DARTS/Astro Query System - SQL Search -
All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".
total 241
No. |
object_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
|
awarded_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
|
quantity_of_hxd_burst
|
processing_status
|
processing_date_mjd
|
processing_date
|
public_date_mjd
|
public_date
|
distribution_date_mjd
|
distribution_date
|
processing_version
|
processing_count
|
processing_software
|
proposal_id
|
proposal_abstract
|
proposal_category
|
proposal_category_code
|
proposal_priority
|
pi_name
|
co_pi_name
|
proposal_affiliated_country
|
proposal_cycle
|
observation_type
|
proposal_title
|
main_instrument
|
has_xis_injection
|
data_access_url
|
ql_access_url
|
ql_image_url
|
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1 | 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 | 48.977877 | 40.801825 | 58.333099 | 21.861106 | 150.77920085 | -13.76419767 | 87.9994 | 55425.2999884259 | 2010-08-17 07:11:59 | 55425.5946527778 | 2010-08-17 14:16:18 | 805097010 | 10.9046 | 10 | 10.9347 | 10.9286 | 0 | 10.9046 | 1 | 1 |