2012-09-11 06:14:09 507068010 304.1484 300 304.1564 304.1484 0 304.1484 2 2 0 2 1 0 0 275.8448 275.8448 461.2638 9 PROCESSED 57607.2211111111 2016-08-07 05:18:24 56018 2012-04-01 00:00:00 56271.4641203704 2012-12-10 11:08:20 3.0.22.44 3 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076001 Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 7 Ao7 NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507068010/ Quick Look
93 GRXE_E_6 268.1913 -26.3855 267.412548 -26.37482 268.368065 -2.954748 3.00107417 -0.0433749 104.9996 56375.3653125 2013-03-24 08:46:03 56377.4119444445 2013-03-26 09:53:12 507073010 101.6745 100 101.6745 101.6745 0 101.6745 2 2 0 2 1 0 0 100.2473 100.2473 176.8078 1 PROCESSED 57610.9396296296 2016-08-10 22:33:04 56018 2012-04-01 00:00:00 56387.5561574074 2013-04-05 13:20:52 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 076002 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 7 AO7 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/507073010/ Quick Look
94 NGC3516 166.8656 72.6213 166.014761 72.891861 123.359499 58.056735 133.14023939 42.38468378 135.8338 55132.2328125 2009-10-28 05:35:15 55137.5272453704 2009-11-02 12:39:14 704062010 251.3555 250 251.3795 251.3715 0 251.3555 2 2 0 2 1 0 0 190.8372 190.8372 333.01 5 PROCESSED 57549.2037268518 2016-06-10 04:53:22 54922 2009-04-01 00:00:00 55152.2729398148 2009-11-17 06:33:02 3.0.22.43 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 046003 We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. EXTRAGALACTIC COMPACT SOURCES 7 A CHRISTOPHER REYNOLDS USA 4 AO4 A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/704062010/ Quick Look
95 GRXE_E_8 268.4708 -25.9492 267.69465 -25.939883 268.614118 -2.515578 3.50431952 -0.037979 86.7223 56718.7089236111 2014-03-02 17:00:51 56720.9585069445 2014-03-04 23:00:15 508077010 103.132 100 103.14 103.132 0 103.14 2 2 0 2 1 0 0 94.8538 94.8538 194.3449 2 PROCESSED 57613.971712963 2016-08-13 23:19:16 56383 2013-04-01 00:00:00 56775.6980787037 2014-04-28 16:45:14 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 086001 We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. GALACTIC DIFFUSE EMISSION 5 A TAKESHI TSURU JAP 8 AO8 ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/508077010/ Quick Look
96 GB_NORTH_2 265.5401 -28.4005 264.749404 -28.376931 266.05313 -5.020438 0.05846164 0.92703829 108.0199 57106.6765856482 2015-03-25 16:14:17 57108.7243634259 2015-03-27 17:23:05 509078010 95.3893 100 95.3893 99.8284 0 99.8124 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.8717361111 2016-08-17 20:55:18 56748 2014-04-01 00:00:00 57119.4143981482 2015-04-07 09:56:44 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096002 The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 9 AO9 MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509078010/ Quick Look
97 GB_NORTH_3 265.8335 -28.3716 265.042917 -28.349452 266.311245 -4.983802 0.21886292 0.72273612 108.0564 57108.7249074074 2015-03-27 17:23:52 57110.9703703704 2015-03-29 23:17:20 509079010 106.9674 100 106.9674 108.1889 0 108.1889 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57617.8792939815 2016-08-17 21:06:11 56748 2014-04-01 00:00:00 57119.4192708333 2015-04-07 10:03:45 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096002 The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. GALACTIC DIFFUSE EMISSION 5 A KATSUJI KOYAMA JAP 9 AO9 MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509079010/ Quick Look
98 SN1006_BGD4 226.2633 -42.7499 225.438524 -42.555935 236.137627 -24.311137 327.5160888 13.6541367 286.3809 56889.2090740741 2014-08-20 05:01:04 56889.7793865741 2014-08-20 18:42:19 509086010 33.5116 30 33.5156 33.5116 0 33.5196 2 2 0 2 0 0 0 0 0 0 0 PROCESSED 57616.5076851852 2016-08-16 12:11:04 56748 2014-04-01 00:00:00 56910.6440162037 2014-09-10 15:27:23 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 096004 We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. GALACTIC DIFFUSE EMISSION 5 A HIROYA YAMAGUCHI USA 9 AO9 THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT XIS Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/509086010/ Quick Look
99 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
100 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
101 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
102 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
103 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
104 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
105 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
106 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
107 ABELL 426 S2 49.8015 40.983 48.